The appearance of Carbonaceous Chondrites on (1) Ceres from observations by the Dawn Framing Camera

NASA Astrophysics Data System (ADS)

Schäfer, Tanja; Schäfer, Michael; Mengel, Kurt; Cloutis, Edward A.; Izawa, Matthew R. M.; Thangjam, Guneshwar; Hoffmann, Martin; Platz, Thomas; Nathues, Andreas; Kallisch, Jan; Ripken, Joachim; Russel, Christopher T.

2016-04-01

NASA's Dawn spacecraft reached dwarf planet Ceres in March 2015 and started data acquisition using three different instruments. These are the Framing Camera (FC; [1]), the Visible & Infrared Spectrometer (VIR; [2]), and the Gamma Ray and Neutron Detector (GRaND; [3]). In our work we focus on the potential appearance of carbonaceous chondritic (CC) material on the cerean surface using Dawn FC color mosaics covering the VIS/NIR wavelength region. In preparation of the Dawn arrival at Ceres, a discrimination scheme for CC groups using FC color ratios was developed by [4] and is based on 121 CC laboratory spectra compiled from RELAB. As the cerean surface material mainly differs by its spectral slope over the whole FC wavelength range (0.44-0.97 μm), we classified the color mosaics by this parameter. We applied the CC discrimination scheme only to those regions on the cerean surface (more than 90 %) which exhibit spectral slopes ≥ -1 % reflectance per μm to exclude the strongly negative sloped regions of large young craters such as Occator, Haulani, and Oxo. These are not likely to be similar to pure CC material as can be seen by their brightness and their bluish spectral slope [5]. We found that the surface material of Ceres is, among the suite of CCs, most similar to Ivuna samples artificially heated to 200 and 300°C [6] and unusual CCs, which naturally experienced heating. The latter ones comprise Dhofar 225, Y-86789 and Y-82162, which have been determined to have undergone aqueous alteration and subsequent thermal metamorphism (e.g. [7,8]).Our comparison with VIR data shows, that the spectra of Ivuna heated to 200°C and 300°C match well the OH-absorption at 2.7 μm but do not show the smaller 3.05-3.1 μm absorption observed on Ceres [9,10,11]. Nevertheless, the remarkably flat UV drop-off detected on the cerean surface may, at least spectrally, correspond to highly aqueously altered and subsequently thermally metamorphosed CC material. Further alteration of this material on a parent body like Ceres may produce spectral changes affecting the 3 μm region, while showing no additional modification in the VIS/NIR region. Scenarios of thermal and geophysical evolution models allow Ceres' differentiation into a core of dehydrated silicates and a shell of hydrated silicates overlain by an icy shell [12,13]. The widespread occurence of material on the cerean surface, spectrally similar to thermally altered CC material, suggests that we possibly see the mineralogy of the hydrated-dehydrated boundary of Ceres exposed by impact gardening and simultaneous loss of the icy shell. Also differing recent models of a convecting mud ocean on Ceres, introduced by [14] and enhanced by [15], allow a lag deposit of aqueously altered fine material on the surface, spectrally corresponding to mildly heated Ivuna samples. References: [1] Sierks, H. et al. 2011. Space Sci. Rev., 163, 1-4, 263-327. [2] De Sanctis, C.M. et al. 2011. Space Sci. Rev., 163, 1-4, 329-369. [3] Prettyman, T.H. et al. 2011. Space Sci. Rev., 163, 1-4, 371-459. [4] Schäfer, T. et al., 2015. Icarus 265, 149-160. [5] Nathues, A. et al., 2015. Nature 528 (7581), 237-240. [6] Hiroi, T. et al., 1996. Lunar Planet. Sci. 27, 551. [7] Brearley, A.J., Jones, R.H., 1998. Chondritic meteorites. In: Planetary Materials, Papike, J.J. (Ed.). Rev. in Mineralogy and Geochem. 36 (1), ch. 3, 1-398. [8] Ivanova, M.A. et al., 2010. Meteoritics & Planet. Sci. 45 (7), 1108-1123. [9] King, T.V.V., et al., 1992. Science 255, 1551-1553. [10] De Sanctis, M.C. et al., 2015. Nature 528 (7581), 241-244. [11] Milliken, R.E., Rivkin, A.S., 2009. Nature Geosci. 2 (4), 258-261. [12] Castillo-Rogez, J.C., McCord, T.B., 2010. Icarus 205 (2), 443-459. [13] Neveu, M., Desch, S.J., Castillo-Rogez, J.C., 2015. J. Geophys. Res. Planets 120 (2), 123-154. [14] Travis, B.J. et al., 2015. Lunar Planet. Sci., #2360. [15] Neveu, M., Desch, S.J., 2015. Geophys. Res. Lett. 42 (23), 10197-10206.

Radio emission in Mercury magnetosphere

NASA Astrophysics Data System (ADS)

Varela, J.; Reville, V.; Brun, A. S.; Pantellini, F.; Zarka, P.

2016-10-01

Context. Active stars possess magnetized wind that has a direct impact on planets that can lead to radio emission. Mercury is a good test case to study the effect of the solar wind and interplanetary magnetic field (IMF) on radio emission driven in the planet magnetosphere. Such studies could be used as proxies to characterize the magnetic field topology and intensity of exoplanets. Aims: The aim of this study is to quantify the radio emission in the Hermean magnetosphere. Methods: We use the magnetohydrodynamic code PLUTO in spherical coordinates with an axisymmetric multipolar expansion for the Hermean magnetic field, to analyze the effect of the IMF orientation and intensity, as well as the hydrodynamic parameters of the solar wind (velocity, density and temperature), on the net power dissipated on the Hermean day and night side. We apply the formalism derived by Zarka et al. (2001, Astrophys. Space Sci., 277, 293), Zarka (2007, Planet. Space Sci., 55, 598) to infer the radio emission level from the net dissipated power. We perform a set of simulations with different hydrodynamic parameters of the solar wind, IMF orientations and intensities, that allow us to calculate the dissipated power distribution and infer the existence of radio emission hot spots on the planet day side, and to calculate the integrated radio emission of the Hermean magnetosphere. Results: The obtained radio emission distribution of dissipated power is determined by the IMF orientation (associated with the reconnection regions in the magnetosphere), although the radio emission strength is dependent on the IMF intensity and solar wind hydro parameters. The calculated total radio emission level is in agreement with the one estimated in Zarka et al. (2001, Astrophys. Space Sci., 277, 293) , between 5 × 105 and 2 × 106 W.

Physical properties of interplanetary dust: laboratory and numerical simulations

NASA Astrophysics Data System (ADS)

Hadamcik, Edith; Lasue, Jeremie; Levasseur-Regourd, Anny-Chantal; Renard, Jean-Baptiste; Buch, Arnaud; Carrasco, Nathalie; Cottin, Hervé; Fray, Nicolas; Guan, Yuan Yong; Szopa, Cyril

Laboratory light scattering measurements with the PROGRA2 experiment, in A300-CNES and ESA dedicated microgravity flights or in ground based configurations, offer an alternative to models for exploring the scattering properties of particles with structures too complex to be easily handled by computer simulations [1,2]. The technique allows the use of large size distributions (nanometers to hundreds of micrometers) and a large variety of materials, similar to those suspected to compose the interplanetary particles [3]. Asteroids are probably the source of compact particles, while comets have been shown to eject compact and fluffy materials [4]. Moreover giant planets provide further a small number of interplanetary particles. Some interstellar particles are also present. To choose the best samples and size distributions, we consider previous numerical models for the interplanetary particles and their evolution with solar distance. In this model, fluffy particles are simulated by fractal aggregates and compact particles by ellipsoids. The materials considered are silicates and carbonaceous compound. The silicate grains can be coated by the organics. Observations are fitted with two parameters: the size distribution of the particles and the ratio of silicates over carbonaceous compounds. From the light scattering properties of the particles, their equilibrium temperature can be calculated for different structures and composition. The variation of their optical properties and temperatures are studied with the heliocentric distance [5,6]. Results on analogs of cometary particles [7] and powdered meteorites as asteroidal particles will be presented and compared to numerical simulations as well as observations. Organics on cometary grains can constitute distributed sources if degraded by solar UV and heat [8, 9]. The optical properties of CxHyNz compounds are studied after thermal evolution [10]. As a first approach, they are used to simulate the evolution of cometary or interplanetary dust organics approaching the Sun. Albedo and polarization variations will be discussed. The polarization evolution will be compared to those obtained through observations [11]. Studies of the properties of our interplanetary dust cloud should provide information to better interpret observations of dust around exoplanets. Some of these planets are very close to their star. The thermal evolution of organics driven by chemical reactions will represent a fundamental knowledge to interpret the relevant polarimetric observations. We acknowledge CNES for funding the PROGRA2 experiment, CNES and ESA for the micro-gravity flights. [1] Renard J.-B. et al., Appl. Opt. 41, 609 (2002) [2] Hadamcik E. et al., In: Light scattering rev. 4, 31 (Kokhanovszky ed.), Springer -Praxis, Berlin (2009) [3] Mann I. et al., Space Sci. Rev. 110, 269 (2004) [4] Hoertz F. et al., Science 314, 716 (2006) [5] Lasue J. et al., Astron. Astrophys. 473, 641 (2007) [6] Levasseur-Regourd A.C et al., Planet Space Sci. 55, 1010 (2007) [7] Hadamcik E. et al., Icarus 190, 660 (2007) [8] Cottin H. et al., Adv. Space Res. 42, 2019 (2008) [9] Fray N. et al., Planet. Space Sci. 53, 1243 (2005) [10] Sciamma-O'Brien E. et al., Icarus, accepted [11] Levasseur-Regourd A.C., et al., In: Interplanetary dust, Gruen, Gustafson B., Dermott S., Fechtig H. (Eds), Springer, Berlin, 57 (2001)

Protecting the Moon for research: ILEWG report

NASA Astrophysics Data System (ADS)

Foing, Bernard H.

We give a report on recommendations with emphasis on environment protection, and since last COSPAR from ILEWG International conferences Exploration and Utilisation of the Moon on held at Cape Canaveral in 2008 (ICEUM10), and in Beijing in May 2010 with IAF (GLUC -ICEUM11). We discuss the different rationale for Moon exploration, as debated at ILEWG. ILEWG Science task group has listed priorities for scientific investigations: clues on the formation and evolution of rocky planets, accretion and bombardment in the inner solar system, comparative planetology processes (tectonic, volcanic, impact cratering, volatile delivery), records astrobiology, survival of organics; past, present and future life; sciences from a biology lunar laboratory. We discuss how to preserve Moon research potential in these areas while operating with instruments, landers, rover during a cooperative robotic village, and during the transition form lunar human outpost to permanent sustainable human base. We discuss how Moon-Mars Exploration can inspire solutions to global Earth sustained development with the trade-off of In-Situ Utilisation of resources; Establishment of permanent robotic infrastructures, Environmental and planetary protection aspects and lessons for Mars; Life sciences laboratories, and support to human exploration. Co-authors: ILEWG Task Groups on Science, Technology and Human Lunar Bases ILEWG Reference documents: http://sci.esa.int/ilewg -10th ILEWG Conference on Exploration and Utilisation of the Moon, NASA Lunar Ex-ploration Analysis Group-PSace Resources Roundtable, Cape Canaveral October 2008, pro-gramme online at http://sci.esa.int/ilewg/ -9th ILEWG Conference on Exploration and Utilisation of the Moon, ICEUM9 Sorrento 2007, programme online at http://sci.esa.int/ilewg/ -8th ILEWG Conference on Exploration and Utilisation of the Moon, Beijing July 2006, programme online at http://sci.esa.int/ilewg/ -The Moon and Near Earth Objects (P. Ehrenfreund , B.H. Foing, A. Cellino Editors), Ad-vances in Space Research, Volume 37, Issue 1, pp 1-192, 2006 -7th ILEWG Conference on Exploration and Utilisation of the Moon, Toronto Sept 2005, Programme and Proceedings on line at www.ilewg.org, R. Richards et al Editors -6th ILEWG Conference on Exploration and Utilisation of the Moon, Udaipur Nov. 2004, Proceedings ( N. Bhandari Editor), Journal Earth System Science, India, 114, No6, Dec 2005, pp. 573-841 -5th ILEWG Conference on Exploration and Utilisation of the Moon, Hawaii Nov 2003, Pro-ceedings ILC2005/ICEUM5 (S.M. Durst et al Editors), Vol 108, 1-576 pp, Science and Tech-nology Series, American Astronautical Society, 2004 -'The next steps in exploring deep space -A cosmic study by the IAA', W. Huntress, D. Stetson, R. Farquhar, J. Zimmerman, B. Clark, W. O'Neil, R. Bourke and B. Foing, Acta Astronautica, Vol 58, Issues 6-7, March-April 2006, p302-377 -IAA/ESA workshop on "Next Steps in Exploring Deep Space", ESTEC 22-23 sept. 2003 (B.H. Foing W. Huntress, conveners) Lunar Exploration, Planetary and Space Science, Vol 50, issue 14-15, Dec 2002 (B.H. Foing al) -ESLAB36 symposium on "Earth-like Planets and Moons", 2002, ESA-SP514, pp. 1-356, (B.H.Foing B. Battrick, editors) -'Lunar Exploration 2000', (B.H. Foing, D. Heather, Editors), Adv. Space Research Vol 30, Nr 8, 2002 -'Earth-Moon Relationships', Proceedings of the Conference held in Padova, Italy at the Ac-cademia Galileiana di Scienze Lettere ed Arti, Nov. 2000, (C. Barbieri and F. Rampazzi, Editors), in Earth, Moon , Planets Vol. 85-86, Nos 1-3, pp 1-575, 2001 -4th International Conference on Exploration and Utilisation of the Moon, ESTEC, 2000, ESA SP-462 (B.H. Foing M. Perry, editors) -Investing in Space: The Challenge for Europe. Long-Term Space Policy Committee, Second Report, May 1999. ESA-SP-2000 -2nd International Lunar Workshop, held at Kyoto in October 1996, Proceedings, H. Mizutani, editor, Japan Space Forum Publisher, 1997 International Lunar Workshop, 1994 May 31-June 3, Beatenberg, Switzerland. Proceedings. Ed. Balsiger, H. et al. European Space Agency, 1994. ESA-SP-1170 -Astronomy and Space Science from the Moon', Proceedings of COSPAR/IAF session at World Congress, Washington, (B.H. Foing et al editors), Advances in Space Research, Volume 14, Issue 6, 1994 -Mission to the Moon, Europe's Priorities for Scientific Exploration and Utilisation of the Moon', R.M. Bonnet et al, European Space Agency, ESA SP-1150, June 1992

Bianchi-III cosmological model with BVDP in modified f(R,T) theory

NASA Astrophysics Data System (ADS)

Mishra, R. K.; Dua, Heena; Chand, Avtar

2018-06-01

In present paper, we have investigated Bianchi type-III cosmological model in modified f(R,T) theory of gravity as proposed by Harko et al. (Phys. Rev. D 84:024020, 2011). To find the solution of field equations, we have used i) bilinear varying deceleration parameter (BVDP) (Mishra et al. in Astrophys. Space Sci. 361:259, 2016b) ii) the fact that expansion scalar of the space-time is proportional to the one of the components of the shear scalar. Physical and geometrical properties of the model have also been discussed along with the pictorial representation of various parameters. We have observed that presented model is compatible with the recent cosmological observations.

The Lunar dusty plasmas -levitation and transport.

NASA Astrophysics Data System (ADS)

Atamaniuk, Barbara; Rothkaehl, Hanna

Lunar dust can exhibit unusual behavior -due to electron photoemission via solar-UV radiation the lunar surface represents a complex plasma -"dusty plasma". The dust grains and lunar surface are electrostatically charged by the Moon's interaction with the local plasma environ-ment and the photoemission of electrons due to solar UV and X-rays. This effect causes the like-charged surface and dust particles to repel each other, and creates a near-surface electric field. Lunar dust must be treated as a dusty plasma. Using analytic (kinetic (Vlasov) and magnetohydrodynamic theory ) and numerical modeling we show physical processes related to levitation and transport dusty plasma on the Moon. These dust grains could affect the lunar environment for radio wave and plasma diagnostics and interfere with exploration activities. References: 1. Wilson T.L. (1992), in Analysis of Interplanetary Dust, M. Zolensky et al. AIP Conf.Proc. 310, 33-44 (AIP, NY), 2.Wilson T.L."LUNAR DUST AND DUSTY PLASMA PHYSICS".40th Lunar and Planetary Science Conference (2009), 3. Grün E., et al.(1993),Nature 363, 144. 4. Morfill G. and Grün E.(1979), Planet. Space Sci.. 27, 1269, 1283, 5. Manka R. and Michel F. (1971), Proc. 2nd Lun. Sci. Conf. 2, 1717 (MIT Press, Cambridge). 6. Manka R. et al.(1973), Lun. Sci.-III, 504. 7. Barbara Atamaniuk "Kinetic Description of Localized Plasma Structure in Dusty Plasmas". Czechoslovak Journal of Physics Vol.54 C 2004

Report from International Lunar Exploration Working Group (ILEWG) to COSPAR

NASA Astrophysics Data System (ADS)

Foing, Bernard H.

We refer to COSPAR and ILEWG ICEUM and lunar conferences and declarations [1-18]. We discuss how lunar missions SMART-1, Kaguya, Chang'E1&2, Chandrayaan-1, LCROSS, LRO, GRAIL, LADEE, Chang'E3 and upcoming missions contribute to lunar exploration objectives & roadmap. We present the GLUC/ICEUM11 declaration and give a report on ongoing relevant ILEWG community activities, with focus on: “1. Science and exploration - World-wide access to raw and derived (geophysical units) data products using consistent formats and coordinate systems will maximize return on investment. We call to develop and implement plans for generation, validation, and release of these data products. Data should be made available for scientific analysis and supporting the development and planning of future missions - There are still Outstanding Questions: Structure and composition of crust, mantle, and core and implications for the origin and evolution of the Earth-Moon system; Timing, origin, and consequences of late heavy bombardment; Impact processes and regolith evolution; Nature and origin of volatile emplacement; Implications for resource utilization. These questions require international cooperation and sharing of results in order to be answered in a cost-effective manner - Ground truth information on the lunar far side is missing and needed to address many important scientific questions, e.g. with a sample return from South Pole-Aitken Basin - Knowledge of the interior is poor relative to the surface, and is needed to address a number of key questions, e.g. with International Lunar Network for seismometry and other geophysical measurements - Lunar missions will be driven by exploration, resource utilization, and science; we should consider minimum science payload for every mission, e.g., landers and rovers should carry instruments to determine surface composition and mineralogy - It is felt important to have a shared database about previous missions available for free, so as to provide inputs to future missions, including a gap analysis of needed measurements. Highly resolved global data sets are required. Autonomous landing and hazard avoidance will depend on the best topographic map of the Moon, achievable by combining shared data. - New topics such as life sciences, partial gravity processes on the Moon should be followed in relation to future exploration needs.” http://sci.esa.int/ilewg/ http://sci.esa.int/ilewg/47170-gluc-iceum11-beijing-2010lunar-declaration/ References: [1] 1st International Lunar Workshop, Balsiger H. et al., Editors, European Space Agency, 1994. ESA-SP-1170. [2] 2nd International Lunar Workshop, Kyoto, H. Mizutani, editor, Japan Space Forum Publisher, 1997. [3] 3rd International Lunar Workshop, Moscow 1998, E. Galimov, editor. [4] ICEUM4, ESTEC, 2000, ESA SP-462, B.H. Foing & M. Perry, editors. [5] ICEUM5, Hawaii Nov 2003, Durst S.M. et al, Editors, Vol 108, 1-576 pp, Science and Technology Series, American Astronautical Society, 2004. [6] ICEUM6, Udaipur 2004, Bhandari N., Editor, Journal Earth Sys-tem Science, India, 114, No6, Dec 2005, pp. 573-841. [7] ICEUM7, Toronto Sept 2005, sci.esa.int/ilewg. [8] ICEUM8, Beijing July 2006, Journal of Chinese Society of Astronautics, Vol. 28 Sup., 2007, Ji W., Editor. [9] ICEUM9, Sorrento, Italy, Foing B., Espinasse S., Kosters G., Editors. http://sci.esa.int/iceum9, Dec. 2007), [11] Ehrenfreund, P., Foing, B.H., Cellino, A. Editors, The Moon and Near Earth Objects, ASR Vol 37, 1, 2006. [12] Foing, B.H. et al editors, 'Astronomy and Space Science from the Moon', ASR 14, 6, 1994. [13] Ip W.-H., Foing, B.H., Masson Ph.L., editors, The Moon and Mars, ASR Vol 23, 11, 1999. [14] Foing, B.H. et al, editor, Lunar Exploration, Planetary and Space Science, Vol 50, 14-15, 2002. [15] Foing, B.H., Heather, D. editors, 'Lunar Exploration 2000', ASR Vol 30, Nr 8, 2002. [16] Huntress, W. et al 'The next steps in exploring deep space - A cosmic study by the IAA', Acta Astronautica, Vol 58, Issues 6-7, 2006, p302-377. [17] http://sci.esa.int/ilewg/43654-declaration-iceum10-leag-srr-florida-2008/ [18] Ehrenfreund P. et al (COSPAR planetary exploration panel report) 2012, ASR Vol 49, Nr 1, pp. 2-48.

Using Lunar Impact Basin Relaxation to Test Impact Flux Models

NASA Astrophysics Data System (ADS)

Nimmo, F.; Conrad, J. W.; Neumann, G. A.; Kamata, S.; Fassett, C.

2017-12-01

Gravity data obtained by the GRAIL mission [1] has constrained the number and distribution of lunar impact basins [2]. We analyzed crater densities for newly-proposed basins to assign relative ages. The extent to which a basin is relaxed is calculated using GRAIL-derived crustal thickness models [3] by comparing the mantle uplift under basins to the surrounding region. With our catalog we can investigate the distribution of basin properties through relative time. We identify a relaxation state transition (RT) around the pre-Nectarian 4 relative age group for basins with diameters > 450 km, similar to previous results using a pre-GRAIL basin catalog [4]. This RT likely signals a change in the global thermal state of the crust, representing the time at which the lunar moho temperature fell below 1400 K [4]. This transition happens 50-100 million years (Myr) after the lunar magma ocean (LMO) solidifies [4]. Based on models and inferences of LMO solidification [5, 6] the RT is expected to occur at 4.25-4.50 Ga, depending on the rate of cooling once a crustal lid has formed [5] and the amount of tidal heating in the early crust [6]. Monotonically declining impact flux models, such as [7] and [8] predict a younger RT; 4.07-4.08 and 4.24-4.27 Ga respectively. A scaled-down version of [8] can fit the RT but fails to match the observed number of younger, unrelaxed basins. Models that invoke a later transient increase in impact flux can reproduce the inferred RT time; for instance, the model of [9] gives a RT age of 4.43-4.46 Ga. This model matches the number of younger basins and implies that basin preservation started at 4.49 Ga, likely before the LMO completely solidified. [1] Zuber M.T. et al. (2013) Science, 339, 668-671. [2] Neumann G.A. et al. (2015) Science Advances, 1, e1500852. [3] Wieczorek M.A. (2013) Science, 339, 671-675. [4] Kamata S. et al. (2015) Icarus, 250, 492-504. [5] Elkins-Tanton L.T. et al. (2011) Earth Planet. Sci. Lett., 304, 326-336. [6] Meyer, J. et al. (2010) Icarus, 208, 1-10. [7] Robbins S.J. (2014) Earth Planet. Sci. Lett., 403, 188-198. [8] Neukum G. et al. (2001) Space Sci. Rev., 96, 55-86. [9] Morbidelli A. et al. (2012) Earth Planet. Sci. Lett., 355, 144-151.

Interpretation of spectrophotometric surface properties of comet 67P/Churyumov-Gerasimenko by laboratory simulations of cometary analogs

NASA Astrophysics Data System (ADS)

Jost, Bernhard; Pommerol, Antoine; Poch, Olivier; Carrasco, Nathalie; Szopa, Cyril; Thomas, Nicolas

2015-11-01

The OSIRIS imaging system [1] onboard European Space Agency’s Rosetta mission has been orbiting the comet 67P/Churyumov-Gerasimenko (67P) since August 2014. It provides an enormous quantity of high resolution images of the nucleus in the visible spectral range. 67P revealed an unexpected diversity of complex surface structures and spectral properties have also been measured [2].To better interpret this data, a profound knowledge of laboratory analogs of cometary surfaces is essential. For this reason we have set up the LOSSy laboratory (Laboratory for Outflow Studies of Sublimating Materials) to study the spectrophotometric properties of ice-bearing cometary nucleus analogs. The main focus lies on the characterization of the surface evolution under simulated space conditions. The laboratory is equipped with two facilities: the PHIRE-2 radio-goniometer [3], designed to measure the bidirectional visible reflectance of samples under a wide range of geometries and the SCITEAS simulation chamber [4], designed to study the evolution of icy samples subliming under low pressure/temperature conditions by hyperspectral imaging in the VIS-NIR range. Different microscopes complement the two facilities.We present laboratory data of different types of fine grained ice particles mixed with non-volatile components (complex organic matter and minerals). As the ice sublimes, a deposition lag of non-volatile constituents is built-up on top of the ice, possibly mimic a cometary surface. The bidirectional reflectance of the samples have been characterized before and after the sublimation process.A comparison of our laboratory findings with recent OSIRIS data [5] will be presented.[1] Keller, H. U., et al., 2007, Space Sci. Rev., 128, 26[2] Thomas, N. , 2015, Science, 347, Issue 6220, aaa0440[3] Jost, B., submitted, Icarus[4] Pommerol, A., et al., 2015. Planet Space Sci 109:106-122.[5] Fornasier, S., et al., in press. Icarus, arXiv:1505.06888

Dust Plasma Environment between Saturn's Rings and Mimas' L Shell

NASA Astrophysics Data System (ADS)

Sittler, E. C., Jr.; Johnson, R. E.

2015-12-01

We will present a new analysis of the available data on the extension of Saturn's ring atmosphere into the magnetosphere beyond the A-ring outer edge (Johnson et al. 2006) out to the orbit of Mimas. This is an interesting region in Saturn's magnetosphere containing the F and G rings and penetrated by the E-ring and the Enceladus neutral torus. This analysis will include a comparison of the Cassini Plasma Spectrometer (CAPS) plasma data, Radio and Plasma Wave Spectrometer (RPWS) plasma wave observations, RPWS Langmuir Probe (LP) observations and Cassini Dust Analyzer (CDA). The central focus will be on the dust plasma interactions. Specific attention will be paid to the SOI data for which there are considerable differences between the ion and electron densities (Elrod et al., 2012) while for other close flybys inside Mimas' L shell such differences are less obvious but the electron data appear to be highly variable. Using previous identifications of nm particles (Jones et al., 2010) inferred from CAPS data and micron sized particles that can be detected by CDA (Kempf et al., 2006) and the RPWS plasma wave dust impact signatures (Kurth et al., 2006) we will attempt to infer the full particle size distribution between the A-ring and Mimas. These nm to micron sized particles can accumulate considerable charge and under certain circumstances could account for the radial trend in the ion density described in Elrod et al. (2014) a critical issue in preparation for the Cassini proximal orbits. References: Elrod, M.K., W.-L. Tseng, R.J. Wilson, R.E. Johnson, J. Geophys. Res., 117, A03207, 2012. Elrod, M.K., W-L Tseng, A.K. Woodson, R.E. Johnson, Icarus, 242, 130-137,2014. Johnson, R. E., et al., Icarus, 180, 393-402, 2006. Jones, G. H., et al., Geophys. Res. Lett., 36, L16204, 2009. Kempf, S., U. Beckmann, R. Srama, M. Horanyi, S. Auerd, E. Grun, Planet. Space Sci., 54, 999-1006, 2006. Kurth, W. S., T.F. Averkamp, D.A. Gurnett, Z. Wang, Planet. Space Sci., 54, 988-998, 2006.

DOE Office of Scientific and Technical Information (OSTI.GOV)

Valerio-Lizarraga, Cristhian A., E-mail: cristhian.alfonso.valerio.lizarraga@cern.ch; Departamento de Investigación en Física, Universidad de Sonora, Hermosillo; Lallement, Jean-Baptiste

The space charge effect of low energy, unbunched ion beams can be compensated by the trapping of ions or electrons into the beam potential. This has been studied for the 45 keV negative hydrogen ion beam in the CERN Linac4 Low Energy Beam Transport using the package IBSimu [T. Kalvas et al., Rev. Sci. Instrum. 81, 02B703 (2010)], which allows the space charge calculation of the particle trajectories. The results of the beam simulations will be compared to emittance measurements of an H{sup −} beam at the CERN Linac4 3 MeV test stand, where the injection of hydrogen gas directlymore » into the beam transport region has been used to modify the space charge compensation degree.« less

Investigating the sensitivity of nitric oxide infrared emissions to electron impact

NASA Astrophysics Data System (ADS)

Campbell, L.; Brunger, M. J.; Allan, M.

2008-05-01

Integral cross sections for low energy electron excitation of the 0→1, 0→2 and 0→3 vibrational modes in nitric oxide have quite recently become available [Trevisan et al. PRA 71, 052714 (2005)]. In this study we adapt our recent work [Campbell and Brunger GRL, in press (2007)], to look at the effect of these new cross sections on the production of nitric oxide infrared radiation. Predictions from our model are compared with measurements from Espy et al. [Planet. Space Sci. 36, 543 (1988)], with the inclusion of the new cross sections improving the agreement of the shape of the spectrum with the measurements.

SOFIA Science Imagery

NASA Image and Video Library

2017-09-14

SCI2016_0006: Map of Cepheus E emphasizing the jets of material flowing to the upper left and lower right from the protostar. The protostar itself is the central yellow-red 'blob" in the colored background map of hydrogen emission made at a wavelength of 4.5 microns by the Spitzer infrared space telescope. The contour curves show the strength of emission from cool carbon monoxide gas measured by the Plateau de Bure radio telescope located in the French Alps. Lefloch et al. used GREAT on SOFIA to measure the amount and velocity of hot carbon monoxide gas at multiple positions along both "wings" of the outflow jet. Credit: Lefloch et al. 2015 Figure 1

Structure of carbonate melts at high pressure

NASA Astrophysics Data System (ADS)

Hudspeth, J.; Sanloup, C.; Cochain, B.; Konopkova, Z.; Afonina, V.; Morgenroth, W.

2015-12-01

Carbonate melts are rare magmas with only a single active volcano (Oldoinyo Lengai,Tanzania [1]). They are of fundamental interest for their role in the Earth's deep carbon cycle and are of immense economic importance due to their affinity for REE strategic metals (niobium, uranium, tantalum, etc). They have remarkable physical properties such as very low viscosity [2] and magmatic temperatures for alkaline carbonate lavas [3] and it has been predicted that their compressibility could be significantly higher than that of silicate melts [4,5]. Despite the atomic structure of carbonate melts being fundamental for controlling their physical and chemical behavior in natural systems, very few structural studies have been reported and these have been largely computational. Here we present initial structural investigations of carbonate melts at mantle pressures using in situ x-ray diffraction in diamond anvil cells. The structure factor S(Q) is transformed to obtain the real space pair distribution function G(R) which describes the local and intermediate range atomic ordering allowing bond length and coordination number changes with pressure to be determined. [1] Krafft and Keller, Science 245:168-170, 1989 [2] Yono et al., Nat. Commun. 5:5091, 2014 [3] Dobson et al., Earth Planet. Sci. Lett. 143:207-215, 1996 [4] Genge et al., Earth Planet. Sci. Lett. 131:225-238, 1995 [5] Jones et al., Rev. Mineral. Geochem. 75:289-322, 2013

Inter-University Upper Atmosphere Global Observation Network (IUGONET) Metadata Database and Its Interoperability

NASA Astrophysics Data System (ADS)

Yatagai, A. I.; Iyemori, T.; Ritschel, B.; Koyama, Y.; Hori, T.; Abe, S.; Tanaka, Y.; Shinbori, A.; Umemura, N.; Sato, Y.; Yagi, M.; Ueno, S.; Hashiguchi, N. O.; Kaneda, N.; Belehaki, A.; Hapgood, M. A.

2013-12-01

The IUGONET is a Japanese program to build a metadata database for ground-based observations of the upper atmosphere [1]. The project began in 2009 with five Japanese institutions which archive data observed by radars, magnetometers, photometers, radio telescopes and helioscopes, and so on, at various altitudes from the Earth's surface to the Sun. Systems have been developed to allow searching of the above described metadata. We have been updating the system and adding new and updated metadata. The IUGONET development team adopted the SPASE metadata model [2] to describe the upper atmosphere data. This model is used as the common metadata format by the virtual observatories for solar-terrestrial physics. It includes metadata referring to each data file (called a 'Granule'), which enable a search for data files as well as data sets. Further details are described in [2] and [3]. Currently, three additional Japanese institutions are being incorporated in IUGONET. Furthermore, metadata of observations of the troposphere, taken at the observatories of the middle and upper atmosphere radar at Shigaraki and the Meteor radar in Indonesia, have been incorporated. These additions will contribute to efficient interdisciplinary scientific research. In the beginning of 2013, the registration of the 'Observatory' and 'Instrument' metadata was completed, which makes it easy to overview of the metadata database. The number of registered metadata as of the end of July, totalled 8.8 million, including 793 observatories and 878 instruments. It is important to promote interoperability and/or metadata exchange between the database development groups. A memorandum of agreement has been signed with the European Near-Earth Space Data Infrastructure for e-Science (ESPAS) project, which has similar objectives to IUGONET with regard to a framework for formal collaboration. Furthermore, observations by satellites and the International Space Station are being incorporated with a view for making/linking metadata databases. The development of effective data systems will contribute to the progress of scientific research on solar terrestrial physics, climate and the geophysical environment. Any kind of cooperation, metadata input and feedback, especially for linkage of the databases, is welcomed. References 1. Hayashi, H. et al., Inter-university Upper Atmosphere Global Observation Network (IUGONET), Data Sci. J., 12, WDS179-184, 2013. 2. King, T. et al., SPASE 2.0: A standard data model for space physics. Earth Sci. Inform. 3, 67-73, 2010, doi:10.1007/s12145-010-0053-4. 3. Hori, T., et al., Development of IUGONET metadata format and metadata management system. J. Space Sci. Info. Jpn., 105-111, 2012. (in Japanese)

Increased delivery of condensation nuclei during the Late Heavy Bombardment to the terrestrial and martian atmospheres

NASA Astrophysics Data System (ADS)

Losiak, Anna

2014-05-01

During the period of the Late Heavy Bombardment (LHB), between 4.1 and 3.8 Ga, the impact rate within the entire Solar System was up to a few thousand times higher than the current value (Ryder 2002, Bottke et al. 2012, Fassett and Minton 2013). Multiple basin-forming events on inner planets that occurred during this time had a strong but short-lasting (up to few thousands of years) effect on atmospheres of Earth and Mars (Sleep et al. 1989, Segura et al. 2002, 2012). However, the role of the continuous flux of smaller impactors has not been assessed so far. We calculated the amount of meteoric material in the 10^-3 kg to 106 kg size range delivered to Earth and Mars during the LHB based on the impact flux at the top of the Earth's atmosphere based on results from Bland and Artemieva (2006). Those values were recalculated for Mars based on Ivanov and Hartmann (2009) and then recalculated to the LHB peak based on estimates from Ryder (2002), Bottke et al. (2012), Fassett and Minton (2013). During the LHB, the amount of meteoritic material within this size range delivered to Earth was up to ~1.7*10^10 kg/year and 1.4*10^10 kg/year for Mars. The impactors that ablate and are disrupted during atmospheric entry can serve as cloud condensation nuclei (Rosen 1968, Hunten et al. 1980, Ogurtsov and Raspopov 2011). The amount of material delivered during LHB to the upper stratosphere and lower mezosphere (Hunten et al. 1980, Bland and Artemieva 2006) is comparable to the current terrestrial annual emission of mineral cloud condensation nuclei of 0.5-8*10^12 kg/year (Tegen 2003). On Mars, the availability of condensation nuclei is one of the main factors guiding water-ice cloud formation (Montmessin et al. 2004), which is in turn one of the main climatic factors influencing the hydrological cycle (Michaels et al. 2006) and radiative balance of the planet (Haberle et al. 1999, Wordsworth et al. 2013, Urata and Toon 2013). Increased delivery of condensation nuclei during the LHB should be taken into account when constructing models of terrestrial and Martian climates around 4 Ga. Bland P.A., Artemieva N.A. (2006) Meteorit.Planet.Sci. 41:607-631. Bottke W.F. et al. (2012) Nature 485: 78-81. Fassett C.I., Minton D.A. (2013) Nat.Geosci. 6:520-524 (2013). Hunten D.M. et al. (1980) J.Atmos.Sci. 37:1342-1357. Haberle R.M. et al. (1999) J.Geophys.Res. 104:8957-8974. Ivanov B.A., Hartmann W.K. (2009) Planets and Moons: Treatise on Geophysics (eds. Spohn T.): 207-243. Michaels T.I. et al. (2006) Geophys.Res.Lett. 33:L16201. Montmessin F. et al. (2004) J.Geophys.Res. 109:E10004. Ogurtsov M.G., Raspopov O.M. (2011) Geomagnetism&Aeronomy 51:275-283. Rosen J.M. (1968) Space Sci.Rev. 9:58-89. Ryder G. (2002) J.Geophys.Res. 107: doi:10.1029/2001JE001583. Segura T.L. et al. (2002) Science 298:1977-1980. Segura T.L. et al. (2012) Icarus 220:144-148. Sleep N.S. et al. (1989) Nature 342:139-142. Tegen I. (2003) Quat.Sci.Rev. 22:1821-1834. Urata R.A., Toon O.B. (2013) Icarus 226:229-250. Wordsworth R. et al. (2012) Icarus 222:1-19.

Space weathering of asteroids: Lessons from Itokawa for future observations

NASA Astrophysics Data System (ADS)

Sasaki, Sho; HIroi, Takahiro

2016-07-01

Introduction Space weathering of surface silicate minerals is the main process that should control the change of brightness and color of airless silicate bodies such and the Moon, Mercury and asteroids. Spectra of S-type asteroids exhibit more overall depletion and reddening, and more weakening of absorption bands than spectra of ordinary chondrites. These spectral mismatches are explained by the space weathering, where the primary proven mechanism of such spectral change is production of nanophase metallic iron particles (npFe0) 1), which were confirmed in the amorphous rim of lunar soil grains 2,3). Vapor-deposition through at high-velocity dust particle impacts as well as implantation of intensive solar wind ions would be responsible for producing the space weathering rims bearing nano-iron particles (npFe0). Simulation experiments using nanosecond pulse laser successfully produced vapor-deposition type npFe0 to change optical properties 4,5,6). Laser experiments showed that pyroxene would be weathered less than olivine, for pyroxene, pulse laser irradiation produced melt (amorphous) droplets containing npFe0, rather than vapour deposited rim that should provide stronger optical effect trough multiple scattering of incidental light. Itokawa Observed by Remote Sensing In November 2005, Japanese Asteroid Sample Return Mission HAYABUSA spacecraft rendezvoused S-type asteroid (25143) Itokawa. Optically, the surface of Itokawa is divided into brighter (and bluer) areas and darker (and redder) areas 7,8). In rough zones, dark boulder-rich surfaces usually superpose on bright materials. The near-infrared spectrometer (NIRS) confirmed previous disk-integrated results that suggested Itokawa's spectrum closely matched a weakly weathered LL5/6 chondrite 9). Although the surface is covered with rocks and is apparently lack of fine regolith, Itokawa's surface show darkening and reddening by space weathering. Experimental results suggest rocky meteorite fragments can be weathered. The presence of opposition effect in rocky terrain of Itokawa suggested that the surface would be covered by particulate materials or porous enough to scatter light. Spectral variations were observed, that can be explained by Hapke's space weathering model, where the amount of npFe0 controls spectral reddening. As for color variation of Itokawa, we can interpret that seismic shaking caused by impacts or planetary encounters should lead to exposure of underlying relatively fresh bright area by removing weathered darker boulder-rich layer. Itokawa - Evidence from Returned Samples In 2011, HAYABUSA returned more than 1000 particulate samples of Itokawa back to the Earth. Analysis of mineral assemblies and composition of Itokawa particles supports that Itokawa has LL-chondrite composition. The most notable discoveries in Itokawa particles is amorphous space-weathering rims containing npFe0 16, 17, 18). Sometimes ion-implanted type-II layers contains vesicles, probably due mainly to trapping solar wind energetic helium with penetration depth up to a few tens µm (composite vesicular rim in 17, 18)). Large vesicles are observed as blisters on the surface of Itokawa particles. Matsumoto et al. 18) identified space weathered rims with blisters on eleven out of twenty regolith particles of Itokawa. It was confirmed that a blister corresponds to a vesicle in npFe0-bearing amorphous layer. These rims with blisters are heterogeneously distributed even in one particle. Sometimes blistered rims are observed in opposite surfaces of the same particle. This is a strong evidence of regolith mixing. So far, there is no correlation between the blister distribution and surface morphologies such as roundness of particles. A few 10 nm amorphous rim can be developed in timescale 1000 yr (based on solar flare density, Regolith mixing processes may prolong timescale of optical maturation on smooth regions of Itokawa. References 1) Hapke B., Cassidy, W. And Wells. E.: Effects of vapor-phase deposition processes on the optical, chemical, and magnetic properties of the lunar regolith, Moon, 13 (1975), 339-353 2) Keller L. P. and McKay D. S.: Science, 261 (1993), 1305-1307. 3) Pieters C. M., et al. Meteorit.: Planet. Sci., 35 (2000), 1101-1107. 4) Yamada, M., et al.: Earth Planets Space 51 (1999), 1255-1265. 5) Sasaki, S., et al.: Nature 410 (2001), 555-557. 6) Brunetto, R., et al.: Icarus 180 (1995), 546-554. 10) Brunetto, R., Loeffler, M. J., Nesvorny, D., Sasaki, S., and Strazzulla, G.: Asteroid Surface Alteration by Space Weathering Processes, in Asteroid IV, Univ. Arizona Press (2015). 11) Hirata, N., et al.: Icarus 200 (2009), 486-502. 12) Ishiguro, M.: Scattered light correction of Hayabusa/AMICA data and quantitative spectral comparisons of Itokawa, Pub. Astron. Soc. Japan, 66 (2014), 55 13) Noguchi, T., et al.: Icarus 206 (2010), 319-326. 14) Nakamura, T., et al.: Science 333 (2011), 1113-1116. 15] Tsuchiyama, A., et al.: Science 333 (2011), 1125-1128. [6) Noguchi, T., et al.: Science 333 (2011), 1121-1125. 17) Noguchi, T., et al.: Meteorit. Planet. Sci., 49 (2014), 188-214. 18) Matsumoto, T. et al. Icarus (2015) 257, 230. 19) Noble S. K. et al. (2011) Meteorit. Planet. Sci., 45 (2011), 2007.

Asteroseismic modelling of the solar-like star β Hydri

NASA Astrophysics Data System (ADS)

Doğan, G.; Brandão, I. M.; Bedding, T. R.; Christensen-Dalsgaard, J.; Cunha, M. S.; Kjeldsen, H.

2010-07-01

We present the results of modelling the subgiant star β Hydri using seismic observational constraints. We have computed several grids of stellar evolutionary tracks using the Aarhus STellar Evolution Code (ASTEC, Christensen-Dalsgaard in Astrophys. Space Sci. 316:13, 2008a), with and without helium diffusion and settling. For those models on each track that are located at the observationally determined position of β Hydri in the Hertzsprung-Russell (HR) diagram, we have calculated the oscillation frequencies using the Aarhus adiabatic pulsation package (ADIPLS, Christensen-Dalsgaard in Astrophys. Space Sci. 316:113, 2008b). Applying the near-surface corrections to the calculated frequencies using the empirical law presented by Kjeldsen et al. (Astrophys. J. 683:L175, 2008), we have compared the corrected model frequencies with the observed frequencies of the star. We show that after correcting the frequencies for the near-surface effects, we have a fairly good fit for both l=0 and l=2 frequencies. We also have good agreement between the observed and calculated l=1 mode frequencies, although there is room for improvement in order to fit all the observed mixed modes simultaneously.

Student-Generated Scientific Inquiry for Elementary Education Undergraduates: Course Development, Outcomes and Implications

ERIC Educational Resources Information Center

Salter, Irene; Atkins, Leslie

2013-01-01

While some researchers have argued for science classrooms that embrace open-inquiry by engaging students in doing science as scientists do (cf. National Research Council [NRC] 1996; Driver et al. in "Sci Educ" 84:287-312, 2000; Windschitl et al. in "Sci Educ" 87(1):112-143, 2008), others have argued that open-inquiry is impractical, ineffective,…

Data supporting Al-Abed et al., Environ. Sci.: Nano, 2016,

EPA Pesticide Factsheets

Data files representing each of the Figures and Tables published in Al-Abed et al., Environ. Sci.: Nano, 2016,3, 593. The data file names identify the Figure or Table and each file contains an internal set of data definitionsThis dataset is associated with the following publication:Al-Abed, S.R., J. Virkutyte, J. Ortenzio , R.M. McCarrick, L. Degn, R. Zucker , N. Coates , K. Cleveland, H. Ma, S. Diamond, K. Dreher , and W. Boyes. Environmental aging alters AI(OH)3 coating of TiO2 nanoparticles enhancing their photocatalytic and phototoxicity activities. Environmental Science: Nano. RSC Publishing, Cambridge, UK, N/A, (2016).

Incorporating English Language Teaching through Science for K-2 Teachers

ERIC Educational Resources Information Center

Shanahan, Therese; Shea, Lauren M.

2012-01-01

English learners are faced with the dual challenge of acquiring English while learning academic content through the medium of the new language (Lee et al. in "J Res Sci Teach" 45(6):726-747, 2008; Stoddart et al. in "J Res Sci Teach" 39(8):664-687, 2002) and therefore need specific accommodations to achieve in both English and the content areas.…

Greening of the Sahara - a paleo perspective on the history of water in the Middle East and North Africa

NASA Astrophysics Data System (ADS)

Bar-Matthews, M.

2012-04-01

The Middle-East, mostly at its southern edge together with North Africa, the northern edge of the Sahara Desert, are located at the boundary between high- to-mid latitude and tropical-subtropical climate systems. The geographical duality of desert adjacent to Mediterranean-type climate regions played and still plays a major role on the water availability. Thanks to the number of important paleoclimate studies that been made on accurate dating of cave speleothems in Southern Arabia and Oman (Fleitmann et al., 2011) and in the northeast Sahara, the Negev Desert Israel (Vaks et al., 2010) and the study of sapropels in Eastern and central Mediterranean (Almogi-Labin et al., 2009; Osborne et al, 2008), it is clear that the region was graced with water during peak interglacials when the African monsoon and westerly storm/rainfall systems intensified. Northward penetration of the Inter Tropical Convergence Zone over the Arabian and African continents resulted in increased discharge of the Nile River and rivers that emerged from central Sahara into the Eastern Mediterranean Sea. Correspondingly, enhanced westerly wind activity led to an increase in rainfall from Atlantic-Mediterranean sources over the entire Mediterranean basin, which even penetrated south into the north-east corner of the Sahara Desert. The Saharo-Arabian Desert became narrower and climatic "windows" opened for the dispersal of hominids and animals out of the African continent at 250-239, 210-193, 138-120, 108-98, 87-84 and 10-6.5 ka BP, with severe dry conditions in between. Greening of the Sahara Desert at these intervals is supported also by various marine and terrestrial records, such as corals, lakes, tufa deposits and archeological findings. Dry conditions prevailed in the Sahara desert during glacials. This is in contrast to the climatic conditions in the Eastern Mediterranean coastal region and the Jordan Rift Valley (Bar-Matthews et al., 2003; Lisker et al., 2010), where water was available for humans and animals who enjoyed a variety of ecological niches for living (Frumkin et al., 2011). Almogi-Labin, A. et a.l (2009) Quat. Sci. Rev. 28, 2882-2896. Bar-Matthews, M. et al (2003 Geochim. Cosmochim. Acta 67, 3181-99. Fleitmann, D. et al. (2011). Quat. Sci. Rev. 30, 783-787. Frumkin, et al. A. (2011). Jour. Human Evol. 60, 437-451 Lisker et al, (2010). Quat. Sci. Rev 29, 1201-1211. Osborne A.H. et al. (2008). Proc. Nat. Acad. Sci. 105, 16444-16447 Vaks et al. (2010). Quat. Sci. Rev. 29, 2647-2662.

Mexican Space Weather Service (SCiESMEX)

NASA Astrophysics Data System (ADS)

Gonzalez-Esparza, J. A.; De la Luz, V.; Corona-Romero, P.; Mejia-Ambriz, J. C.; Gonzalez, L. X.; Sergeeva, M. A.; Romero-Hernandez, E.; Aguilar-Rodriguez, E.

2017-01-01

Legislative modifications of the General Civil Protection Law in Mexico in 2014 included specific references to space hazards and space weather phenomena. The legislation is consistent with United Nations promotion of international engagement and cooperation on space weather awareness, studies, and monitoring. These internal and external conditions motivated the creation of a space weather service in Mexico. The Mexican Space Weather Service (SCiESMEX in Spanish) (www.sciesmex.unam.mx) was initiated in October 2014 and is operated by the Institute of Geophysics at the Universidad Nacional Autonoma de Mexico (UNAM). SCiESMEX became a Regional Warning Center of the International Space Environment Services (ISES) in June 2015. We present the characteristics of the service, some products, and the initial actions for developing a space weather strategy in Mexico. The service operates a computing infrastructure including a web application, data repository, and a high-performance computing server to run numerical models. SCiESMEX uses data of the ground-based instrumental network of the National Space Weather Laboratory (LANCE), covering solar radio burst emissions, solar wind and interplanetary disturbances (by interplanetary scintillation observations), geomagnetic measurements, and analysis of the total electron content (TEC) of the ionosphere (by employing data from local networks of GPS receiver stations).

Numerical modeling of Stickney crater and its aftermath

NASA Astrophysics Data System (ADS)

Schwartz, Stephen R.; Michel, Patrick; Bruck Syal, Megan; Owen, J. Michael; Miller, Paul L.; Richardson, Derek C.; Zhang, Yun

2016-10-01

Phobos is characterized by a large crater called Stickney. Its collisional formation and its aftermath have important implications on the final structure, morphology, and surface properties of Phobos that still need further clarification. This is particularly important in the current environment, with space mission concepts to Phobos under active study by several space agencies. SPH hydrocode simulations of the impact that formed Stickney crater [1] have been performed. Using the Soft-Sphere Discrete Element Method (SSDEM) collisional routine of the N-body code pkdgrav [2], we take the outcome of SPH simulations as inputs and model the ensuing phase of the crater formation process and its ejecta evolution under the gravitational influence of Phobos and Mars. In our simulations, about 9 million particles comprise Phobos' shape [3], and the evolution of particles that are expected to form or leave the crater is followed using multiple plausible orbits for Phobos around Mars. We track the immediate fate of low-speed ejecta (~3-8 m/s), allowing us to test an hypothesis [4] that they may scour certain groove marks that have been observed on Phobos' surface and to quantify the amounts and locations of re-impacting ejecta. We also compute the orbital fate of ejecta whose speed is below the system escape speed (about 3 km/s). This allows us to estimate the thickness and distribution of the final ejecta blanket and to check whether crater chains may form. Finally, particles forming the crater walls are followed until achieving stability, allowing us to estimate the final crater depth and diameter. We will show examples of these simulations from a set of SPH initial conditions and over a range of parameters (e.g., material friction coefficients). Work ongoing to cover a larger range of plausible impact conditions, allowing us to explore different scenarios to explain Phobos' observed properties and to infer more, giving useful constraints to space mission studies. [1] Bruck Syal, M. et al. (this meeting); [2] Schwartz, S.R. et al. 2012, Granul. Matter 14, 363; [3] Willner, K. et al. 2010, E. Earth Planet. Sci. Lett. 294, 541; [4] Wilson, L. & Head, J.W. 2015, Planet. Space Sci. 105, 26.

Deployable Camera (DCAM3) System for Observation of Hayabusa2 Impact Experiment

NASA Astrophysics Data System (ADS)

Sawada, Hirotaka; Ogawa, Kazunori; Shirai, Kei; Kimura, Shinichi; Hiromori, Yuichi; Mimasu, Yuya

2017-07-01

An asteroid exploration probe "Hayabusa2", that was developed by Japan Aerospace Exploration Agency (JAXA), was launched on December 3rd, 2014 to challenge complicated and accurate operations during the mission phase around the C-type asteroid 162137 Ryugu (1999 JU3) (Tsuda et al. in Acta Astron. 91:356-362, 2013). An impact experiment on a surface of the asteroid will be conducted using the Small Carry-on Impactor (SCI) system, which will be the world's first artificial crater creation experiment on asteroids (Saiki et al. in Proc. International Astronautical Congress, IAC-12.A3.4.8, 2012, Acta Astron. 84:227-236, 2013a; Proc. International Symposium on Space Technology and Science, 2013b). We developed a new micro Deployable CAMera (DCAM3) system for remote observations of the impact phenomenon applying our conventional DCAM technology that is one of the smallest probes in space missions and gained a great success in past Japanese mission IKAROS (Interplanetary Kite-craft Accelerated by Radiation Of the Sun). DCAM3 is a miniaturized separable unit that contains two cameras and radio communication devices for transmission image data to the mothership "Hayabusa2", and it observes the impact experiment at an unsafe region in where the "Hayabusa2" is difficult to stay because of a risk of exploding and impacting debris hitting. In this paper, we report details of the DCAM3 system and development results as well as our mission plan for the DCAM3 observation during the SCI experiment.

Mapping Ejecta Thickness Around Small Lunar Craters

NASA Astrophysics Data System (ADS)

Brunner, A.; Robinson, M. S.

2016-12-01

Detailed knowledge of the distribution of ejecta around small ( 1 km) craters is still a key missing piece in our understanding of crater formation. McGetchin et al. [1] compiled data from lunar, terrestrial, and synthetic craters to generate a semi-empirical model of radial ejecta distribution. Despite the abundance of models, experiments, and previous field and remote sensing studies of this problem, images from the 0.5 m/pixel Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC) [2] provides the first chance to quantify the extent and thickness of ejecta around kilometer scale lunar craters. Impacts excavate fresh (brighter) material from below the more weathered (darker) surface, forming a relatively bright ejecta blanket. Over time space weathering tends to lower the reflectance of the ejected fresh material [3] resulting in the fading of albedo signatures around craters. Relatively small impacts that excavate through the high reflectance immature ejecta of larger fresh craters provide the means of estimating ejecta thickness. These subsequent impacts may excavate material from within the high reflectance ejecta layer or from beneath that layer to the lower-reflectance mature pre-impact surface. The reflectance of the ejecta around a subsequent impact allows us to categorize it as either an upper or lower limit on the ejecta thickness at that location. The excavation depth of each crater found in the ejecta blanket is approximated by assuming a depth-to-diameter relationship relevant for lunar simple craters [4, e.g.]. Preliminary results [Figure] show that this technique is valuable for finding the radially averaged profile of the ejecta thickness and that the data are roughly consistent with the McGetchin equation. However, data from craters with asymmetric ejecta blankets are harder to interpret. [1] McGetchin et al. (1973) Earth Planet. Sci. Lett., 20, 226-236. [2] Robinson et al. (2010) Space Sci. Rev., 150, 1-4, 81-124. [3] Denevi et al. (2014) J. Geophys. Res. Planets, 119, 5, 976-997. [4] Wood and Anderson (1978), LPSC IX, 3669-3689.

A miniature laser ablation mass spectrometer for quantitative in situ chemical composition investigation of lunar surface

NASA Astrophysics Data System (ADS)

Brigitte Neuland, Maike; Grimaudo, Valentine; Mezger, Klaus; Moreno-García, Pavel; Riedo, Andreas; Tulej, Marek; Wurz, Peter

2016-04-01

The chemical composition of planetary bodies, moons, comets and asteroids is a key to understand their origin and evolution [Wurz,2009]. Measurements of the elemental and isotopic composition of rocks yield information about the formation of the planetary body, its evolution and following processes shaping the planetary surface. From the elemental composition, conclusions about modal mineralogy and petrology can be drawn. Isotope ratios are a sensitive indicator for past events on the planetary body and yield information about origin and transformation of the matter, back to events that occurred in the early solar system. Finally, measurements of radiogenic isotopes make it possible to carry out dating analyses. All these topics, particularly in situ dating analyses, quantitative elemental and highly accurate isotopic composition measurements, are top priority scientific questions for future lunar missions. An instrument for precise measurements of chemical composition will be a key element in scientific payloads of future landers or rovers on lunar surface. We present a miniature laser ablation mass spectrometer (LMS) designed for in situ research in planetary and space science and optimised for measurements of the chemical composition of rocks and soils on a planetary surface. By means of measurements of standard reference materials we demonstrate that LMS is a suitable instrument for in situ measurements of elemental and isotopic composition with high precision and accuracy. Measurements of soil standards are used to confirm known sensitivity coefficients of the instrument and to prove the power of LMS for quantitative elemental analyses [Neuland,2016]. For demonstration of the capability of LMS to measure the chemical composition of extraterrestrial material we use a sample of Allende meteorite [Neuland,2014]. Investigations of layered samples confirm the high spatial resolution in vertical direction of LMS [Grimaudo,2015], which allows in situ studying of past surface processes on a planetary surface. Analyses of Pb isotopes show that the statistical uncertainty for the age determination by LMS is about ±100 Myrs, if abundance of 206Pb and 207Pb is 20ppm and 2ppm respectively [Riedo,2013]. These Pb isotopes have abundances of tens to hundreds of ppm in lunar KREEP [Nemchin,2008]. We demonstrate the measurement capabilities of LMS for petrographic and mineralogical analyses, for isotopic studies and dating analyses, which are key topics for future missions to the Moon. Having the LMS instrument installed on a lunar rover would allow measuring the chemical composition of many rock and soil samples, distributed over a certain area, inside the South Pole Aitken Basin for example. LMS measurements would yield valuable conclusions about age and mineralogy. References: [Wurz,2009]Wurz,P. et al. 2009, AIP Conf.Proc., CP1144:70-75. [Grimaudo,2015]Grimaudo, V. et al. 2015, Anal.Chem. 87: 2037-2041. [Neuland,2014]Neuland, M.B. et al. 2014, Planet.Space Sci.101:196-209. [Neuland,2016]Neuland M.B. et al. 2016, Meas. Sci. Technol.,submitted. [Riedo,2013]Riedo A. et al., 2013 Planet. Space Sci. 87: 1-13. [Nemchin,2008]Nemchin et al., 2008 Geochim. Cosmochim.Acta 72:668-689.

Finite-Difference Time-Domain Modeling of Infrasonic Waves Generated by Supersonic Auroral Arcs

NASA Astrophysics Data System (ADS)

Pasko, V. P.

2010-12-01

Atmospheric infrasonic waves are acoustic waves with frequencies ranging from ˜0.02 to ˜10 Hz [e.g., Blanc, Ann. Geophys., 3, 673, 1985]. The importance of infrasound studies has been emphasized in the past ten years from the Comprehensive Nuclear-Test-Ban Treaty verification perspective [e.g., Le Pichon et al., JGR, 114, D08112, 2009]. A proper understanding of infrasound propagation in the atmosphere is required for identification and classification of different infrasonic waves and their sources [Drob et al., JGR, 108, D21, 4680, 2003]. In the present work we employ a FDTD model of infrasound propagation in a realistic atmosphere to provide quantitative interpretation of infrasonic waves produced by auroral arcs moving with supersonic speed. We have recently applied similar modeling approaches for studies of infrasonic waves generated from thunderstorms [e.g., Few, Handbook of Atmospheric Electrodynamics, H. Volland (ed.), Vol. 2, pp.1-31, CRC Press, 1995], quantitative interpretation of infrasonic signatures from pulsating auroras [Wilson et al., GRL, 32, L14810, 2005], and studies of infrasonic waves generated by transient luminous events in the middle atmosphere termed sprites [e.g., Farges, Lightning: Principles, Instruments and Applications, H.D. Betz et al. (eds.), Ch.18, Springer, 2009]. The related results have been reported in [Pasko, JGR, 114, D08205, 2009], [de Larquier et al., GRL, 37, L06804, 2010], and [de Larquier, MS Thesis, Penn State, Aug. 2010], respectively. In the FDTD model, the altitude and frequency dependent attenuation coefficients provided by Sutherland and Bass [J. Acoust. Soc. Am., 115, 1012, 2004] are included in classical equations of acoustics in a gravitationally stratified atmosphere using a decomposition technique recently proposed by de Groot-Hedlin [J. Acoust. Soc. Am., 124, 1430, 2008]. The auroral infrasonic waves (AIW) in the frequency range 0.1-0.01 Hz associated with the supersonic motion of auroral arcs have been extensively studied for over four decades [e.g., Wilson and Nichparenko, Nature, 214, 1299, 1967; Wilson, JGR, 74, 1813,1969; JGR, 77, 1820, 1972; JATP, 37, 973, 1975; Inframatics, (10), 1, 2005]. The Lorentz force and Joule heating are discussed in the existing literature as primary sources producing infrasound waves associated with auroral electrojet [Chimonas and Hines, Planet. Space Sci., 18, 565, 1970; Chimonas and Peltier, Planet. Space Sci., 18, 599, 1970; Wilson, 1972; Swift, JGR, 78, 8305, 1973; Wilson et al., Planet. Space Sci., 24, 1155, 1976; Chimonas, JATP, 39, 799, 1977; Brekke, JATP, 41, 475, 1979]. We emphasize that up to now no quantitative multi-dimensional modeling of infrasound generation and propagation in a realistic atmosphere in association with supersonic auroras has been conducted. Results indicate, in particular, that a body force ˜10-8 N/m3 acting in the electrojet volume with cross-sectional area 10 km by 10 km is fully sufficient to produce the observed pressure perturbations on the ground ˜0.2 Pa (2 dynes/cm2) [Wilson, 1969]. We will report quantitative modeling of complex infrasonic waveforms including direct shock and reflected shockwaves, which are refracted back to the earth by the thermosphere [Wilson, 1969].

How Old is Cone Crater at the Apollo 14 Landing Site?

NASA Astrophysics Data System (ADS)

Hiesinger, Harald; Simon, Ina; van der Bogert, Carolyn H.; Robinson, Mark S.; Plescia, Jeff B.

2015-04-01

The Lunar Reconnaissance Orbiter (LRO) Narrow Angle Cameras (NAC) provides new opportunities to investigate crater size-frequency distributions (CSFDs) on individual geological units at key lunar impact craters. We performed new CSFD measurements for the Copernican-aged Cone crater at the Apollo 14 landing site because it is an anchor point for the lunar cratering chronology at young ages [1-4]. Cone crater (340 m diameter) is located about 1100 m NE of the Apollo 14 landing site on a 90 m high ridge of the Fra Mauro Formation, and exhibits a sharp rim [e.g., 5,6,7]. Samples from Cone crater were collected from four stations (Dg, C1, C2, C') during the Apollo 14 mission [7]. Exposure ages of those samples were used to date the formation of Cone crater. Although there is a considerable range of exposure ages (~12 Ma [8] to ~661 Ma [9]), several studies of Cone crater samples indicate an age of ~25-26 Ma [e.g., 2,10,11]. On the basis of our CSFD measurements we determined an absolute model age (AMA) for Cone crater of ~39 Ma, which is in the range of model ages derived by previous CSFD measurements that vary between ~24 Ma [12] and ~73 Ma [13]. However, we found a wide spread of model ages ranging from ~16 to ~82 Ma for individual areas on the crater ejecta blanket. Like [13], we find that the CSFD measurements on LROC images yield older AMAs than previous CSFDs [e.g., 12]. However, our results are closer to the older CSFDs than to those of [13] and are just within the error bars of [14]. Our derived N(1) = 3.26 x 10-5 km-2 is almost identical to the N(1) = 3.36 x 10-5 km-2 of [15]. Comparing the CSFD results to exposure ages of the returned samples we find somewhat older ages. However, at least two of our count areas produce AMAs that are within the error bars of the exposure ages [e.g., 10]. Six other areas show ages that are within two standard deviations to the exposure ages [e.g., 10]. For two count areas that were directly sampled, we obtained ages that are 10 and 23 Ma older than the exposure ages [e.g., 10]. We find that CSFD measurements performed on the ejecta blanket of Cone crater yield AMAs that agree well with the exposure ages, considering the relatively small count areas and the hummocky nature of the ejecta blanket. However, the AMAs are generally older than the exposure ages, which may be due to the small count area sizes [16], a possibly higher recent impact rate [17], some unidentified secondary craters [13], poor calibration of the production function, or inaccurate exposure ages. [1] Hiesinger et al. (2012) J. Geophys. Res. 117. [2] Stöffler and Ryder (2001) Chronology and Evolution of Mars. [3] Neukum (1983) Habil. thesis, U. of Munich. [4] Neukum et al. (2001) Space Sci. Rev. 96. [5] Swann et al. (1971) Apollo 14 Prelim. Sci. Rep. [6] Carlson (1978) NASA STI/Recon Technical Report. [7] Swann (1977) Washington US Govt. Print. Off. [8] Bhandari et al. (1972) Proc. Lunar Planet. Sci. Conf. 3. [9] Crozaz et al. (1972) Proc. Lunar Planet. Sci. Conf. 3. [10] Arvidson et al. (1975) Moon 13. [11] Stadermann et al. (1991) Geochim. Cosmochim. Acta 55. [12] Moore et al. (1980) Moon and Planets 23. [13] Plescia and Robinson (2011) LPSC 42. [14] Williams et al. (2014) Icarus 235. [15] Robbins (2014) Earth Planet. Sci. Lett. 403. [16] van der Bogert et al. (2015) LPSC 46. [17] McEwen et al. (2015) LPSC 46.

Evaluation of observation-driven evaporation algorithms: results of the WACMOS-ET project

NASA Astrophysics Data System (ADS)

Miralles, Diego G.; Jimenez, Carlos; Ershadi, Ali; McCabe, Matthew F.; Michel, Dominik; Hirschi, Martin; Seneviratne, Sonia I.; Jung, Martin; Wood, Eric F.; (Bob) Su, Z.; Timmermans, Joris; Chen, Xuelong; Fisher, Joshua B.; Mu, Quiaozen; Fernandez, Diego

2015-04-01

Terrestrial evaporation (ET) links the continental water, energy and carbon cycles. Understanding the magnitude and variability of ET at the global scale is an essential step towards reducing uncertainties in our projections of climatic conditions and water availability for the future. However, the requirement of global observational data of ET can neither be satisfied with our sparse global in-situ networks, nor with the existing satellite sensors (which cannot measure evaporation directly from space). This situation has led to the recent rise of several algorithms dedicated to deriving ET fields from satellite data indirectly, based on the combination of ET-drivers that can be observed from space (e.g. radiation, temperature, phenological variability, water content, etc.). These algorithms can either be based on physics (e.g. Priestley and Taylor or Penman-Monteith approaches) or be purely statistical (e.g., machine learning). However, and despite the efforts from different initiatives like GEWEX LandFlux (Jimenez et al., 2011; Mueller et al., 2013), the uncertainties inherent in the resulting global ET datasets remain largely unexplored, partly due to a lack of inter-product consistency in forcing data. In response to this need, the ESA WACMOS-ET project started in 2012 with the main objectives of (a) developing a Reference Input Data Set to derive and validate ET estimates, and (b) performing a cross-comparison, error characterization and validation exercise of a group of selected ET algorithms driven by this Reference Input Data Set and by in-situ forcing data. The algorithms tested are SEBS (Su et al., 2002), the Penman- Monteith approach from MODIS (Mu et al., 2011), the Priestley and Taylor JPL model (Fisher et al., 2008), the MPI-MTE model (Jung et al., 2010) and GLEAM (Miralles et al., 2011). In this presentation we will show the first results from the ESA WACMOS-ET project. The performance of the different algorithms at multiple spatial and temporal scales for the 2005-2007 reference period will be disclosed. The skill of these algorithms to close the water balance over the continents will be assessed by comparisons to runoff data. The consistency in forcing data will allow to (a) evaluate the skill of these five algorithms in producing ET over particular ecosystems, (b) facilitate the attribution of the observed differences to either algorithms or driving data, and (c) set up a solid scientific basis for the development of global long-term benchmark ET products. Project progress can be followed on our website http://wacmoset.estellus.eu. REFERENCES Fisher, J. B., Tu, K.P., and Baldocchi, D.D. Global estimates of the land-atmosphere water flux based on monthly AVHRR and ISLSCP-II data, validated at 16 FLUXNET sites. Remote Sens. Environ. 112, 901-919, 2008. Jiménez, C. et al. Global intercomparison of 12 land surface heat flux estimates. J. Geophys. Res. 116, D02102, 2011. Jung, M. et al. Recent decline in the global land evapotranspiration trend due to limited moisture supply. Nature 467, 951-954, 2010. Miralles, D.G. et al. Global land-surface evaporation estimated from satellite-based observations. Hydrol. Earth Syst. Sci. 15, 453-469, 2011. Mu, Q., Zhao, M. & Running, S.W. Improvements to a MODIS global terrestrial evapotranspiration algorithm. Remote Sens. Environ. 115, 1781-1800, 2011. Mueller, B. et al. Benchmark products for land evapotranspiration: LandFlux-EVAL multi- dataset synthesis. Hydrol. Earth Syst. Sci. 17, 3707-3720, 2013. Su, Z. The Surface Energy Balance System (SEBS) for estimation of turbulent heat fluxes. Hydrol. Earth Syst. Sci. 6, 85-99, 2002.

PlanetServer/EarthServer: Big Data analytics in Planetary Science

NASA Astrophysics Data System (ADS)

Pio Rossi, Angelo; Oosthoek, Jelmer; Baumann, Peter; Beccati, Alan; Cantini, Federico; Misev, Dimitar; Orosei, Roberto; Flahaut, Jessica; Campalani, Piero; Unnithan, Vikram

2014-05-01

Planetary data are freely available on PDS/PSA archives and alike (e.g. Heather et al., 2013). Their exploitation by the community is somewhat limited by the variable availability of calibrated/higher level datasets. An additional complexity of these multi-experiment, multi-mission datasets is related to the heterogeneity of data themselves, rather than their volume. Orbital - so far - data are best suited for an inclusion in array databases (Baumann et al., 1994). Most lander- or rover-based remote sensing experiment (and possibly, in-situ as well) are suitable for similar approaches, although the complexity of coordinate reference systems (CRS) is higher in the latter case. PlanetServer, the Planetary Service of the EC FP7 e-infrastructure project EarthServer (http://earthserver.eu) is a state-of-art online data exploration and analysis system based on the Open Geospatial Consortium (OGC) standards for Mars orbital data. It provides access to topographic, panchromatic, multispectral and hyperspectral calibrated data. While its core focus has been on hyperspectral data analysis through the OGC Web Coverage Processing Service (Oosthoek et al., 2013; Rossi et al., 2013), the Service progressively expanded to host also sounding radar data (Cantini et al., this volume). Additionally, both single swath and mosaicked imagery and topographic data are being added to the Service, deriving from the HRSC experiment (e.g. Jaumann et al., 2007; Gwinner et al., 2009) The current Mars-centric focus can be extended to other planetary bodies and most components are general purpose ones, making possible its application to the Moon, Mercury or alike. The Planetary Service of EarthServer is accessible on http://www.planetserver.eu References: Baumann, P. (1994) VLDB J. 4 (3), 401-444, Special Issue on Spatial Database Systems. Cantini, F. et al. (2014) Geophys. Res. Abs., Vol. 16, #EGU2014-3784, this volume Heather, D., et al.(2013) EuroPlanet Sci. Congr. #EPSC2013-626 Gwinner, K., et al., Earth Planet. Sci. Lett., 294, 506-519, doi:10.1016/j.epsl.2009.11.007. Oosthoek, J.H.P, et al. (2013) Advances in Space Research. DOI: 10.1016/j.asr.2013.07.002 Rossi, A. P., et al. (2013) XLDB Workshop Europe, CERN, Switzerland

Wind circulation regimes at Venus' cloud tops: Ground-based Doppler velocimetry using CFHT/ESPaDOnS and comparison with simultaneous cloud tracking measurements using VEx/VIRTIS in February 2011

NASA Astrophysics Data System (ADS)

Machado, Pedro; Widemann, Thomas; Luz, David; Peralta, Javier

2014-11-01

We present new results based on ground-based Doppler spectroscopic measurements, obtained with the ESPaDOnS spectrograph at Canada-France-Hawaii telescope (CFHT) and simultaneous observations of velocity fields, obtained from space by the VIRTIS-M instrument on board the Venus Express spacecraft. These measurements are based on high-resolution spectra of Fraunhofer lines in the visible to NIR range (0.37-1.05 μm) acquired on February 19-21, 2011 at a resolution of about 80,000, measuring Venus' winds at 70 km, using incoming solar radiation scattered by cloud top particles in the observer's direction (Widemann, T., et al., [2007]. Planet. Space Sci. 55, 1741-1756; Widemann, T., et al., [2008]. Planet. Space Sci. 56, 1320-1334). The zonal wind field has been characterized by latitudinal bands, at a phase angle Φ = (68.7 ± 0.3) ° , between +10°N and 60°S, by steps of 10°, and from [ ϕ -ϕE ] = - 50 ° to sub-Earth longitude ϕE = 0 ° , by steps of 12°. From space, VIRTIS-M UV (0.38 μm) imaging exposures on the dayside were acquired simultaneously in orbit 1786, providing the first simultaneous cloud-tracking measurements with Doppler velocimetry. From the ground, we measured a zonal mean background velocity of v‾z = (117.3 ± 18.0) ms-1 on February 19, and v‾z = (117.5 ± 14.5) ms-1 on February 21. We detect an unambiguous poleward meridional flow on the morning dayside hemisphere of (18.8 ± 12.3) m s-1 on February 19/21. Latitudinal variations of the zonal and meridional winds are further compared with the simultaneous VIRTIS data. We discuss temporal variability as well as its statistical significance.

A review of the liquid metal diffusion data obtained from the space shuttle endeavour mission STS-47 and the space shuttle columbia mission STS-52

NASA Astrophysics Data System (ADS)

Shirkhanzadeh, Morteza

Accurate data of liquid-phase solute diffusion coefficients are required to validate the condensed -matter physics theories. However, the required data accuracy to discriminate between com-peting theoretical models is 1 to 2 percent(1). Smith and Scott (2) have recently used the measured values of diffusion coefficients for Pb-Au in microgravity to validate the theoretical values of the diffusion coefficients derived from molecular dynamics simulations and several Enskog hard sphere models. The microgravity data used was obtained from the liquid diffusion experiments conducted on board the Space Shuttle Endeavour (mission STS-47) and the Space Shuttle Columbia (mission STS-52). Based on the analysis of the results, it was claimed that the measured values of diffusion coefficients were consistent with the theoretical results and that the data fit a linear relationship with a slope slightly greater than predicted by the molecular dynamics simulations. These conclusions, however, contradict the claims made in previous publications (3-5) where it was reported that the microgravity data obtained from the shuttle experiments fit the fluctuation theory (D proportional to T2). A thorough analysis of data will be presented to demonstrate that the widely-reported micro-gravity results obtained from shuttle experiments are not reliable and sufficiantly accurate to discriminate between competing theoretical models. References: 1. J.P. Garandet, G. Mathiak, V. Botton, P. Lehmann and A. Griesche, Int. J. Thermophysics, 25, 249 (2004). 2.P.J. Scott and R.W. Smith, J. Appl. Physics 104, 043706 (2008). 3. R.W. Smith, Microgravity Sci. Technol. XI (2) 78-84 (1998). 4.Smith et al, Ann. N.Y. Acad. Sci. 974:56-67 (2002) (retracted). 5.R.A. Herring et al, J. Jpn. Soc. Microgravity Appl., Vol.16, 234-244 (1999).

Public Data Set: Erratum: "Multi-point, high-speed passive ion velocity distribution diagnostic on the Pegasus Toroidal Experiment" [Rev. Sci. Instrum. 83, 10D516 (2012)

DOE Data Explorer

Burke, Marcus G. [University of Wisconsin-Madison] (ORCID:0000000176193724); Fonck, Raymond J. [University of Wisconsin-Madison] (ORCID:0000000294386762); Bongard, Michael W. [University of Wisconsin-Madison] (ORCID:0000000231609746); Schlossberg, David J. [University of Wisconsin-Madison] (ORCID:0000000287139448); Winz, Gregory R. [University of Wisconsin-Madison] (ORCID:0000000177627184)

2016-07-18

This data set contains openly-documented, machine readable digital research data corresponding to figures published in M.G. Burke et al., 'Erratum: "Multi-point, high-speed passive ion velocity distribution diagnostic on the Pegasus Toroidal Experiment" [Rev. Sci. Instrum. 83, 10D516 (2012)],' Rev. Sci. Instrum. 87, 079902 (2016).

Simulating the Atmospheric Impact of Criegee Intermediates: Implementation of new understanding in atmospheric chemical mechanisms

NASA Astrophysics Data System (ADS)

Bloss, William; Newland, Mike; Rickard, Andrew; Vereecken, Luc; Evans, Mathew; Munoz, Amalia; Rodenas, Mila

2016-04-01

Unsaturated hydrocarbons - alkenes - account for about 90% of global VOC. Stabilized Criegee Intermediates (SCI) are thought to be formed in the atmosphere mainly from reactions of unsaturated hydrocarbons with ozone. SCI have been shown in laboratory and chamber experiments to rapidly oxidise SO2 and NO2, providing a potentially important gas phase oxidation route for these species in the atmosphere. They have also been implicated in the formation of aerosol and organic acids. However, the importance of SCI reactions with traces gases is critically dependent on the relative ratio of the rate constants for the reactions of the SCI with these and other trace gases, with H2O, and for unimolecular decomposition, which vary between SCIs, and between geometric isomers. The selection of reactions and rate constants is critically important in determining the calculated impact of SCI processes upon atmospheric composition and chemistry. Since the recent resurgence in interest in this chemistry, a number of model studies have been performed, with SCI mechanisms of varying comprehensiveness and accuracy, as the understanding of the community has evolved from new laboratory, theoretical and chamber studies, and field observations. Here we present an assessment of the dependence of modelled SCI abundance, behaviour and impacts upon the Criegee mechanism adopted, in the context of (a) the accepted status quo prior to the laboratory and field studies of Welz et al. and Mauldin et al., (b) changes to the SCI mechanism reflecting new kinetics for key bimolecular reactions, e.g. with SO2 and NO2; (c) emerging understanding of the interactions of SCI with water vapour and their unimolecular decomposition and (d) reactions with other atmospheric trace gases. The modelled SCI behaviour is compared with the results from recent chamber studies, and the resulting calculated SCI abundance and impacts evaluated for urban and forested atmospheric boundary layer scenarios.

On stochastic differential equations with arbitrarily slow convergence rates for strong approximation in two space dimensions.

PubMed

Gerencsér, Máté; Jentzen, Arnulf; Salimova, Diyora

2017-11-01

In a recent article (Jentzen et al. 2016 Commun. Math. Sci. 14 , 1477-1500 (doi:10.4310/CMS.2016.v14.n6.a1)), it has been established that, for every arbitrarily slow convergence speed and every natural number d ∈{4,5,…}, there exist d -dimensional stochastic differential equations with infinitely often differentiable and globally bounded coefficients such that no approximation method based on finitely many observations of the driving Brownian motion can converge in absolute mean to the solution faster than the given speed of convergence. In this paper, we strengthen the above result by proving that this slow convergence phenomenon also arises in two ( d =2) and three ( d =3) space dimensions.

The Oxygen Isotopic Composition of the Sun

NASA Astrophysics Data System (ADS)

McKeegan, K. D.; Kallio, A.; Heber, V. S.; Jarzebinski, G.; Mao, P.; Coath, C.; Kunihiro, T.; Wiens, R. C.; Judith, A.; Burnett, D. S.

2010-12-01

An accurate and precise determination of the oxygen isotopic composition of the Sun is the highest priority scientific goal of the Genesis Mission [1] as such data would provide a baseline from which one could interpret the oxygen isotopic anomalies found at all spatial scales in inner solar system materials. We have measured oxygen isotope compositions of implanted solar wind in 40 spots along a radial traverse of the Genesis SiC target sample 60001 by depth profiling with the UCLA MegaSIMS [2]. Mass-dependent fractionation induced by the solar wind concentrator [3] ion optics was corrected by comparison of the concentrator 22Ne/20Ne with that measured in a bulk solar wind target (diamond-like carbon on Si, [4]). The solar wind captured at L1 has an isotopic composition of (δ18O, δ17O) ≈ (-99, -79)‰, a value which is far removed from the terrestrial mass fractionation line. Profiles from the central portion of the target, where solar concentrations are highest and background corrections minimal, yield a mean Δ17O = -28.3 ± 1.8 ‰ indicating that the Earth and other planetary materials from the inner solar system are highly depleted in 16O relative to the solar wind. A mass-dependent fractionation of ~ -20%/amu in the acceleration of solar wind is required if we hypothesize that the photospheric oxygen isotope value, which represents the bulk starting composition of the solar system, is on the 16O-mixing line characteristic of refractory phase in primitive meteorites [5]. With this assumption, our preferred value for the bulk solar oxygen isotope composition is δ18O ≈ δ17O ≈ -57‰. A mechanism is required to fractionate oxygen isotopes in a non-mass-dependent manner to deplete 16O by ~6 to 7% in the rocky materials of the solar nebula. As oxygen is the third most abundant element in the solar system, and the most abundant in the terrestrial planets, this mechanism must operate on a large scale. Isotope-selective photochemistry, for example as in self-shielding of CO, operating in the solar nebula [6,7] or its precursor cloud [8] is a leading candidate; other models involving molecular symmetry-dependent reactions are also viable [9,10]. References: [1] D. Burnett et al. (2003) Space Sci. Rev. 105, 509. [2] K. McKeegan et al. (2008) LPSC XXIX, #2020. [3] R.Wiens et al. (2003) Space Sci. Rev. 105, 601. [4] V. Heber et al. Space Sci. Rev. 130, 309. [5] R. Clayton and T. Mayeda (1978) EPSL 40, 168. [6] R. Clayton (2002) Nature 415, 860. [7] J. Lyons and E. Young (2005) Nature 434, 317. [8] H. Yurimoto and K. Kuramoto (2004) Science 305, 1763. [9] M. Thiemens (1999) Science 283, 341. [10] R. Marcus (2004) J. Chem. Phys. 121, 8201.

Spectral modeling of Ceres VIR data from Dawn: Method and Result

NASA Astrophysics Data System (ADS)

Raponi, Andrea; De Sanctis, M. C.; Ciarniello, M.; Carrozzo, F. G.; Ammannito, E.; Capaccioni, F.; Capria, M. T.; Frigeri, A.; Fonte, S.; Giardino, M.; Longobardo, A.; Magni, G.; Marchi, S.; Palomba, E.; Pieters, C. M.; Tosi, F.; Turrini, D.; Zambon, F.; Raymond, C. A.; Russell, C. T.

2015-11-01

The Dawn spacecraft [1] is at Ceres, the closest of the IAU-defined dwarf planets to the Sun. This work focuses on the interpretation of Ceres’ surface composition based on the data from the VIR instrument [2] onboard Dawn. The Visible InfraRed (VIR) mapping spectrometer combines high spectral and spatial resolution in the VIS (0.25-1mm) and IR (1-5mm) spectral ranges. VIR will provide a very good coverage of the surface during its orbital mission at Ceres.In order to model the measured spectra, we have utilized Hapke's radiative transfer model [3], which allows estimation of the mineral composition, the relative abundances of the spectral end-members, and the grain size. Optical constants of the spectral end-members are approximated by applying the methodology described in [4] to IR spectra reflectance obtained from the RELAB database.The observed spectra of Ceres surface are affected by a thermal emission component that prevents direct comparison with laboratory data at longer wavelengths. Thus to model the whole wavelength range measured by VIR, the thermal emission is modeled together with the reflectance. Calibrated spectra are first cleaned by removing artefacts. A best fit is obtained with a least square optimization algorithm. For further details on the method, see reference [5].The range 2.5 - 2.9 μm is severely hindered by Earth's atmosphere, but it contains a strong absorption band that dominates the IR Ceres’ spectrum. Thanks to the VIR instrument we can obtain a compositional model for the whole IR range [6]. We used several different combinations of materials hypothesized to be representative of the Ceres’ surface including phyllosilicates, ices, carbonaceous chondrites and salts. The results will be discussed.Acknowledgements This work is supported by the Italian Space Agencies and NASA. Enabling contributions from the Dawn Instrument, Operations, and Science Teams are gratefully acknowledged.Reference[1] Russell et al., Space Sci. Rev., 163, 3-23, 2011.[2] De Sanctis et al., Space Sci. Rev., 163, 329-369, 2011.[3] Hapke, Cambridge Univ. Press., 1993, 2012.[4] Carli et al., Icarus, 235, 207-219, 2014.[5] Raponi, PhD Thesis, arXiv:1503.08172, 2015.[6] De Sanctis et al., Nature submitted 2015.

A Global Scale Scenario for Prebiotic Chemistry: Silica-Based Self-Assembled Mineral Structures and Formamide.

PubMed

Saladino, Raffaele; Botta, Giorgia; Bizzarri, Bruno Mattia; Di Mauro, Ernesto; Garcia Ruiz, Juan Manuel

2016-05-17

The pathway from simple abiotically made organic compounds to the molecular bricks of life, as we know it, is unknown. The most efficient geological abiotic route to organic compounds results from the aqueous dissolution of olivine, a reaction known as serpentinization (Sleep, N.H., et al. (2004) Proc. Natl. Acad. Sci. USA 101, 12818-12822). In addition to molecular hydrogen and a reducing environment, serpentinization reactions lead to high-pH alkaline brines that can become easily enriched in silica. Under these chemical conditions, the formation of self-assembled nanocrystalline mineral composites, namely silica/carbonate biomorphs and metal silicate hydrate (MSH) tubular membranes (silica gardens), is unavoidable (Kellermeier, M., et al. In Methods in Enzymology, Research Methods in Biomineralization Science (De Yoreo, J., Ed.) Vol. 532, pp 225-256, Academic Press, Burlington, MA). The osmotically driven membranous structures have remarkable catalytic properties that could be operating in the reducing organic-rich chemical pot in which they form. Among one-carbon compounds, formamide (NH2CHO) has been shown to trigger the formation of complex prebiotic molecules under mineral-driven catalytic conditions (Saladino, R., et al. (2001) Biorganic & Medicinal Chemistry, 9, 1249-1253), proton irradiation (Saladino, R., et al. (2015) Proc. Natl. Acad. Sci. USA, 112, 2746-2755), and laser-induced dielectric breakdown (Ferus, M., et al. (2015) Proc Natl Acad Sci USA, 112, 657-662). Here, we show that MSH membranes are catalysts for the condensation of NH2CHO, yielding prebiotically relevant compounds, including carboxylic acids, amino acids, and nucleobases. Membranes formed by the reaction of alkaline (pH 12) sodium silicate solutions with MgSO4 and Fe2(SO4)3·9H2O show the highest efficiency, while reactions with CuCl2·2H2O, ZnCl2, FeCl2·4H2O, and MnCl2·4H2O showed lower reactivities. The collections of compounds forming inside and outside the tubular membrane are clearly specific, demonstrating that the mineral self-assembled membranes at the same time create space compartmentalization and selective catalysis of the synthesis of relevant compounds. Rather than requiring odd local conditions, the prebiotic organic chemistry scenario for the origin of life appears to be common at a universal scale and, most probably, earlier than ever thought for our planet.

New mapping of Radlandi basin and detailed analysis of its inner plains

NASA Astrophysics Data System (ADS)

Minelli, Francesco; Giorgetti, Carolina; Mondini, Alessandro; Pauselli, Cristina; Mancinelli, Paolo

2013-04-01

NEW MAPPING OF RADITLADI BASIN AND DETAILED ANALYSIS OF ITS INNER PLAINS. Francesco Minelli 1, Carolina Giorgetti 1, Alessandro C. Mondini 2, Cristina Pauselli 1, Paolo Mancinelli1. 1 Gruppo di Geologia Strutturale e Geofisica (GSG), Dipartimento di Scienze della Terra, Università degli Studi di Perugia, 06123, Perugia, Italy . Email: minelli91@yahoo.it. 2 CNR IRPI Perugia, 06123, Perugia. Introduction: The Raditladi basin is a large peak-ring impact crater discovered during the MESSENGER (MErcury Surface, Space ENvironment, GEochemistry, and Ranging) first flyby of Mercury in January 2008 [1]. The Raditladi basin is relatively young [2], and the study of the internal structures give an indication of the processes that acted recently in Mercury's geological history. Geological mapping: We first present the geological mapping of Raditladi crater. In the map we defined different sub-units on the base of previous studies [4][5] and surface morphology and reflectance. Through a GIS software we associated a polygonal layer to each sub-unit, this allowed to distinguish nine different layers. Due to the similarities with the Rachmaninoff basin, to define sub-units mapped on Raditladi, we adopted Rachmaninoff crater's units definitions made by Marchi et al. (2011) [4]. Structures analysis : We also mapped secondary structures consisting in concentric troughs arranged in a circular pattern. We defined two different kinds of troughs: (i) structures characterized by a distinct flat floor and interpretable as grabens, and (ii) structures with linear and curvilinear segments [5]. Inner plain deposit: The analysis of the topography made possible the estimation of the deposit's thickness. The measurement of the thickness is possible thanks to the presence of two small craters, crater A and crater, located in Raditladi's Inner plain. Observing the morphology of the two small craters' rim and hummocky central floor, we distinguished two different units: the shallower consists in thin material [6] and the deeper consists in shocked surface. To estimate the deposit thickness, we realized two sections across the two craters, we considered the rim uplift due to the stratigraphic doubling [7], and the depth at which we observed the shocked surface situated below the surficial deposit. Moreover the two craters, one near the center and the other near the peak ring, allowed us to observe the variation of the deposit's thickness: tracing a section that cuts both the craters is possible to appreciate its thinning towards the basin center. On the base of impact crater experiment made by Takita & Sumita (2011) [6] we supposed that the deposit consist in a thin upper layer of material with a fine granulometry. The deposit thickness measured in the crater B, near the peak ring, is 839 m and in the crater A, near the basin center, is 846 m. In conclusion, the obtained values, differing only for 7 m, show an approximately constant thickness of the deposit from the basin center, where the values is slightly greater, to the peak ring. References: [1] Solomon S.C. et al. (2008) Science, 321, 59-62.[2] Strom R.G. et al. (2008) Science, 321, 79. [3] Hawkins S.E. et al. (2007) Space Sci. Rev., 131, 247-338[4] Marchi S. et al. (2011) Planet. Space Sci, 59, 1968-1980. [5] Prockter L.M. et al. (2009) Lunar Planet. Sci. Conf. Abstract, 40, 1758. [6] Takita H. & Sumita I. (2011) Japan Geoscience Union Meeting 2011, PPS020-P05. [7] H.J. Melosh (1989) Oxford Monographs on Geology and Geophysics Series, 11.

The Case of the Great Space Exploration: An Educator Guide with Activities in Mathematics, Science, and Technology. The NASA SCI Files. EG-2004-09-12-LARC

ERIC Educational Resources Information Center

Ricles, Shannon; Jaramillo, Becky; Fargo, Michelle

2004-01-01

In this companion to the "NASA SCI Files" episode "The Case of the Great Space Exploration," the tree house detectives learn about NASA's new vision for exploring space. In four segments aimed at grades 3-5, students learn about a variety of aspects of space exploration. Each segment of the guide includes an overview, a set of objectives,…

The microbe capture experiment in space: Fluorescence microscopic detection of microbes captured by aerogel

NASA Astrophysics Data System (ADS)

Sugino, Tomohiro; Yokobori, Shin-Ichi; Yang, Yinjie; Kawaguchi, Yuko; Okudaira, Kyoko; Tabata, Makoto; Kawai, Hideyuki; Hasegawa, Sunao; Yamagishi, Akihiko

Microbes have been collected at the altitude up to about 70 km in the sampling experiment done by several groups[1]. We have also collected high altitude microbes, by using an airplane and balloons[2][3][4][5]. We collected new deinococcal strain (Deinococcus aetherius and Deinococ-cus aerius) and several strains of spore-forming bacilli from stratosphere[2][4][5]. However, microbe sampling in space has never been reported. On the other hand, "Panspermia" hy-pothesis, where terrestrial life is originated from outside of Earth, has been proposed[6][7][8][9]. Recent report suggesting existence of the possible microbe fossils in the meteorite of Mars origin opened the serious debate on the possibility of migration of life embedded in meteorites (and cosmic dusts)[10][11]. If we were able to find terrestrial microbes in space, it would suggest that the terrestrial life can travel between astronomical bodies. We proposed a mission "Tanpopo: Astrobiology Exposure and Micrometeoroid Capture Experiments" to examine possible inter-planetary migration of microbes, organic compounds and meteoroids on Japan Experimental Module of the International Space Station (ISS)[12]. Two of six sub themes in this mission are directly related to interplanetary migration of microbes. One is the direct capturing experi-ment of microbes (probably within the particles such as clay) in space by the exposed ultra-low density aerogel. Another is the exposure experiment to examine survivability of the microbes in harsh space environment. They will tell us the possibility of interplanetary migration of microbes (life) from Earth to outside of Earth (or vise versa). In this report, we will report whether aerogel that have been used for the collection of space debris and cosmic dusts can be used for microbe sampling in space. We will discuss how captured particles by aerogel can be detected with DNA-specific fluorescent dye, and how to distinguish microbes from other mate-rials (i.e. aerogel and particles such as clay). The surface of micro-particles captured by aerogel is often vitrified. The non-specific fluorescent light is often observed from vitrified materials. Therefore, we need to distinguish fluorescent light of stained microbes from that of vitrified ma-terials. We are going to use two types of differences (wavelength dependence and attenuation rate of fluorescent) between stained microbes with DNA-specific fluorescent dye and other ma-terials such as clay and aerogel. Fluorescent light of stained microbes shows attenuation faster than that of vitrified materials. Fluorescent light of vitrified materials shows broader range of emission spectra than that of stained microbes. In addition, we simulated the high-speed collision experiment of micro-particles to the aerogel with the two stage light gas gun (ca. 4 km/s). The micro-particles containing pre-stained and dried cells of Deinococcus radiodurans mixed with clay material were used for the collision experiment, and the captured particles were observed with fluorescence microscope. This experiment suggests that the captured microbes can be detected and be distinguished from clay materials. Reference [1] Yang, Y. et al. (2009) Biol. Sci. Space, 23, 151-163. [2] Yang, Y., et al. (2008) Biol. Sci. Space 22:18-25. [3] Yang, Y., et al. (2008) JAXA-RR-08-001: 34-42. [4] Yang, Y., et al. (2009) Internatl. J. Syst. Evol. Bacteriol., 59: 1862-1866. [5] Yang, Y. et al. (2010) Internatl. J. Syst. Evol. Bacteriol. (in press). [6] Arrhenius, S. (1908) Worlds in the Making-the Evolution of the Universe (translation to English by H. Borns) Harper and Brothers Publishers, New York. [7]Crick, F. (1981) Life Itself. Simon Schuster, New York. [8] W.L. Nicholson et al., Microbiol. Mol. Biol. Rev. 64 (2000) 548. [9] G. Horneck et al., Orig. Life Evol. Biosph. 31 (2001) 527. [10] Chyba, C. and C. Sagan (1992) Nature 355: 125-132. [11] Sandford, S. A., et al. (2006) Science 314: 1720-1724. [12] Yamagishi, A., et al. (2008) International Symposium on Space Technology and Science (ISTS) Web Paper Archives. 2008-k-05.

Particle trapping and beam transport issues in laser driven accelerators

NASA Astrophysics Data System (ADS)

Gwenael, Fubiani; Wim, Leemans; Eric, Esarey

2000-10-01

The LWFA and colliding pulses [1][2] sheme are capable of producing very compact electron bunches where the longitudinal size is much smaller than the transverse size. In this case, even if the electrons are relativistic, space charge force can affect the longitudinal and transverse bunch properties [3][4]. In the Self-modulated regime and the colliding pulse sheme, electrons are trapped from the background plasma and rapidly accelerated. We present theoretical studies of the generation and transport of electron bunches in LWFAs. The space charge effect induced in the bunch is modelled assuming the bunch is ellipsoid like. Beam transport in vacuum, comparison between gaussian and waterbag distribution, comparison between envelope model and PIC simulation will be discussed. This work is supported by the Director, Office of Science, Office of High Energy & Nuclear Physics, High Energy Physics Division, of the U.S Department of Energy, under Contract No. DE-AC03-76SF00098 [1]E.Esarey et al.,IEEE Trans. Plasma Sci. PS-24,252 (1996); W.P. Leemans et al, ibidem, 331. [2]D. Umstadter et al., Phys. Rev. Lett. 76, 2073 (1996); E.Esarey et al., Phys. Rev. Lett. 79, 2682 (1997); C.B Schroeder et al., Phys. Rev. E59, 6037 (1999) [3]DESY M87-161 (1987); DESY M88-013 (1988) [4] R.W. Garnett and T.P Wangler, IEEE Part. Acce. Conf. (1991)

Reply to the EFSA (2016) on the relevance of recent publications (Hofmann et al. 2014, 2016) on environmental risk assessment and management of Bt-maize events (MON810, Bt11 and 1507).

PubMed

Kruse-Plass, Maren; Hofmann, Frieder; Kuhn, Ulrike; Otto, Mathias; Schlechtriemen, Ulrich; Schröder, Boris; Vögel, Rudolf; Wosniok, Werner

2017-01-01

In this commentary, we respond to a report of the EFSA GMO Panel (EFSA EFSA Supp Publ, 1) that criticises the outcomes of two studies published in this journal (Hofmann et al. Environ Sci Eur 26: 24, 2; Environ Sci Eur 28: 14, 3). Both publications relate to the environmental risk assessment and management of Bt-maize, including maize events MON810, Bt11 and maize 1507. The results of Hofmann et al. (Environ Sci Eur 26: 24, 2), using standardised pollen mass filter deposition measurements, indicated that the EFSA Panel model had underestimated pollen deposition and, hence, exposure of non-target organisms to Bt-maize pollen. The results implied a need for safety buffer distances in the kilometre range for protected nature reserve areas instead of the 20-30 m range recommended by the EFSA Panel. As a result, the EFSA Panel revised their model (EFSA EFSA J 13: 4127, 4), adopting the slope of the empirical data from Hofmann et al. The intercept, however, was substantially reduced to less than 1% at one point by introducing further assumptions based on the estimates of mainly panel members, citing possible 'uncertainty'. Hofmann et al. (Environ Sci Eur 28: 14, 3) published extensive empirical data regarding pollen deposition on leaves. These results were part of a larger 3-year study involving detailed measurements of pollen release, dispersal and deposition over the maize flowering period. The data collected in situ confirmed the previous predictions of Hofmann et al. (Environ Sci Eur 26: 24, 2). Mean levels and observed variability of pollen deposition on maize and four lepidopteran host plants exceeded the assumptions and disagreed with the conclusions of the EFSA Panel. The EFSA Panel reacted in a report (EFSA EFSA Supp Publ, 1) criticising the methods and outcomes of the two published studies of Hofmann et al. while reaffirming their original recommendations. We respond here point-by-point, showing that the critique is not justified. Based on our results on Urtica leaf pollen density, we confirm the need for specific environmental impact assessments for Bt-maize cultivation with respect to protected habitats within isolation buffer distances in the kilometre range.

The Shock and Vibration Bulletin: Proceedings on the Symposium on ShocK and Vibration (52nd) Held in New Orleans, Louisiana on 26-28 October 1981. Part 4. Fatigue and Random Loading Control, Isolation and Damping

DTIC Science & Technology

1982-05-01

functions for every ergodic ensemble or process, but this frequency for each time-acceleration involves in principle a different kind data input, but...geometries Journal Phys. E: Sci. Instrum. 14, (solid and hollow) are different . 202-207. 5. CONCLUSION It has been shown in principle that tests with a...Center, Huntsville, AL SPACE SIIUI’LE SOLID ROCKE FIOOSTEIt WATER ENTRY CAVITY COLLAPSE LOADS I. T. Keefe and E. A. Rawls , Chrysler Corporation, Slidell

Microfluidic Experiments Studying Pore Scale Interactions of Microbes and Geochemistry

NASA Astrophysics Data System (ADS)

Chen, M.; Kocar, B. D.

2016-12-01

Understanding how physical phenomena, chemical reactions, and microbial behavior interact at the pore-scale is crucial to understanding larger scale trends in groundwater chemistry. Recent studies illustrate the utility of microfluidic devices for illuminating pore-scale physical-biogeochemical processes and their control(s) on the cycling of iron, uranium, and other important elements 1-3. These experimental systems are ideal for examining geochemical reactions mediated by microbes, which include processes governed by complex biological phenomenon (e.g. biofilm formation, etc.)4. We present results of microfluidic experiments using a model metal reducing bacteria and varying pore geometries, exploring the limitations of the microorganisms' ability to access tight pore spaces, and examining coupled biogeochemical-physical controls on the cycling of redox sensitive metals. Experimental results will provide an enhanced understanding of coupled physical-biogeochemical processes transpiring at the pore-scale, and will constrain and compliment continuum models used to predict and describe the subsurface cycling of redox-sensitive elements5. 1. Vrionis, H. A. et al. Microbiological and geochemical heterogeneity in an in situ uranium bioremediation field site. Appl. Environ. Microbiol. 71, 6308-6318 (2005). 2. Pearce, C. I. et al. Pore-scale characterization of biogeochemical controls on iron and uranium speciation under flow conditions. Environ. Sci. Technol. 46, 7992-8000 (2012). 3. Zhang, C., Liu, C. & Shi, Z. Micromodel investigation of transport effect on the kinetics of reductive dissolution of hematite. Environ. Sci. Technol. 47, 4131-4139 (2013). 4. Ginn, T. R. et al. Processes in microbial transport in the natural subsurface. Adv. Water Resour. 25, 1017-1042 (2002). 5. Scheibe, T. D. et al. Coupling a genome-scale metabolic model with a reactive transport model to describe in situ uranium bioremediation. Microb. Biotechnol. 2, 274-286 (2009).

Cosmic dust flux on Earth inferred from the Concordia micrometeorite collection

NASA Astrophysics Data System (ADS)

Engrand, Cécile; Duprat, Jean; Dartois, Emmanuel; Godard, Marie; Delauche, Lucie

2017-04-01

The present extraterrestrial flux incoming to Earth is dominated by cosmic dust, i.e. micrometeorites in the 20-500 microns size range. Prior to atmospheric entry, the flux is estimated to ˜30 000 tons.yr-1 [1]. The proportion of this flux reaching the earth surface as dust particles is debated [e.g. 2]. Since 2000, we recover micrometeorites from ultraclean snow in the vicinity of the Dome C Concordia station in Antarctica. This region has a well-characterized and small precipitation rate (˜ 3.5 g of water per year) that allows collecting micrometeorites from large equivalent surfaces (> 100 m2.yrs) by sampling reasonable volumes of snow. The high efficiency and cleanliness of the collecting process at Dome C has enabled the recovery of several thousands of particles larger than ˜ 20 μm, constituting the Concordia micrometeorite collection [3]. The Concordia micrometeorites have a young terrestrial age of about 50 years. We characterized more than three thousand micrometeorites (both melted and unmelted particles) by secondary electron microscopy and classified them in the textural types defined in [4]. A preliminary flux value of 6,000 tons.yr-1 was given in [5] from the early Concordia collection examination. We now have better statistics to update this value. References: [1] Love S.G. and Brownlee D.E. (1993) Science 262, 550-553. [2] Peucker-Ehrenbrink B., et al. (2016) Elements 12, 191-196. [3] Duprat J., et al. (2007) Adv. Space Res. 39, 605-611. [4] Genge M.J., et al. (2008) Meteorit. Planet. Sci. 43, 497-515. [5] Duprat J., et al. (2006) Meteorit. Planet. Sci. 41 Suppl., A48 (#5239).

Distribution of phyllosilicates on Ceres

NASA Astrophysics Data System (ADS)

Ammannito, Eleonora; De Sanctis, Maria Cristina; Ciarniello, Mauro; Frigeri, Alessandro; Giacomo Carrozzo, Filippo; Combe, Jean Philippe; Ehlmann, Bethany; Marchi, Simone; McSween, Hap Y.; Raponi, Andrea; Castillo-Rogez, Julie C.; Toplis, Michael J.; Tosi, Federico; Longobardo, Andrea; Palomba, Ernesto; Pieters, Carle M.; Raymond, Carol A.; Schenk, Paul; Zambon, Francesca; Russell, Christopher T.

2016-04-01

Studies of the dwarf planet Ceres using ground-based and orbiting telescopes proposed a variety of possible surficial composition including water in clay minerals [1], ammoniated phyllosilicates [2], or a mixture of brucite, Mg2CO3 and iron-rich serpentine [3, 4]. But the lack of spectral data in the 2.5 to 2.9 μm interval has precluded definitive identifications. The Dawn spacecraft has been acquiring spectra of the surface of Ceres since January 2015 [5, 6, 7]. The average thermally corrected reflectance spectrum of Ceres shows that the 2.6-4.2μm region is characterized by a broad asymmetric feature, characteristic of H2O/OH bearing materials, with several distinct narrower absorption bands [8]. This spectrum is compatible with the presence on the surface of a mixture of ammoniated-phyllosilicates, Mg-phyllosilicates, carbonates, and dark materials [8]. A strong 2.7-μm absorption dominates the overall spectral properties, and it has been attributed to OH-stretching vibrations in phyllosilicates [9] while the weaker 3.05 μm absorption has been attributed to the presence of NH4+ in phyllosilicates [10]. The spectral parameters of the absorption features at 2.7 and 3.05 μm have been computed to study their position and intensity. The computed spectral position of both absorption features is remarkably homogeneous. The average values are 2.727±0.005 and 3.061±0.005 μm respectively. Since the position of both features is sensitive to the chemical composition of the phyllosilicates, we conclude that the composition of phyllosilicates does not significantly change across the mapped portion of Ceres' surface. The computed values are indicative of Mg-OH phases, like antigorite (Mg-serpentine) or saponite (Mg-smectite) [9]. The presence of Mg-, rather than Fe-serpentine on Ceres may be interpreted as an indication that alteration had been extensive, while the lack of geochemical variation indicates that this is true throughout the exposed upper layer with no significant compositional gradients. The computed spectral intensity of both absorption features shows some variability. For the 2.7 absorption, the average value is 0.251±0.006, while the range of variability is between 0.20 and 0.29. For the 3.05 absorption, the average value is 0.055±0.012, while the range of variability is between 0.03 and 0.09. Interestingly, the distributions of the intensities of the two bands broadly match. Among several possibilities, the most likely explanation for the variability in intensity is a changing abundance of phyllosilicates within the assemblage forming the surface of Ceres. In conclusion, while the chemical composition of the phyllosilicates is remarkably constant, their abundance is variable. The compositional homogeneity characterized by the pervasive presence of Mg- and NH4-bearing phyllosilicates indicates endogenous formation by a globally widespread and extensive alteration processes while the variations in the amount of phyllosilicate suggest the existence of a vertically stratified upper crust. References: [1] Lebofsky, L. et al. (1981) Icarus, 48, 453-459. [2] King T. et al. (1992) Science, 255, 1551-1553. [3] Rivkin A.S. et al. (2006) Icarus, 185, 563-567. [4] Milliken R.E. and Rivkin A.S. (2009) Nature Geosci., 2, 258-261. [5] Russell C.T. and Raymond C.A. (2011) Space Sci. Rev., 163, 3-23. [6] Russell C.T. et al. (2015) EPSC. [7] De Sanctis M.C. et al. (2011) Space Sci. Rev., 163, 329-369. [8] De Sanctis M.C. et al. (2015) Nature. [9] Bishop J.L. et al. (2008) ClayMiner., 43, 35-54. [10] Bishop J.L. et al. (2002) Planet. Space Sci., 50.

Recent Experimental Advances to Determine (noble) Gases in Waters

NASA Astrophysics Data System (ADS)

Kipfer, R.; Brennwald, M. S.; Huxol, S.; Mächler, L.; Maden, C.; Vogel, N.; Tomonaga, Y.

2013-12-01

In aquatic systems noble gases, radon, and bio-geochemically conservative transient trace gases (SF6, CFCs) are frequently applied to determine water residence times and to reconstruct past environmental and climatic conditions. Recent experimental breakthroughs now enable ● to apply the well-established concepts of terrestrial noble gas geochemistry in waters to the minute water amounts stored in sediment pore space and in fluid inclusions (A), ● to determine gas exchange processes on the bio-geochemical relevant time scales of minutes - hours (B), and ● to separate diffusive and advective gas transport in soil air (C). A. Noble-gas analysis in water samples (< 1 g) facilitates determining the solute transport in the pore space and identifying the origin of bio- and geogenic fluids in (un) consolidated sediments [1]. Advanced techniques that combine crushing and sieving speleothem samples in ultra-high-vacuum to a specific grain size allow to separate air and water-bearing fluid inclusions and thus enables noble-gas-based reconstruction of environmental conditions from water masses as small as 1mg [2]. B. The coupling of noble gas analysis with approaches of gas chromatography permits combined analysis of noble gases and other gases species (e.g., SF6, CFCs, O2, N2) from a single water sample. The new method substantially improves ground water dating by SF6 and CFCs as excess air is quantified from the same sample and hence can adequately be corrected for [3]. Portable membrane-inlet mass spectrometers enable the quasi-continuous and real-time analysis of noble gases and other dissolved gases directly in the field, allowing, for instance, quantification of O2 turnover rates on small time scales [4]. C. New technical developments perfect 222Rn analysis in water by the synchronous the determination of the short-lived 220Rn. The combined 220,222Rn analysis sheds light on the emanation behaviour of radon by identifying soil water content to be the crucial control of 220Rn occurrence in the environment, e.g., making an argument why 220Rn is not detectable in water, but in soil air. As 220Rn occurrence is of 'very local origin' the combined analysis of 220,222Rn in soil air allows differentiating between advective and diffusive soil gas transport [5]. By discussing these recent achievements, we intend to stimulate a broader discussion to identify future applications of noble and other gases in (un) conventional aquatic systems, such as blood. [1] Tomonaga et al. (2011) Limnol. Oceanogr. Methods, 9, 42-49, doi:10:4319/lom.2011.9.42. [2] Vogel et al. (2013) Geochem. Geophys. Geosyst., 14, doi:10.1002/ggge.20164. [3] Brennwald et al. (2013) Environ. Sci. Technol., Article ASAP, DOI: 10.1021/es401698p. [4] Mächler et al. (2012) Environ. Sci. Technol., 47, 7060-7066. [5] Huxol et al. Environ. Sci. Technol., in revision.

Eventos de Desconexão no Cometa P/Halley sob a Ótica do Modelo de Reconexão Magnética

NASA Astrophysics Data System (ADS)

Voelzke, M. R.; Matsuura, O. T.

1998-08-01

531 imagens contidas no The International Halley Watch Atlas of Large-Scale Phenomena (Brandt et al., 1992) cobrindo o período de setembro de 1985 a julho de 1986 foram analisadas visando identificar, caracterizar as propriedades e correlacionar estruturas morfológicas da cauda de plasma do cometa P/Halley. A análise revelou 47 eventos de desconexão (DEs) (Niedner & Brandt, 1979; Jockers, 1985; Celnik et al., 1988; Delva et al., 1991). A análise completa de todas as imagens encontra-se publicada em Voelzke & Matsuura, 1998. A distribuição dos DEs na distância heliocêntrica apresenta um caráter bimodal possivelmente associado com a distribuição espacial das fronteiras de setor magnético do meio interplanetário. Os 47 DEs fotografados em 47 imagens distintas permitiram determinar 19 origens de DEs, ou seja, o instante em que supostamente o cometa cruzou a fronteira entre setores magnéticos do vento solar. Tais dados cometários foram comparados com dados do vento solar provenientes de medidas realizadas in situ pelas sondas IMP-8, ICE e PVO, que mediram a variação da velocidade do vento solar, da densidade e da pressão dinâmica durante o intervalo analisado. Os dados destas sondas espaciais em conjunto com os da sonda Vega 1 foram usados para determinar o tempo das passagens do lençol de corrente. Com base nos dados das sondas foram calculadas as coordenadas heliográficas retroativas do lençol de corrente na "superfície fonte" dos mapas sinóticos do campo magnético de Hoeksema, 1989. O cálculo retroativo é feito através de um modelo simples de expressão do vento solar com velocidade uniforme, sendo considerada a co-rotação da magnetosfera com o Sol. Este trabalho apresenta os resultados desta comparação e a análise cinemática da origem dos DEs, determinada sob a hipótese que o plasma desconectado de um dado DE afasta-se com velocidade constante do núcleo cometário (Voelzke & Matsuura, 1998) e compara esta análise com outras que determinam o tempo de desconexão a partir de um movimento linear constantemente acelerado (Yi et al., 1994). A velocidade de um DE para outro varia enormemente. - Brandt, J.C., Niedner, M.B.Jr. and Rahe, J., (1992) The International Halley Watch Atlas of Large-Scale Phenomena (printed by: Johnson Printing Co., Boulder, CO), University of Colorado-Boulder. - Celnik, W.E., Koczet, P., Schlosser, W., Schulz, R., Svejda, P. and Weissbauer, K., (1988) Astron. Astrophys. Suppl. Ser. 72, 89. - Delva, M., Schwingenschuh, K., Niedner, M.B.Jr. and Gringauz, K.I., (1991) Planet. Space Sci. 39, Number 5, 697. - Hoeksema, J.T., (1989) Adv. Space Res. 9, 141. - Jockers, K., (1985) Astron. Astrophys. Suppl. Ser. 62, 791. - Niedner, M.B.Jr. and Brandt, J.C., (1979) Astrophys. J. 234, 723. - Voelzke, M.R. and Matsuura, O.T., (1988) Planet. Space Sci. 46, 835. - Yi, Y., Caputo, M.F. and Brandt, J.C., (1994) Planet. Space Sci. 42, Number 9, 705.

Micromorphic approach for gradient-extended thermo-elastic-plastic solids in the logarithmic strain space

NASA Astrophysics Data System (ADS)

Aldakheel, Fadi

2017-11-01

The coupled thermo-mechanical strain gradient plasticity theory that accounts for microstructure-based size effects is outlined within this work. It extends the recent work of Miehe et al. (Comput Methods Appl Mech Eng 268:704-734, 2014) to account for thermal effects at finite strains. From the computational viewpoint, the finite element design of the coupled problem is not straightforward and requires additional strategies due to the difficulties near the elastic-plastic boundaries. To simplify the finite element formulation, we extend it toward the micromorphic approach to gradient thermo-plasticity model in the logarithmic strain space. The key point is the introduction of dual local-global field variables via a penalty method, where only the global fields are restricted by boundary conditions. Hence, the problem of restricting the gradient variable to the plastic domain is relaxed, which makes the formulation very attractive for finite element implementation as discussed in Forest (J Eng Mech 135:117-131, 2009) and Miehe et al. (Philos Trans R Soc A Math Phys Eng Sci 374:20150170, 2016).

Research Stanchion and Transporter for Small Ruminants

DTIC Science & Technology

1988-03-30

L, Plumlee V P, Hobbs C S, at al. The Design and Operation of Metabolism Units for Nutritional Studies With Swine. J Anin Sci 1951; 10:88-98. 12...Restraint for Yucatan Miniature Swine. Lab Anim Sci 1983; 33(1):95-97. i . I ൖ ----------. A . APPEM4IX I UATEITLS LIST I. Stainless Steel Tubing: a

Face-Centred Cubic Iron: Ab Initio Calculations of Sound Velocities in the Lunar Core

NASA Astrophysics Data System (ADS)

Wood, M. C.; Wood, I. G.; Vočadlo, L.

2017-12-01

Studies, such as the reanalysis of the Apollo lunar seismograms [1], have shown that the Moon has undergone differentiation and possesses a small core. The composition of the lunar core is not well constrained, and many compositional models have been suggested including combinations of iron, nickel, and light elements such as sulphur and carbon [e.g. 1, 2, 3, 4], and other more exotic compositions [5]. Additional constraints are crucial to our understanding of the Moon, including its formation, the dynamics of its interior, and a lunar dynamo. We use ab initio molecular dynamics simulations to calculate elastic constants of face-centred cubic (fcc) iron and iron alloys and hence sound velocities at lunar core conditions, at 5-6 GPa and 1,300-1,900 K [3]. The results from these simulations will then be compared with the data from the Apollo seismograms and experimental data to help form a description of the lunar interior. [1] Weber et al. (2011) Science 331, 309-312. [2] Dasgupta et al. (2009) Geochim. Cosmochim. Acta 73, 6678-6692. [3] Antonangeli et al. (2015) Proc. Natl. Acad. Sci. U.S.A. 112, 3916-3919. [4] Righter et al. (2017) Earth Planet. Sci. Lett. 463, 323-332. [5] Wieczorek & Zuber (2002) Lunar Planet. Sci. 33, abstract 1384.

A Global Scale Scenario for Prebiotic Chemistry: Silica-Based Self-Assembled Mineral Structures and Formamide

PubMed Central

2016-01-01

The pathway from simple abiotically made organic compounds to the molecular bricks of life, as we know it, is unknown. The most efficient geological abiotic route to organic compounds results from the aqueous dissolution of olivine, a reaction known as serpentinization (Sleep, N.H., et al. (2004) Proc. Natl. Acad. Sci. USA 101, 12818–12822). In addition to molecular hydrogen and a reducing environment, serpentinization reactions lead to high-pH alkaline brines that can become easily enriched in silica. Under these chemical conditions, the formation of self-assembled nanocrystalline mineral composites, namely silica/carbonate biomorphs and metal silicate hydrate (MSH) tubular membranes (silica gardens), is unavoidable (Kellermeier, M., et al. In Methods in Enzymology, Research Methods in Biomineralization Science (De Yoreo, J., Ed.) Vol. 532, pp 225–256, Academic Press, Burlington, MA). The osmotically driven membranous structures have remarkable catalytic properties that could be operating in the reducing organic-rich chemical pot in which they form. Among one-carbon compounds, formamide (NH2CHO) has been shown to trigger the formation of complex prebiotic molecules under mineral-driven catalytic conditions (Saladino, R., et al. (2001) Biorganic & Medicinal Chemistry, 9, 1249–1253), proton irradiation (Saladino, R., et al. (2015) Proc. Natl. Acad. Sci. USA, 112, 2746–2755), and laser-induced dielectric breakdown (Ferus, M., et al. (2015) Proc Natl Acad Sci USA, 112, 657–662). Here, we show that MSH membranes are catalysts for the condensation of NH2CHO, yielding prebiotically relevant compounds, including carboxylic acids, amino acids, and nucleobases. Membranes formed by the reaction of alkaline (pH 12) sodium silicate solutions with MgSO4 and Fe2(SO4)3·9H2O show the highest efficiency, while reactions with CuCl2·2H2O, ZnCl2, FeCl2·4H2O, and MnCl2·4H2O showed lower reactivities. The collections of compounds forming inside and outside the tubular membrane are clearly specific, demonstrating that the mineral self-assembled membranes at the same time create space compartmentalization and selective catalysis of the synthesis of relevant compounds. Rather than requiring odd local conditions, the prebiotic organic chemistry scenario for the origin of life appears to be common at a universal scale and, most probably, earlier than ever thought for our planet. PMID:27115539

Interrelationships of Prenatal and Postnatal Growth, Hormones, Diet, and Breast Cancer

DTIC Science & Technology

2006-03-01

Breslow NE, Day NE. Statistical methods in cancer research, vol. 1. The analysis of case-control studies, IARC Sci. Publ. 32, Lyon, IARC, 1980 . 9...weight (Ekbom et al, 1992; Innes et al, 2000; Michels et al, 1996; Sander- son et al, 1996). Conversely, high adolescent (Coates et al, 1999; Hislop et...Brinton and Swanson, 1992; Choi et al, 1978; Coates et al, 1999; Franceschi et al, 1996; Hislop et al, 1986; Le Marchand et al, 1988a; Pryor et al, 1989

An analytical study of physical models with inherited temporal and spatial memory

NASA Astrophysics Data System (ADS)

Jaradat, Imad; Alquran, Marwan; Al-Khaled, Kamel

2018-04-01

Du et al. (Sci. Reb. 3, 3431 (2013)) demonstrated that the fractional derivative order can be physically interpreted as a memory index by fitting the test data of memory phenomena. The aim of this work is to study analytically the joint effect of the memory index on time and space coordinates simultaneously. For this purpose, we introduce a novel bivariate fractional power series expansion that is accompanied by twofold fractional derivatives ordering α, β\\in(0,1]. Further, some convergence criteria concerning our expansion are presented and an analog of the well-known bivariate Taylor's formula in the sense of mixed fractional derivatives is obtained. Finally, in order to show the functionality and efficiency of this expansion, we employ the corresponding Taylor's series method to obtain closed-form solutions of various physical models with inherited time and space memory.

SciDB and Geoinformatics Analysis

NASA Astrophysics Data System (ADS)

Brown, Paul

2015-04-01

The SciDB project took as its design goals a list of features identified as being critical to scientific data management in a survey of working scientists (Stonebraker et al 2009). Earth scientists working with remote sensing data were well represented among those polled so it should come as no surprise that the platform has been embraced by that community. In this talk we focus on work done by researchers at NASA and INPE, and on applications created by commercial data providers in Korea and the United States. For each use-case, we will review the project team's objectives, the nature and quantity of the data involved, the their workload queries. As we discuss each use-case we will describe what is emerging as "best practice" for data management and analysis in this space. M. Stonebraker, J. Becla, D. J. DeWitt, K. T. Lim, D. Maier, O. Ratzesberger, and S. B. Zdonik. Requirements for science data bases and scidb. In CIDR 2009, Fourth Biennial Conference on Innovative Data Systems Research, Asilomar, CA, USA, January 4-7, 2009, Online Proceedings, 2009.

Selective Vulnerability of Cortical Border Zone to Microembolic Infarct.

PubMed

Bergui, Mauro; Castagno, Davide; D'Agata, Federico; Cicerale, Alessandro; Anselmino, Matteo; Maria Ferrio, Federica; Giustetto, Carla; Halimi, Franck; Scaglione, Marco; Gaita, Fiorenzo

2015-07-01

Endovascular procedures, including atrial fibrillation transcatheter ablation, may cause microembolization of brain arteries. Microemboli often cause small sized and clinically silent cerebral ischemias (SCI). These lesions are clearly visible on early postoperative magnetic resonance diffusion-weighted images. We analyzed SCI distribution in a population of patients submitted to atrial fibrillation transcatheter ablation. Seventy-eight of 927 consecutive patients submitted to atrial fibrillation transcatheter ablation were found positive for acute SCI on a postoperative magnetic resonance. SCI were identified and marked, and their coordinates were transformed from native space into the International Consortium for Brain Mapping/Montreal Neurological Institute space. We then computed the voxel-wise probability distribution map of the SCI using the activation likelihood estimation approach. SCI were more commonly found in the cortex. In supratentorial regions, SCI selectively involved cortical border zone between anterior, middle, and posterior cerebral arteries; in infratentorial regions, distal territory of posteroinferior cerebellar artery. Possible explanations include selective embolization, linked to the vascular anatomy of pial arteries supplying those territories, reduced clearance of emboli in a relatively hypoperfused zone, or a combination of both. This particular distribution of lesions has been reported in both animal models and in patients with microemboli of different sources. A selective vulnerability of cortical border zone to microemboli occurring during atrial fibrillation transcatheter ablation was observed. We hypothesize that such selectivity may apply to microemboli of different sources. © 2015 American Heart Association, Inc.

Amphibolite of the Xinghuadukou group from the Xinlin-Xiguitu belt, NE China: new evidence for the NE branch of the Paleo-Asian Ocean

NASA Astrophysics Data System (ADS)

Hou, Wenzhu

2017-04-01

The tectonic evolution of the Paleo-Asian Ocean (PAO) witnessed the cycling of two supercontinents, Rodinia and Pangea, in Earth's geological history. This long-lasting paleo-ocean was initiated by the breakup of the supercontinent Rodinia during the Early Neoproterozoic (1,2) and terminated by the final collage of the supercontinent Pangea from Central to Eastern (current coordinates) Asia, likely lasting to the Late Permian or Early Triassic (3,4). Numerous continental and island arcs, seamounts, mid-ocean ridges and micro-blocks were amalgamated responding to the subduction and consumption of the oceanic crust of the PAO, to form the most complex and long-living Phanerozoic accretionary orogenic belt, the Central Asian Orogenic Belt (CAOB) (5,6). Trapped by the collision and amalgamation of the eastern segment of CAOB, several rock suites of oceanic affinity were reported along the Xinlin-Xiguitu belt that connects the Erguna block to the northwest and the Xing'an block to the southeast in NE China, including the Toudaoqiao blueschist (7), Jifeng ophiolite (although the forming environment remains debatable, see 8 and 9), and Xinlin ophiolite (10,11). All these suites have been proposed to be the relics of the NE branch of the PAO. However, along the northeastern extension of this belt, outcropped the Xinghuadukou group that was previously thought Paleoproterozoic in age yet has been reconsidered to be Cambrian (12), the relationship of which and this belt remains unclear. In this study, a suite of amphibolite was collected from the Xinghuadukou group outcropped in the easternmost Xinlin-Xiguitu belt in NE China and conducted geochemical analysis to discuss their forming environment and tectonic implications. Samples display low SiO2 (45%-49%wt), low K2O (0.55%-1.07%wt) compositions, low in A/CNK, but high in A/NK and FeOt/MgO ratios. REE compositions are relative low (ΣREE=52-122ppm) showing a flat chondrite normative pattern with slight enrichment in LREE ((La/Ya)N=1.5-2.4) and no Eu anomaly (Eu/Eu*=0.9-1.0). The LILE fractionation is indistinctive ((Sr/Y)N=1.1-1.8). Samples show an evident E-MORB affinity. Along with the previous studies, it can be concluded: 1) the protolith of the amphibolite of the Xinghuadukou group is a suite of tholeiitic basalt that formed in the oceanic islands environment; 2) with all the oceanic suites reported in Xinlin-Xiguitu belt, a branch of the Eastern PAO can be well defined, which likely existed from the Late Neoproterozoic to Late Cambrian, so called the Xinlin-Xiguitu Ocean. Acknowledgements: This study was financially supported by the National Natural Science Foundation of China (Projects 41190075, 41190070, 41230207, 41390441), the Hong Kong Research Grants Council General Research Fund (HKU7063/13P and 17301915), and the HKU Seed Funding Programme for Basic Research (201311159126). References: 1. N. L. Dobretsov et al., Gondwana Res. 6(2), 143-159 (2003). 2. J. Tang et al., Precambrian Res. 224, 597-611 (2013). 3. J. Y. Li, J. Asian Earth Sci. 26(3), 207-224 (2006). 4. P. R. Eizenhöfer et al., Tectonics 33(4), 441-463 (2014). 5. B. F. Windley et al., J. Geol. Soc. 164(1), 31-47 (2007). 6. W. Xiao et al., Annu. Rev. Earth Planet. Sci. 43, 477-507 (2015). 7. J. B. Zhou et al., J. Asian Earth Sci. 97, 197-210 (2015). 8. Z. Feng et al., Int. J. Earth Sci. 105(2), 491-505 (2016). 9. D. H. Ni, Int. J. Earth Sci. (2016). doi:10.1007/s00531-016-1412-2 10. R. S. Li, Heilongjiang Geology, 2(1), 21-32 (1991). 11. W. Yan et al., Earth Sci. - J. Chin. Uni. Geo. 8 (2014). 12. L. Miao et al., Chin. Sci. Bull. 52(8), 1112-1124 (2007).

Climate Consensus and "Misinformation": A Rejoinder to "Agnotology, Scientific Consensus, and the Teaching and Learning of Climate Change"

ERIC Educational Resources Information Center

Legates, David R.; Soon, Willie; Briggs, William M.; Monckton of Brenchley, Christopher

2015-01-01

Agnotology is the study of how ignorance arises via circulation of misinformation calculated to mislead. Legates et al. ("Sci Educ" 22:2007-2017, 2013) had questioned the applicability of agnotology to politically-charged debates. In their reply, Bedford and Cook ("Sci Educ" 22:2019-2030, 2013), seeking to apply agnotology to…

Electron Cyclotron Resonance (ECR) Ion Source Development at the Holified Radioactive Ion Beam Facility

NASA Astrophysics Data System (ADS)

Bilheux, Hassina; Liu, Yuan; Alton, Gerald; Cole, John; Williams, Cecil; Reed, Charles

2004-11-01

Performance of ECR ion sources can be significantly enhanced by increasing the physical size of their ECR zones in relation to the size of their plasma volumes (spatial and frequency domain methods).^3-5 A 6 GHz, all-permanent magnet ECR ion source with a large resonant plasma volume has been tested at ORNL.^6 The magnetic circuit can be configured for creating both flat-β (volume) and conventional minimum-β (surface) resonance conditions. Direct comparisons of the performance of the two source types can be made under similar operating conditions. In this paper, we clearly demonstrate that the flat-β source outperforms its minimum-β counterpart in terms of charge state distribution and intensity within a particular charge state. ^1bilheuxhn@ornl.gov ^2Managed by UT-Battelle, LLC, for the U.S. Department of Energy under contract DE-AC05-00OR22725. ^3G.D. Alton, D.N. Smithe, Rev. Sci. Instrum. 65 (1994) 775. ^4G.D. Alton et al., Rev. Sci. Instrum. 69 (1998) 2305. ^5Z.Q. Xie, C.M. Lyneis, Rev. Sci. Instrum. 66 (1995) 4218. ^6Y. Liu et al., Rev. Sci. Instrum. 69 (1998) 1311.

Measurement of Coherent π^{+} Production in Low Energy Neutrino-Carbon Scattering.

PubMed

Abe, K; Andreopoulos, C; Antonova, M; Aoki, S; Ariga, A; Assylbekov, S; Autiero, D; Ban, S; Barbi, M; Barker, G J; Barr, G; Bartet-Friburg, P; Batkiewicz, M; Bay, F; Berardi, V; Berkman, S; Bhadra, S; Blondel, A; Bolognesi, S; Bordoni, S; Boyd, S B; Brailsford, D; Bravar, A; Bronner, C; Buizza Avanzini, M; Calland, R G; Campbell, T; Cao, S; Caravaca Rodríguez, J; Cartwright, S L; Castillo, R; Catanesi, M G; Cervera, A; Cherdack, D; Chikuma, N; Christodoulou, G; Clifton, A; Coleman, J; Collazuol, G; Coplowe, D; Cremonesi, L; Dabrowska, A; De Rosa, G; Dealtry, T; Denner, P F; Dennis, S R; Densham, C; Dewhurst, D; Di Lodovico, F; Di Luise, S; Dolan, S; Drapier, O; Duffy, K E; Dumarchez, J; Dytman, S; Dziewiecki, M; Emery-Schrenk, S; Ereditato, A; Feusels, T; Finch, A J; Fiorentini, G A; Friend, M; Fujii, Y; Fukuda, D; Fukuda, Y; Furmanski, A P; Galymov, V; Garcia, A; Giffin, S G; Giganti, C; Gizzarelli, F; Gonin, M; Grant, N; Hadley, D R; Haegel, L; Haigh, M D; Hamilton, P; Hansen, D; Harada, J; Hara, T; Hartz, M; Hasegawa, T; Hastings, N C; Hayashino, T; Hayato, Y; Helmer, R L; Hierholzer, M; Hillairet, A; Himmel, A; Hiraki, T; Hirota, S; Hogan, M; Holeczek, J; Horikawa, S; Hosomi, F; Huang, K; Ichikawa, A K; Ieki, K; Ikeda, M; Imber, J; Insler, J; Intonti, R A; Irvine, T J; Ishida, T; Ishii, T; Iwai, E; Iwamoto, K; Izmaylov, A; Jacob, A; Jamieson, B; Jiang, M; Johnson, S; Jo, J H; Jonsson, P; Jung, C K; Kabirnezhad, M; Kaboth, A C; Kajita, T; Kakuno, H; Kameda, J; Karlen, D; Karpikov, I; Katori, T; Kearns, E; Khabibullin, M; Khotjantsev, A; Kielczewska, D; Kikawa, T; Kim, H; Kim, J; King, S; Kisiel, J; Knight, A; Knox, A; Kobayashi, T; Koch, L; Koga, T; Konaka, A; Kondo, K; Kopylov, A; Kormos, L L; Korzenev, A; Koshio, Y; Kropp, W; Kudenko, Y; Kurjata, R; Kutter, T; Lagoda, J; Lamont, I; Larkin, E; Lasorak, P; Laveder, M; Lawe, M; Lazos, M; Lindner, T; Liptak, Z J; Litchfield, R P; Li, X; Longhin, A; Lopez, J P; Ludovici, L; Lu, X; Magaletti, L; Mahn, K; Malek, M; Manly, S; Marino, A D; Marteau, J; Martin, J F; Martins, P; Martynenko, S; Maruyama, T; Matveev, V; Mavrokoridis, K; Ma, W Y; Mazzucato, E; McCarthy, M; McCauley, N; McFarland, K S; McGrew, C; Mefodiev, A; Metelko, C; Mezzetto, M; Mijakowski, P; Minamino, A; Mineev, O; Mine, S; Missert, A; Miura, M; Moriyama, S; Mueller, Th A; Murphy, S; Myslik, J; Nakadaira, T; Nakahata, M; Nakamura, K G; Nakamura, K; Nakamura, K D; Nakayama, S; Nakaya, T; Nakayoshi, K; Nantais, C; Nielsen, C; Nirkko, M; Nishikawa, K; Nishimura, Y; Novella, P; Nowak, J; O'Keeffe, H M; Ohta, R; Okumura, K; Okusawa, T; Oryszczak, W; Oser, S M; Ovsyannikova, T; Owen, R A; Oyama, Y; Palladino, V; Palomino, J L; Paolone, V; Patel, N D; Pavin, M; Payne, D; Perkin, J D; Petrov, Y; Pickard, L; Pickering, L; Pinzon Guerra, E S; Pistillo, C; Popov, B; Posiadala-Zezula, M; Poutissou, J-M; Poutissou, R; Przewlocki, P; Quilain, B; Radermacher, T; Radicioni, E; Ratoff, P N; Ravonel, M; Rayner, M A M; Redij, A; Reinherz-Aronis, E; Riccio, C; Rojas, P; Rondio, E; Roth, S; Rubbia, A; Rychter, A; Sacco, R; Sakashita, K; Sánchez, F; Sato, F; Scantamburlo, E; Scholberg, K; Schoppmann, S; Schwehr, J; Scott, M; Seiya, Y; Sekiguchi, T; Sekiya, H; Sgalaberna, D; Shah, R; Shaikhiev, A; Shaker, F; Shaw, D; Shiozawa, M; Shirahige, T; Short, S; Smy, M; Sobczyk, J T; Sobel, H; Sorel, M; Southwell, L; Stamoulis, P; Steinmann, J; Stewart, T; Stowell, P; Suda, Y; Suvorov, S; Suzuki, A; Suzuki, K; Suzuki, S Y; Suzuki, Y; Tacik, R; Tada, M; Takahashi, S; Takeda, A; Takeuchi, Y; Tanaka, H K; Tanaka, H A; Terhorst, D; Terri, R; Thakore, T; Thompson, L F; Tobayama, S; Toki, W; Tomura, T; Touramanis, C; Tsukamoto, T; Tzanov, M; Uchida, Y; Vacheret, A; Vagins, M; Vallari, Z; Vasseur, G; Wachala, T; Wakamatsu, K; Walter, C W; Wark, D; Warzycha, W; Wascko, M O; Weber, A; Wendell, R; Wilkes, R J; Wilking, M J; Wilkinson, C; Wilson, J R; Wilson, R J; Yamada, Y; Yamamoto, K; Yamamoto, M; Yanagisawa, C; Yano, T; Yen, S; Yershov, N; Yokoyama, M; Yoo, J; Yoshida, K; Yuan, T; Yu, M; Zalewska, A; Zalipska, J; Zambelli, L; Zaremba, K; Ziembicki, M; Zimmerman, E D; Zito, M; Żmuda, J

2016-11-04

We report the first measurement of the flux-averaged cross section for charged current coherent π^{+} production on carbon for neutrino energies less than 1.5 GeV, and with a restriction on the final state phase space volume in the T2K near detector, ND280. Comparisons are made with predictions from the Rein-Sehgal coherent production model and the model by Alvarez-Ruso et al., the latter representing the first implementation of an instance of the new class of microscopic coherent models in a neutrino interaction Monte Carlo event generator. We observe a clear event excess above background, disagreeing with the null results reported by K2K and SciBooNE in a similar neutrino energy region. The measured flux-averaged cross sections are below those predicted by both the Rein-Sehgal and Alvarez-Ruso et al.

Evaluation of parameters of Black Hole, stellar cluster and dark matter distribution from bright star orbits in the Galactic Center

NASA Astrophysics Data System (ADS)

Zakharov, Alexander

It is well-known that one can evaluate black hole (BH) parameters (including spin) analyz-ing trajectories of stars around BH. A bulk distribution of matter (dark matter (DM)+stellar cluster) inside stellar orbits modifies trajectories of stars, namely, generally there is a apoas-tron shift in direction which opposite to GR one, even now one could put constraints on DM distribution and BH parameters and constraints will more stringent in the future. Therefore, an analyze of bright star trajectories provides a relativistic test in a weak gravitational field approximation, but in the future one can test a strong gravitational field near the BH at the Galactic Center with the same technique due to a rapid progress in observational facilities. References A. Zakharov et al., Phys. Rev. D76, 062001 (2007). A.F. Zakharov et al., Space Sci. Rev. 148, 301313(2009).

Measurement of Coherent π+ Production in Low Energy Neutrino-Carbon Scattering

NASA Astrophysics Data System (ADS)

Abe, K.; Andreopoulos, C.; Antonova, M.; Aoki, S.; Ariga, A.; Assylbekov, S.; Autiero, D.; Ban, S.; Barbi, M.; Barker, G. J.; Barr, G.; Bartet-Friburg, P.; Batkiewicz, M.; Bay, F.; Berardi, V.; Berkman, S.; Bhadra, S.; Blondel, A.; Bolognesi, S.; Bordoni, S.; Boyd, S. B.; Brailsford, D.; Bravar, A.; Bronner, C.; Buizza Avanzini, M.; Calland, R. G.; Campbell, T.; Cao, S.; Caravaca Rodríguez, J.; Cartwright, S. L.; Castillo, R.; Catanesi, M. G.; Cervera, A.; Cherdack, D.; Chikuma, N.; Christodoulou, G.; Clifton, A.; Coleman, J.; Collazuol, G.; Coplowe, D.; Cremonesi, L.; Dabrowska, A.; De Rosa, G.; Dealtry, T.; Denner, P. F.; Dennis, S. R.; Densham, C.; Dewhurst, D.; Di Lodovico, F.; Di Luise, S.; Dolan, S.; Drapier, O.; Duffy, K. E.; Dumarchez, J.; Dytman, S.; Dziewiecki, M.; Emery-Schrenk, S.; Ereditato, A.; Feusels, T.; Finch, A. J.; Fiorentini, G. A.; Friend, M.; Fujii, Y.; Fukuda, D.; Fukuda, Y.; Furmanski, A. P.; Galymov, V.; Garcia, A.; Giffin, S. G.; Giganti, C.; Gizzarelli, F.; Gonin, M.; Grant, N.; Hadley, D. R.; Haegel, L.; Haigh, M. D.; Hamilton, P.; Hansen, D.; Harada, J.; Hara, T.; Hartz, M.; Hasegawa, T.; Hastings, N. C.; Hayashino, T.; Hayato, Y.; Helmer, R. L.; Hierholzer, M.; Hillairet, A.; Himmel, A.; Hiraki, T.; Hirota, S.; Hogan, M.; Holeczek, J.; Horikawa, S.; Hosomi, F.; Huang, K.; Ichikawa, A. K.; Ieki, K.; Ikeda, M.; Imber, J.; Insler, J.; Intonti, R. A.; Irvine, T. J.; Ishida, T.; Ishii, T.; Iwai, E.; Iwamoto, K.; Izmaylov, A.; Jacob, A.; Jamieson, B.; Jiang, M.; Johnson, S.; Jo, J. H.; Jonsson, P.; Jung, C. K.; Kabirnezhad, M.; Kaboth, A. C.; Kajita, T.; Kakuno, H.; Kameda, J.; Karlen, D.; Karpikov, I.; Katori, T.; Kearns, E.; Khabibullin, M.; Khotjantsev, A.; Kielczewska, D.; Kikawa, T.; Kim, H.; Kim, J.; King, S.; Kisiel, J.; Knight, A.; Knox, A.; Kobayashi, T.; Koch, L.; Koga, T.; Konaka, A.; Kondo, K.; Kopylov, A.; Kormos, L. L.; Korzenev, A.; Koshio, Y.; Kropp, W.; Kudenko, Y.; Kurjata, R.; Kutter, T.; Lagoda, J.; Lamont, I.; Larkin, E.; Lasorak, P.; Laveder, M.; Lawe, M.; Lazos, M.; Lindner, T.; Liptak, Z. J.; Litchfield, R. P.; Li, X.; Longhin, A.; Lopez, J. P.; Ludovici, L.; Lu, X.; Magaletti, L.; Mahn, K.; Malek, M.; Manly, S.; Marino, A. D.; Marteau, J.; Martin, J. F.; Martins, P.; Martynenko, S.; Maruyama, T.; Matveev, V.; Mavrokoridis, K.; Ma, W. Y.; Mazzucato, E.; McCarthy, M.; McCauley, N.; McFarland, K. S.; McGrew, C.; Mefodiev, A.; Metelko, C.; Mezzetto, M.; Mijakowski, P.; Minamino, A.; Mineev, O.; Mine, S.; Missert, A.; Miura, M.; Moriyama, S.; Mueller, Th. A.; Murphy, S.; Myslik, J.; Nakadaira, T.; Nakahata, M.; Nakamura, K. G.; Nakamura, K.; Nakamura, K. D.; Nakayama, S.; Nakaya, T.; Nakayoshi, K.; Nantais, C.; Nielsen, C.; Nirkko, M.; Nishikawa, K.; Nishimura, Y.; Novella, P.; Nowak, J.; O'Keeffe, H. M.; Ohta, R.; Okumura, K.; Okusawa, T.; Oryszczak, W.; Oser, S. M.; Ovsyannikova, T.; Owen, R. A.; Oyama, Y.; Palladino, V.; Palomino, J. L.; Paolone, V.; Patel, N. D.; Pavin, M.; Payne, D.; Perkin, J. D.; Petrov, Y.; Pickard, L.; Pickering, L.; Pinzon Guerra, E. S.; Pistillo, C.; Popov, B.; Posiadala-Zezula, M.; Poutissou, J.-M.; Poutissou, R.; Przewlocki, P.; Quilain, B.; Radermacher, T.; Radicioni, E.; Ratoff, P. N.; Ravonel, M.; Rayner, M. A. M.; Redij, A.; Reinherz-Aronis, E.; Riccio, C.; Rojas, P.; Rondio, E.; Roth, S.; Rubbia, A.; Rychter, A.; Sacco, R.; Sakashita, K.; Sánchez, F.; Sato, F.; Scantamburlo, E.; Scholberg, K.; Schoppmann, S.; Schwehr, J.; Scott, M.; Seiya, Y.; Sekiguchi, T.; Sekiya, H.; Sgalaberna, D.; Shah, R.; Shaikhiev, A.; Shaker, F.; Shaw, D.; Shiozawa, M.; Shirahige, T.; Short, S.; Smy, M.; Sobczyk, J. T.; Sobel, H.; Sorel, M.; Southwell, L.; Stamoulis, P.; Steinmann, J.; Stewart, T.; Stowell, P.; Suda, Y.; Suvorov, S.; Suzuki, A.; Suzuki, K.; Suzuki, S. Y.; Suzuki, Y.; Tacik, R.; Tada, M.; Takahashi, S.; Takeda, A.; Takeuchi, Y.; Tanaka, H. K.; Tanaka, H. A.; Terhorst, D.; Terri, R.; Thakore, T.; Thompson, L. F.; Tobayama, S.; Toki, W.; Tomura, T.; Touramanis, C.; Tsukamoto, T.; Tzanov, M.; Uchida, Y.; Vacheret, A.; Vagins, M.; Vallari, Z.; Vasseur, G.; Wachala, T.; Wakamatsu, K.; Walter, C. W.; Wark, D.; Warzycha, W.; Wascko, M. O.; Weber, A.; Wendell, R.; Wilkes, R. J.; Wilking, M. J.; Wilkinson, C.; Wilson, J. R.; Wilson, R. J.; Yamada, Y.; Yamamoto, K.; Yamamoto, M.; Yanagisawa, C.; Yano, T.; Yen, S.; Yershov, N.; Yokoyama, M.; Yoo, J.; Yoshida, K.; Yuan, T.; Yu, M.; Zalewska, A.; Zalipska, J.; Zambelli, L.; Zaremba, K.; Ziembicki, M.; Zimmerman, E. D.; Zito, M.; Żmuda, J.; T2K Collaboration

2016-11-01

We report the first measurement of the flux-averaged cross section for charged current coherent π+ production on carbon for neutrino energies less than 1.5 GeV, and with a restriction on the final state phase space volume in the T2K near detector, ND280. Comparisons are made with predictions from the Rein-Sehgal coherent production model and the model by Alvarez-Ruso et al., the latter representing the first implementation of an instance of the new class of microscopic coherent models in a neutrino interaction Monte Carlo event generator. We observe a clear event excess above background, disagreeing with the null results reported by K2K and SciBooNE in a similar neutrino energy region. The measured flux-averaged cross sections are below those predicted by both the Rein-Sehgal and Alvarez-Ruso et al. models.

Collisional and Dynamical Evolution of Planetary Systems

NASA Technical Reports Server (NTRS)

Weidenschilling, Stuart J.

2004-01-01

Senior Scientst S. J. Weidenschilling presents his final administrative report in the research program entitled "Collisional and Dynamical Evolution of Planetary Systems," on which he was the Principal Investigator. This research program produced the following publications: 1) "Jumping Jupiters" in binary star systems. F. Marzari, S. J. Weidenschilling, M. Barbieri and V. Granata. Astrophys. J., in press, 2005; 2) Formation of the cores of the outer planets. To appear in "The Outer Planets" (R. Kallenbach, ED), ISSI Conference Proceedings (Space Sci. Rev.), in press, 2005; 3) Accretion dynamics and timescales: Relation to chondrites. S. J. Weidenschilling and J. Cuzzi. In Meteorites and the Early Solar System LI (D. Lauretta et al., Eds.), Univ. of Arizona Press, 2005; 4) Asteroidal heating and thermal stratification of the asteroid belt. A. Ghosh, S. J.Weidenschilling, H. Y. McSween, Jr. and A. Rubin. In Meteorites and the Early Solar System I1 (D. Lauretta et al., Eds.), Univ. of Arizona Press, 2005.

Digital particle image thermometry/velocimetry: a review

NASA Astrophysics Data System (ADS)

Dabiri, Dana

2009-02-01

Digital particle image thermometry/velocimetry (DPIT/V) is a relatively new methodology that allows for measurements of simultaneous temperature and velocity within a two-dimensional domain, using thermochromic liquid crystal tracer particles as the temperature and velocity sensors. Extensive research has been carried out over recent years that have allowed the methodology and its implementation to grow and evolve. While there have been several reviews on the topic of liquid crystal thermometry (Moffat in Exp Therm Fluid Sci 3:14-32, 1990; Baughn in Int J Heat Fluid Flow 16:365-375, 1995; Roberts and East in J Spacecr Rockets 33:761-768, 1996; Wozniak et al. in Appl Sci Res 56:145-156, 1996; Behle et al. in Appl Sci Res 56:113-143, 1996; Stasiek in Heat Mass Transf 33:27-39, 1997; Stasiek and Kowalewski in Opto Electron Rev 10:1-10, 2002; Stasiek et al. in Opt Laser Technol 38:243-256, 2006; Smith et al. in Exp Fluids 30:190-201, 2001; Kowalewski et al. in Springer handbook of experimental fluid mechanics, 1st edn. Springer, Berlin, pp 487-561, 2007), the focus of the present review is to provide a relevant discussion of liquid crystals pertinent to DPIT/V. This includes a background on liquid crystals and color theory, a discussion of experimental setup parameters, a description of the methodology’s most recent advances and processing methods affecting temperature measurements, and finally an explanation of its various implementations and applications.

Can dryland geoproxy data generate Quaternary palaeoclimate and palaeoenvironmental records?

NASA Astrophysics Data System (ADS)

Thomas, David S. G.

2017-04-01

Dryland regions present many challenges for robustly reconstructing late Quaternary palaeoenvironments and palaeoclimates, not least a common deficit, or considerable spatial variability, in the availability of high resolution biological proxy data sources. Substantial advances have been made in some regions in recent years, through the exploitation of new high resolution biomarker and isotope records, for example from hyrax middens (e.g. Chase et al., 2012) and from offshore sediments (e.g. Collins et al., 2014). In others however, suitable data sources for these approaches are absent, so these approaches are not available or if data are applied from distant sources, subject to risks of excessive spatial extrapolation of records in environmental contexts where environmental gradients are steep and variability is common (Thomas and Burrough, 2012, Thomas et al., 2013). In these contexts, geoproxy records, derived from the analysis of landforms and their associated sediments, are often utilised in dryland Quaternary research (e.g. Burrough and Thomas 2009, Stone and Thomas, 2013, Thomas, 2013, Lancaster et al., 2015), but with a number of associated difficulties (e.g. Chase, 2009). This paper examines these difficulties and then explores different approaches to the analysis of Quaternary landform records. It is argued that geoproxies with chronometric control, usually provided by OSL dating, have considerable potential to improve data on Quaternary environmental and climate dynamics, if records are interpreted effectively and appropriately (e.g. Bailey and Thomas, 2014, Thomas and Burrough, 2016). Examples of challenges and new approaches will be drawn from aeolian and fluvial domains, and from research in Africa, Australia and Arabia. Bailey RM, Thomas DSG 2014 Earth Surf. Proc. Landf. 39, 614-631. Burrough SL, Thomas DSG 2009. Geomorphology 103, 285-298. Chase, B 2009. Earth-Sci Rev. 93, 31-45. Chase BM et al. 2010 Quat. Sci. Rev. 56, 107-125. Collins JA et al. 2014 Earth Planet. Sci. Let. 398, 1-10. Lancaster N et al. 2016 Quat. Int. 410, 3-10. Stone AEC, Thomas DSG 2013 J. Arid Env. 93, 40-58. Thomas DSG 2013 Earth Surf. Proc. Landf. 38, 3-16. Thomas DSG, Burrough SL 2012 Quat. Int. 253, 5-17. Thomas DSG et al. 2012 J. Quat. Sci. 27, 7-12. Thomas DSG, Burrough SL 2016 Quat. Int. 410, 30-45.

Exploring Earth and the Solar System: Educational Outreach Through NASA's Space Place, SciJinks, and Climate Kids Websites

NASA Technical Reports Server (NTRS)

Meneses, Joseph Chistopher

2012-01-01

NASA's Space Place team publishes engaging content and creates an effective environment to inspire a young audience to dare mighty things. NASA uses the Space Place, Climate Kids, and SciJinks websites to cultivate interest among elementary-school-aged children in both science and technology. During my summer internship at Jet Propulsion Laboratory I used Adobe Flash and ActionScript 3 to develop content for the Space Place, Climate Kids, and SciJinks sites. In addition, I was involved in the development process for ongoing and new projects during my internship. My involvement allowed me to follow a project from concept to design, implementation, and release. I personally worked on three projects this summer, two of which are currently in deployment. The first is a scrambled letter-tile guessing game titled Solar System Scramble. The second, Butterfrog Mix-Up, is a rotating-tile puzzle game. The third project is a unfinished prototype for a maze game.

Monosodium Luminol for Improving Brain Function in Gulf War Illness

DTIC Science & Technology

2015-10-01

Jain et al., PLoS One, 7: e46340, 2012; McAvoy et al., Front Syst Neurosci , 9:120. eCollection 2015; Oomen et al., Wiley Interdiscip Rev Cogn Sci...2007; Yassa and Stark, Trends Neurosci , 34: 515-525). In this test, each rat successively explored two different sets of identical objects (object

Modeling collective behavior of molecules in nanoscale direct deposition processes

NASA Astrophysics Data System (ADS)

Lee, Nam-Kyung; Hong, Seunghun

2006-03-01

We present a theoretical model describing the collective behavior of molecules in nanoscale direct deposition processes such as dip-pen nanolithography. We show that strong intermolecular interactions combined with nonuniform substrate-molecule interactions can produce various shapes of molecular patterns including fractal-like structures. Computer simulations reveal circular and starlike patterns at low and intermediate densities of preferentially attractive surface sites, respectively. At large density of such surface sites, the molecules form a two-dimensional invasion percolation cluster. Previous experimental results showing anisotropic patterns of various chemical and biological molecules correspond to the starlike regime [P. Manandhar et al., Phys. Rev. Lett. 90, 115505 (2003); J.-H. Lim and C. A. Mirkin, Adv. Mater. (Weinheim, Ger.) 14, 1474 (2002); D. L. Wilson et al., Proc. Natl. Acad. Sci. U.S.A. 98, 13660 (2001); M. Su et al., Appl. Phys. Lett. 84, 4200 (2004); R. McKendry et al., Nano Lett. 2, 713 (2002); H. Zhou et al., Appl. Surf. Sci. 236, 18 (2004); G. Agarwal et al., J. Am. Chem. Soc. 125, 580 (2003)].

SciServer Compute brings Analysis to Big Data in the Cloud

NASA Astrophysics Data System (ADS)

Raddick, Jordan; Medvedev, Dmitry; Lemson, Gerard; Souter, Barbara

2016-06-01

SciServer Compute uses Jupyter Notebooks running within server-side Docker containers attached to big data collections to bring advanced analysis to big data "in the cloud." SciServer Compute is a component in the SciServer Big-Data ecosystem under development at JHU, which will provide a stable, reproducible, sharable virtual research environment.SciServer builds on the popular CasJobs and SkyServer systems that made the Sloan Digital Sky Survey (SDSS) archive one of the most-used astronomical instruments. SciServer extends those systems with server-side computational capabilities and very large scratch storage space, and further extends their functions to a range of other scientific disciplines.Although big datasets like SDSS have revolutionized astronomy research, for further analysis, users are still restricted to downloading the selected data sets locally - but increasing data sizes make this local approach impractical. Instead, researchers need online tools that are co-located with data in a virtual research environment, enabling them to bring their analysis to the data.SciServer supports this using the popular Jupyter notebooks, which allow users to write their own Python and R scripts and execute them on the server with the data (extensions to Matlab and other languages are planned). We have written special-purpose libraries that enable querying the databases and other persistent datasets. Intermediate results can be stored in large scratch space (hundreds of TBs) and analyzed directly from within Python or R with state-of-the-art visualization and machine learning libraries. Users can store science-ready results in their permanent allocation on SciDrive, a Dropbox-like system for sharing and publishing files. Communication between the various components of the SciServer system is managed through SciServer‘s new Single Sign-on Portal.We have created a number of demos to illustrate the capabilities of SciServer Compute, including Python and R scripts accessing a range of datasets and showing the data flow between storage and compute components.Demos, documentation, and more information can be found at www.sciserver.org.SciServer is funded by the National Science Foundation Award ACI-1261715.

A New Type of Transient Luminous Events Produced by Terrestrial Gamma-ray Flashes

NASA Astrophysics Data System (ADS)

Xu, W.; Celestin, S. J.; Pasko, V. P.; Marshall, R. A.

2016-12-01

Discovered in 1994 by the Burst and Transient Source Experiment (BATSE) detector aboard the Compton Gamma-Ray Observatory [Fishman et al., Science, 264, 1313, 1994], Terrestrial Gamma-ray Flashes (TGFs) are high-energy photon bursts originating from the Earth's atmosphere characterized by their close association with thunderstorm activities. Since the discovery, TGFs have also been observed by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) [Smith et al., Science, 307, 1085, 2005], the Fermi Gamma-ray Space Telescope [Briggs et al., JGR, 115, A07323, 2010], and the Astrorivelatore Gamma a Immagini Leggero (AGILE) satellite [Marisaldi et al., JGR, 115, A00E13, 2010]. Space-borne measurements have revealed the temporal and spectral features of TGFs: typically lasting from fractions of to a few milliseconds, having a fluence of fractions of photons/cm2, and exhibiting a hard energy spectra extending up to a few tens of MeVs [Dwyer et al., Space Sci. Rev., 173, 133, 2012]. Moreover, detailed analyses of radio emissions have pointed out the close correlation between TGFs and the initial development stages of normal polarity intra-cloud lightning that transports negative charge upward (+IC) [e.g., Lu et al., GRL, 37, L11806, 2010; JGR, 116, A03316, 2011]. In this work, we show that, while TGFs pass through the atmosphere, the large quantities of energetic electrons knocked out during collisions of gamma-rays with air molecules can generate significant amount of excited species of neutral and ionized nitrogen molecules, thereby leading to production of a new type of transient luminous events (TLEs). The spectroscopic and morphological features of this predicted luminous phenomenon have been theoretically quantified in the framework of Monte Carlo simulations. Considering the measurability of this type of events and its close relation with TGFs, corresponding measurements would provide a novel perspective to investigate TGFs, as well as the initial breakdown stage of lightning discharges.

Exploring a Model of Situated Professional Development: Impact on Classroom Practice

ERIC Educational Resources Information Center

Singer, Jonathan; Lotter, Christine; Feller, Robert; Gates, Harry

2011-01-01

A hallmark of current science education reform involves teaching through inquiry. However, the widespread use of inquiry-based instruction in many classrooms has not occurred (Roehrig and Luft in "Int J Sci Educ" 26:3-24, 2004; Schneider et al. in "J Res Sci Teach" 42:283-312, 2005). The purpose of this study was to investigate the impact of a…

Erratum: “Multi-point, high-speed passive ion velocity distribution diagnostic on the Pegasus Toroidal Experiment” [Rev. Sci. Instrum. 83, 10D516 (2012)

DOE PAGES

Burke, Marcus G.; Fonck, Raymond J.; Bongard, Michael W.; ...

2016-07-18

This article corrects an error in M.G. Burke et al., 'Multi-point, high-speed passive ion velocity distribution diagnostic on the Pegasus Toroidal Experiment,' Rev. Sci. Instrum. 83, 10D516 (2012) pertaining to ion temperature. The conclusions of this paper are not altered by the revised ion temperature measurements.

The Importance of In Situ Measurements and Sample Return in the Search for Chemical Biosignatures on Mars or other Solar System Bodies (Invited)

NASA Astrophysics Data System (ADS)

Glavin, D. P.; Brinckerhoff, W. B.; Conrad, P. G.; Dworkin, J. P.; Eigenbrode, J. L.; Getty, S.; Mahaffy, P. R.

2013-12-01

The search for evidence of life on Mars and elsewhere will continue to be one of the primary goals of NASA's robotic exploration program for decades to come. NASA and ESA are currently planning a series of robotic missions to Mars with the goal of understanding its climate, resources, and potential for harboring past or present life. One key goal will be the search for chemical biomarkers including organic compounds important in life on Earth and their geological forms. These compounds include amino acids, the monomer building blocks of proteins and enzymes, nucleobases and sugars which form the backbone of DNA and RNA, and lipids, the structural components of cell membranes. Many of these organic compounds can also be formed abiotically as demonstrated by their prevalence in carbonaceous meteorites [1], though, their molecular characteristics may distinguish a biological source [2]. It is possible that in situ instruments may reveal such characteristics, however, return of the right samples to Earth (i.e. samples containing chemical biosignatures or having a high probability of biosignature preservation) would enable more intensive laboratory studies using a broad array of powerful instrumentation for bulk characterization, molecular detection, isotopic and enantiomeric compositions, and spatially resolved chemistry that may be required for confirmation of extant or extinct life on Mars or elsewhere. In this presentation we will review the current in situ analytical capabilities and strategies for the detection of organics on the Mars Science Laboratory (MSL) rover using the Sample Analysis at Mars (SAM) instrument suite [3] and discuss how both future advanced in situ instrumentation [4] and laboratory measurements of samples returned from Mars and other targets of astrobiological interest including the icy moons of Jupiter and Saturn will help advance our understanding of chemical biosignatures in the Solar System. References: [1] Cronin, J. R and Chang S. (1993) In The Chemistry of Life's Origin, pp. 209-258. [2] Summons et al. (2008) Space Sci. Rev. 135, 133. [3] Mahaffy, P. R. et al. (2012) Space Sci. Rev. 170, 401. [4] Getty, S. A. et al. (2013) IEEE Aerospace Conf. Proc. 10.1109/AERO.2013.6497391.

Engineering Bony Hybrid Organs In Vitro

DTIC Science & Technology

2006-11-01

microfluidic cell culture system using elastomeric channels and Braille displays (Gu et al., 2004; Futai et al., 2004). We have now further developed this...Takayama S, 2004: Computerized microfluidic cell culture using elastomeric channels and braille displays. Proc. Natl. Acad. Sci. USA 101, 15861-15866

Temperament dictates endotoxin-induced metabolic changes in Brahman bulls

USDA-ARS?s Scientific Manuscript database

We previously reported that animal temperament influences the rectal temperature response, sickness behavior scores, serum concentrations of epinephrine (Burdick et al., 2011; Innate Immunity), and serum cytokine concentrations (Hulbert et al., 2009; J. Anim. Sci. 86 (Suppl 2):527) following a provo...

On the origin of the energy dissipation anomaly in (Hall) magnetohydrodynamics

NASA Astrophysics Data System (ADS)

Galtier, Sébastien

2018-05-01

Incompressible Hall magnetohydrodynamics (MHD) may be the subject of energy dissipation anomaly which stems from the lack of smoothness of the velocity and magnetic fields. I derive the exact expression of which appears to be closely connected with the well-known 4/3 exact law of Hall MHD turbulence theory. This remarkable similitude suggests a deeper mathematical property of the fluid equations. In the MHD limit, the expression of differs from the one derived by Gao et al (2013 Acta Math. Sci. 33 865–71) which presents miscalculations. The energy dissipation anomaly can be used to better estimate the local heating in space plasmas where in situ measurements are accessible.

Physics Criteria for a Subscale Plasma Liner Experiment

DOE PAGES

Hsu, Scott C.; Thio, Yong C. Francis

2018-02-02

Spherically imploding plasma liners, formed by merging hypersonic plasma jets, are a proposed standoff driver to compress magnetized target plasmas to fusion conditions (Hsu et al. in IEEE Trans Plasma Sci 40:1287, 2012). Here, in this paper, the parameter space and physics criteria are identified for a subscale, plasma-liner-formation experiment to provide data, e.g., on liner ram-pressure scaling and uniformity, that are relevant for addressing scientific issues of full-scale plasma liners required to achieve fusion conditions. Lastly, based on these criteria, we quantitatively estimate the minimum liner kinetic energy and mass needed, which informed the design of a subscale plasmamore » liner experiment now under development.« less

Physics Criteria for a Subscale Plasma Liner Experiment

DOE Office of Scientific and Technical Information (OSTI.GOV)

Hsu, Scott C.; Thio, Yong C. Francis

Spherically imploding plasma liners, formed by merging hypersonic plasma jets, are a proposed standoff driver to compress magnetized target plasmas to fusion conditions (Hsu et al. in IEEE Trans Plasma Sci 40:1287, 2012). Here, in this paper, the parameter space and physics criteria are identified for a subscale, plasma-liner-formation experiment to provide data, e.g., on liner ram-pressure scaling and uniformity, that are relevant for addressing scientific issues of full-scale plasma liners required to achieve fusion conditions. Lastly, based on these criteria, we quantitatively estimate the minimum liner kinetic energy and mass needed, which informed the design of a subscale plasmamore » liner experiment now under development.« less

Mechanisms of Cytotoxicity of the Aids Virus

DTIC Science & Technology

1994-08-01

al., 1987; Luciw et al., 1989), sheep (visna virus) (Haas et al., 1985), goats (caprine-arthritis encepha- litis virus) (Narayan & Cork , 1985), and...into therapeutic maneuvers which may suppress virus replication and/or cytopathicity, and assist in the development of a vaccine for WIV prevention. 7...and AIDS. Narayan and Cork , 1985, Rev. Infect. Dis. 7:89. Niederran et al., 1989, Proc. Natl. Acad. Sci. 86:1128. Pederson et al., 1987, Science 235

Spectro-polarimetry of Ice-dust Mixtures measured in the Laboratory with Application to the Solar System and Beyond

NASA Astrophysics Data System (ADS)

Poch, O.; Schmid, H. M.; Pommerol, A.; Jost, B.; Brouet, Y.; Thomas, N.

2015-12-01

Polarimetric observations of atmosphere-less Solar System bodies can give clues on the texture and on the physico-chemical composition of their surfaces, as reviewed by Mishchenko et al. (2010) and Bagnulo et al. (2011). Measurements performed in the laboratory on carefully characterized samples can provide reference data that can be used for direct comparison with remote-sensing polarimetric observations. In particular, we want to study the spectral dependence of the polarization and the way it is correlated or not with the surface albedo. In the Laboratory for Outflow Studies of Sublimating Materials (LOSSy) at the University of Bern, we have developed the capability to prepare and analyze optically thick analogues of planetary or cometary surfaces composed of water ice, minerals and carbonaceous compounds. Water-free dust of high porosity can also be produced by sublimation of ice under space-simulated conditions (Pommerol et al., 2015). Here, we present the first results of polarization measurements performed in the LOSSy. A Stokes polarimeter is used to measure the Stokes parameters describing the polarization of the visible light scattered by icy samples illuminated with a randomly polarized light simulating the star light. Additionally, a radio-goniometer, equipped with polarizers, can also measure the phase angle dependence of the linearly polarized scattered light. These measurements could provide interesting inputs to complement the theoretical models and predict or interpret spectro-polarimetric properties of Solar System objects and circumstellar disks. Mishchenko, M., et al., 2010, Polarimetric Remote Sensing of Solar System Objects. Bagnulo, S., et al., 2011, J. Quant. Spectrosc. Ra. 112, 2059. Pommerol, A., et al., 2015, Planet. Space Sci. 109-110, 106-122.

The Role of Scientific Communication Skills in Trainees' Intention to Pursue Biomedical Research Careers: A Social Cognitive Analysis.

PubMed

Cameron, Carrie; Lee, Hwa Young; Anderson, Cheryl; Byars-Winston, Angela; Baldwin, Constance D; Chang, Shine

2015-01-01

Scientific communication (SciComm) skills are indispensable for success in biomedical research, but many trainees may not have fully considered the necessity of regular writing and speaking for research career progression. Our purpose was to investigate the relationship between SciComm skill acquisition and research trainees' intentions to remain in research careers. We used social cognitive career theory (SCCT) to test a model of the relationship of SciComm skills to SciComm-related cognitive variables in explaining career intentions. A sample of 510 graduate students and postdoctoral fellows at major academic health science centers in the Texas Medical Center, Houston, Texas, were surveyed online. Results suggested that interest in performing SciComm tasks, SciComm outcome expectations (SCOEs), and SciComm productivity predicted intention to remain in a research career, while SciComm self-efficacy did not directly predict career intention. SCOEs also predicted interest in performing SciComm tasks. As in other SCCT studies, SciComm self-efficacy predicted SCOEs. We conclude that social cognitive factors of SciComm skill acquisition and SciComm productivity significantly predict biomedical trainees' intentions to pursue research careers whether within or outside academia. While further studies are needed, these findings may lead to evidence-based interventions to help trainees remain in their chosen career paths. © 2015 C. Cameron et al. CBE—Life Sciences Education © 2015 The American Society for Cell Biology. This article is distributed by The American Society for Cell Biology under license from the author(s). It is available to the public under an Attribution–Noncommercial–Share Alike 3.0 Unported Creative Commons License (http://creativecommons.org/licenses/by-nc-sa/3.0).

Self-organisation of adsorbed nitrogen on (100) and (410) copper faces: a SPA-LEED study

NASA Astrophysics Data System (ADS)

Sotto, M.; Croset, B.

2000-08-01

The self-organisation of nitrogen nanostructures at different coverages on a (100) copper surface is studied by spot profile analysing low energy electron diffraction (SPA-LEED). The existence of two surface states with a domain of coverage leading to coexistence of the two states as already observed by scanning tunneling microscopy (STM) [Leibsle and Robinson, Phys. Rev. B 47 (1993) 15 865; Leibsle et al., Surf. Sci. 317 (1994) 309; Leibsle, Surf. Sci. 440 (1999) L835] and low energy electron diffraction (LEED) [Sotto et al., Surf. Sci. 371 (1997) 36] is confirmed. In the first state, the surface is organised in square shape islands separated by bare copper <100> rows. This work shows that the surface periodicity depends on the preparation of the nitrogen overlayer. When nitrogen coverage is obtained by adsorption with a sample temperature near 320°C, the periodicity does not vary with coverage and is found to be equal to 55±2 Å. At coverages below 0.75±0.05 and if the nitrogen is deposited at room temperature followed by an anneal at 320°C, during long periods of time, the periodicity evolves to large values (˜97±3 Å). During thermal desorption, the long range order with decreasing coverage is maintained but the surface periodicity also evolves continuously to large values (˜100 Å). However, a surface periodicity of 55±2 Å seems to be a characteristic length of this system. The second surface state corresponds to large c(2×2)N domains separated by <110> trenches [Leibsle and Robinson, Phys. Rev. B 47 (1993) 15 865; Leibsle et al., Surf. Sci. 317 (1994) 309; Leibsle, Surf. Sci. 440 (1999) L835]. Nitrogen adsorption on a (410) stepped face induces a reconstruction into a (810) face with double step height. The complex behaviour of this film growth is discussed in the light of existing theories about the driving force leading to nanostructuration.

Anticipating Stock Market Movements with Google and Wikipedia

NASA Astrophysics Data System (ADS)

Moat, Helen Susannah; Curme, Chester; Stanley, H. Eugene; Preis, Tobias

Many of the trading decisions that have led to financial crises are captured by vast, detailed stock market datasets. Here, we summarize two of our recent studies which investigate whether Internet usage data contain traces of attempts to gather information before such trading decisions were taken. By analyzing changes in how often Internet users searched for financially related information on Google (Preis et al., Sci Rep 3:1684, 2013) and Wikipedia (Moat et al., Sci Rep 3:1801, 2013), patterns are found that may be interpreted as "early warning signs" of stock market moves. Our results suggest that online data may allow us to gain new insight into early information gathering stages of economic decision making.

Early Human Occupation on the Northeast Tibetan Plateau

NASA Astrophysics Data System (ADS)

Rhode, D.; Madsen, D.; Brantingham, P.; Perrault, C.

2010-12-01

The Tibetan Plateau presents great challenges for human occupation: low oxygen, high ultraviolet radiation, harsh seasonal climate, low overall biological productivity. How and when early humans were able to cope physiologically, genetically, and behaviorally with these extremes is important for understanding the history of human adaptive flexibility. Our investigations of prehistoric human settlement on the northeast Tibetan Plateau focus on (a) establishing well-dated evidence for occupation of altitudes >3000 m, (b) the environmental context of high altitude adaptation, and (c) relations of hunting and pastoralism to lower-altitude agrarian systems. We observe two major prehistoric settlement patterns in the Qinghai Lake area. The earliest, ~15,000-7500 yr old, consists of small isolated firehearths with sparse associated stone tools and wild mammal remains (1). Numerous hearths often occur in the same localities, indicating repeated short-duration occupations by small hunting parties. A second pattern, ~9000-4000 yr old, was established during the Holocene climatic optimum. These sites represent prolonged seasonal residential occupation, containing dark anthropogenic midden, hearth and pit constructions, abundant stone tools, occasional ceramics, and abundant diverse faunal remains (including medium-large mammals but lacking domestic sheep/yak)(2). These Plateau-margin base camps allowed greater intensity of use of the high Plateau. Residential occupation was strongly influenced by nearby lower-altitude farming communities; development of the socioeconomic landscape along the Yellow River likely played at least as great a role in Plateau occupation patterns as did Holocene environmental changes. Holocene vegetation changes in the NE Tibetan Plateau have been attributed to climate (3) or anthropogenic modification (4). Our results document changes in shrub/tree presence from ~12,000-4000 BP, similar to pollen records, that likely reflect climate rather than anthropogenic grazing pressure, because domestic yak/sheep remains are absent archaeologically before ~4000 BP. Our results have implications for the age of distinct Tibetan high-altitude physiological adaptations (5), suggested to be as recent as ~2750 BP. Prolonged occupation of Plateau margins commenced much earlier, but year-round occupation above 4000 m likely occurred only with the emergence of yak pastoralism (6). Genetic models need to consider which environmental factors lead to strong selection for genetic divergence (e.g., seasonal vs year-round occupation, occupation at ~3000 m vs >4000 m, etc); settlement history reconstructions such as that presented here can help. (1)Brantingham PJ, et al. 2007, Elsevier Dev Quat Sci 9:129-150; Madsen DB, et al. 2006, J Arch Sci 33:1433-1444. (2)Rhode D, et al. 2007, J Arch Sci 34:600-612. (3)Herzschuh, U, et al. 2010, Glo Ecol Biogeog 19:278-286. (4)Miehe G, et al. 2009, Palaeo Palaeo Palaeo 267:130-147.; Schlütz F., Lehmkuhl F., 2009, Quat Sci Rev 28:1449-1471. (5)Beall C, et al. 2010, PNAS 107:11459-11464; Simonson TS, et al. 2010, Science 329:72-75; Yi X. et al., 2010, Science 329:75-78. (6)Rhode D, et al. 2007, Elsevier Dev Quat Sci 9:205-226.

Helicon antenna radiation patterns in a high-density hydrogen linear plasma device

NASA Astrophysics Data System (ADS)

Caneses, J. F.; Blackwell, B. D.; Piotrowicz, P.

2017-11-01

Antenna radiation patterns in the vicinity of a helicon antenna are investigated in hydrogen plasmas produced in the MAGPIE linear plasma device. Using a uniform cold-plasma full-wave code, we model the wave physics in MAGPIE and find good agreement with experimental wave measurements. We show for the first time which antenna elements in a helicon device couple most strongly to the plasma and discuss the physical mechanism that determines this effect. Helicon wavefields in the near field of the antenna are best described in terms of the group velocity and ray direction, while far from the antenna, helicon wavefields behave like plane waves and are best described in terms of eigen-modes. In addition, we present recent 2D axis-symmetric full-wave simulations of the 120 kW helicon source in ProtoMPEX [Rapp et al., IEEE Trans. Plasma Sci. 44(12), 3456-3464 (2016); Caughman et al., J. Vac. Sci. Technol. Vac. Surf. Films 35, 03E114 (2017); and Goulding et al., Fusion Sci. Technol. 72(4), 588-594 (2017)] ( n e ˜ 5 × 1019 m-3, B 0 ˜ 70 mT, and f = 13.56 MHz) where the antenna radiation patterns are evident, and we provide an interpretation of the numerical results using the ideas developed in this paper.

Spectroscopic imaging of limiter heat and particle fluxes and the resulting impurity sources during Wendelstein 7-X startup plasmas.

PubMed

Stephey, L; Wurden, G A; Schmitz, O; Frerichs, H; Effenberg, F; Biedermann, C; Harris, J; König, R; Kornejew, P; Krychowiak, M; Unterberg, E A

2016-11-01

A combined IR and visible camera system [G. A. Wurden et al., "A high resolution IR/visible imaging system for the W7-X limiter," Rev. Sci. Instrum. (these proceedings)] and a filterscope system [R. J. Colchin et al., Rev. Sci. Instrum. 74, 2068 (2003)] were implemented together to obtain spectroscopic data of limiter and first wall recycling and impurity sources during Wendelstein 7-X startup plasmas. Both systems together provided excellent temporal and spatial spectroscopic resolution of limiter 3. Narrowband interference filters in front of the camera yielded C-III and H α photon flux, and the filterscope system provided H α , H β , He-I, He-II, C-II, and visible bremsstrahlung data. The filterscopes made additional measurements of several points on the W7-X vacuum vessel to yield wall recycling fluxes. The resulting photon flux from both the visible camera and filterscopes can then be compared to an EMC3-EIRENE synthetic diagnostic [H. Frerichs et al., "Synthetic plasma edge diagnostics for EMC3-EIRENE, highlighted for Wendelstein 7-X," Rev. Sci. Instrum. (these proceedings)] to infer both a limiter particle flux and wall particle flux, both of which will ultimately be used to infer the complete particle balance and particle confinement time τ P .

Variegation of active regions on comet 67P/Churyumov-Gerasimenko

NASA Astrophysics Data System (ADS)

Oklay, Nilda; Vincent, Jean-Baptiste; Fornasier, Sonia; Pajola, Maurizio; Besse, Sebastien; Lara, Luisa M.; Barucci, Maria Antonietta; Mottola, Stefano; Sierks, Holger; Pommerol, Antoine; Masoumzadeh, Nafiseh; Lazzarin, Monica; Scholten, Frank; Preusker, Frank; Hall, Ian

2015-11-01

Since Rosetta spacecraft’s arrival to the comet 67P, the OSIRIS scientific imager (Optical, Spectroscopic, and Infrared Remote Imaging System, Keller et al. 2007) is successfully observing the nucleus with high spatial resolution in the 250-1000 nm range thanks to set of 26 dedicated filters.While 67P has a typical red spectral slope, the active areas tend to display bluer spectra (Sierks et al. 2015, Fornasier et al. 2015). We performed a spectral analysis of the active areas and derived spectral characteristics of them, possibly indicating the presence of material enriched in volatiles.The ‘activity thresholds’ spectral method (Oklay et al, 2015) is used for the identification of the active areas. In most cases, areas detected with this technique have been later on confirmed as active sources (Lara et al. 2015, Lin et al. 2015, Vincent et al. 2015) by direct detection of dust jets. This technique is therefore able to identify currently active areas, but also predicts which regions of the surface are likely to become activated once they receive enough insolation.Acknowledgements: OSIRIS was built by a consortium led by the Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany, in collaboration with CISAS, University of Padova, Italy, the Laboratoire d'Astrophysique de Marseille, France, the Instituto de Astrofi­sica de Andalucia, CSIC, Granada, Spain, the Scientific Support Office of the European Space Agency, Noordwijk, The Netherlands, the Instituto Nacional de Tecnica Aeroespacial, Madrid, Spain, the Universidad Politechnica de Madrid, Spain, the Department of Physics and Astronomy of Uppsala University, Sweden, and the Institut für Datentechnik und Kommunikationsnetze der Technischen Universität Braunschweig, Germany. We thank the Rosetta Science Ground Segment at ESAC, the Rosetta Mission Operations Centre at ESOC and the Rosetta Project at ESTEC for their outstanding work enabling the science return of the Rosetta Mission.Keller, et al. 2007, Space Sci. Rev., 128, 433Sierks et al. 2015, Science, 347,1Fornasier et al. 2015, A&A, published onlineLara et al. 2015, A&A, published onlineLin et al. 2015, A&A, published onlineVincent et al. 2015, A&A, submittedOklay et al. 2015, in preparation

Investigation of micrometre-sized fossil by laser mass spectrometer (LMS) designed for in situ space research

NASA Astrophysics Data System (ADS)

Tulej, Marek; Neubeck, Anna; Ivarsson, Magnus; Brigitte Neuland, Maike; Riedo, Andreas; Wurz, Peter

2015-04-01

Search for signatures of life on other planets is one of the most important goals of current planetary missions. Among various possible biomarkers, which can be investigated in situ on planetary surfaces, the detection of bio-relevant elements in planetary materials is of considerable interest and the abundance of isotopes can be important signatures of past and present bioactivities [1, 2]. We investigate the chemical composition of fossilised biological inclusions embedded in a carbonate host phase by a miniature laser ablation mass spectrometer (LMS) [3]. The LMS instrument combines a laser ablation ion source for ablation, atomisation and ionisation of surface material with a reflectron time-of-flight (TOF) mass spectrometer. LMS delivers mass spectra of almost all elements and their isotopes. In the current setup a fs-laser ablation ion source is applied with high lateral (15 um) and vertical (sub-um) resolution [4, 7] and the mass analyser supports mass resolution of 400-500 (at 56Fe mass peak) and dynamic range of eight orders of magnitude [5, 6]. From the 200 mass spectra recorded at 200 different locations on the carbonate sample surface, five mass spectra were identified which recorded the chemical composition of inclusions; from the other mass spectra the composition of the carbonate host matrix could be determined. The microscopic inspection of the sample surface and correlation with the coordinates of the laser ablation measurements made the confirmation to the location of the inclusion [8]. For the carbonate host matrix, the mass spectrometric analysis yielded the major elements H, C, O, Na, Mg, K and Ca and the trace elements Li, B and Cl. The measurements at the inclusion locations yielded in addition, the detection of F, Si, P, S, Mn, Fe, Ni, Co and Se. For most of the major elements the isotope ratios were found to be conform to the terrestrial values within a few per mills, while for minor and trace elements the determination of isotope ratios were less accurate due to low signal to noise ratios (SNR). The isotope abundances for the lightest isotope of B, S were observed to be larger than terrestrial, which is consistent with isotope fractionation by bio-relevant processes and a salty ocean. The studies demonstrates the current performance of the miniature LMS for in situ investigation of highly heterogeneous samples and its capabilities for the identification of fossilised biological matter. References: [1] Summons et al., Astrobiology, 11, 157, 2011. [2] Wurz et al., Sol. Sys. Res. 46 408, 2012. [3] Rohner et al.,Meas. Sci. Technol., 14, 2159, 2003. [4] Riedo et al., J. Anal. Atom. Spectrom. 28, 1256, 2013. [5] Riedo et al., J. Mass Spectrom.48, 1, 2013. [6] Neuland et al., Planet. Space. Sci. 101, 196, 2014. [7] Grimaudo et al., Anal. Chem. 2014, submitted. [8] Tulej et al. Geostand. Geoanal. Res., 2014; DOI: 10.1111/j.1751-908X.2014.00302.x

Mass Spectrometry in Jupiter's Atmosphere: Vertical Variation of Volatile Vapors

NASA Astrophysics Data System (ADS)

Wong, Michael H.; Atreya, Sushil K.; Mahaffy, Paul R.

2014-05-01

The Galileo Probe made the first and only in situ measurements of composition in Jupiter's atmosphere, led by the Galileo Probe Mass Spectrometer, or GPMS [1]. The major contribution from this instrument was the measurement of abundances and isotope ratios of the noble gases, as well as the volatile gases CH4, NH3, H2O, and H2S [2,3]. These initial results were further refined by detailed laboratory calibrations for the noble gases [4] and the volatiles [5]. The probe measurements resulted in the first determination of the heavy element abundances (except carbon that was known previously) and He/H ratio, which provide critical constraints to models of the formation of Jupiter and the origin of its atmosphere [6,7]. The condensable volatiles, or CVs (ammonia, H2S, and water), increased with depth in the probe entry site. This vertical variation was observed at levels much deeper than the modeled cloud bases, as predicted by one-dimensional chemical equilibrium models. The discrepancy is due to the probe's entry into a dry region known as a 5-μm hot spot. The 5-μm hot spots are part of an atmospheric wave system that encircles Jupiter just north of the equator. Despite the anomalous meteorology, the bulk abundances of NH3 and H2S were measured by the probe, and found to be enriched with respect to solar composition (similarly to the non-condensable volatile CH4). The deepest water mixing ratio, however, was observed to be depleted relative to solar composition. We review an updated context for the CV vertical profiles measured by the GPMS, based on the latest results from remote sensing, simulation, and reinterpretation of Galileo Probe measurements. In particular, we find that (1) the bulk abundance of water in Jupiter's atmosphere must be greater than the subsolar abundance derived from the deepest GPMS measurements [8], and that (2) CV mixing ratios are controlled by a range of processes in addition to condensation of the ices NH3, NH4SH, and H2O [5-9]. Both bulk abundances and spatial variation of these species will be further constrained by the Juno mission, scheduled to arrive at Jupiter in 2016. References: [1] Niemann, H.B. et al. 1992, SSRv 60, 111-142 [2] Niemann, H.B. et al. 1996, Science 272, 846-849 [3] Niemann, H.B. et al. 1998, JGR 103, 22831-22845 [4] Mahaffy, P.R. et al. 2000, JGR 105, 15061-15071 [5] Wong, M.H. et al. 2004, Icarus 171, 153-170 [6] Atreya, S.K. et al., 1999, Planet. Space Sci. 47, 1243-1262 [7] Atreya, S.K. et al., 2003, Planet. Space Sci. 451, 105-112 [8] Wong, M.H. et al., 2008, in Reviews in Mineralogy and Geochemistry, vol. 68. Mineralogical Society of America, Chantilly, VA, pp. 219-246 [9] Wong, M.H., 2009, Icarus 199, 231-235

Boolean networks with veto functions

NASA Astrophysics Data System (ADS)

Ebadi, Haleh; Klemm, Konstantin

2014-08-01

Boolean networks are discrete dynamical systems for modeling regulation and signaling in living cells. We investigate a particular class of Boolean functions with inhibiting inputs exerting a veto (forced zero) on the output. We give analytical expressions for the sensitivity of these functions and provide evidence for their role in natural systems. In an intracellular signal transduction network [Helikar et al., Proc. Natl. Acad. Sci. USA 105, 1913 (2008), 10.1073/pnas.0705088105], the functions with veto are over-represented by a factor exceeding the over-representation of threshold functions and canalyzing functions in the same system. In Boolean networks for control of the yeast cell cycle [Li et al., Proc. Natl. Acad. Sci. USA 101, 4781 (2004), 10.1073/pnas.0305937101; Davidich et al., PLoS ONE 3, e1672 (2008), 10.1371/journal.pone.0001672], no or minimal changes to the wiring diagrams are necessary to formulate their dynamics in terms of the veto functions introduced here.

High Temperature, Controlled-Atmosphere Aerodynamic Levitation Experiments with Applications in Planetary Science

NASA Astrophysics Data System (ADS)

Macris, C. A.; Badro, J.; Eiler, J. M.; Stolper, E. M.

2016-12-01

The aerodynamic levitation laser apparatus is an instrument in which spherical samples are freely floated on top of a stream of gas while being heated with a CO2laser to temperatures up to about 3500 °C. Laser heated samples, ranging in size from 0.5 to 3.5 mm diameter, can be levitated in a variety of chemically active or inert atmospheres in a gas-mixing chamber (e.g., Hennet et al. 2006; Pack et al. 2010). This allows for containerless, controlled-atmosphere, high temperature experiments with potential for applications in earth and planetary science. A relatively new technique, aerodynamic levitation has been used mostly for studies of the physical properties of liquids at high temperatures (Kohara et al. 2011), crystallization behavior of silicates and oxides (Arai et al. 2004), and to prepare glasses from compositions known to crystallize upon quenching (Tangeman et al. 2001). More recently, however, aerodynamic levitation with laser heating has been used as an experimental technique to simulate planetary processes. Pack et al. (2010) used levitation and melting experiments to simulate chondrule formation by using Ar-H2 as the flow gas, thus imposing a reducing atmosphere, resulting in reduction of FeO, Fe2O3, and NiO to metal alloys. Macris et al. (2015) used laser heating with aerodynamic levitation to reproduce the textures and diffusion profiles of major and minor elements observed in impact ejecta from the Australasian strewn field, by melting a powdered natural tektite mixed with 60-100 μm quartz grains on a flow of pure Ar gas. These experiments resulted in quantitative modeling of Si and Al diffusion, which allowed for interpretations regarding the thermal histories of natural tektites and their interactions with the surrounding impact vapor plume. Future experiments will employ gas mixing (CO, CO2, H2, O, Ar) in a controlled atmosphere levitation chamber to explore the range of fO2applicable to melt-forming impacts on other rocky planetary bodies, including the Moon and Mars. Arai et al., Rev. Sci. Instrum. 75, 2262-2265 (2004) Hennet et al., Rev. Sci. Instrum. 73, 124-129 (2001) Kohara et al., P. Natl. Acad. Sci.USA 108, 14780-14785 (2011) Macris et al., GSA Abstracts with Programs 47, 437 (2015) Pack et al., Geochem. T. 11, 1-16 (2010) Tangeman et al., Geophys. Res. Lett. 28, 2517-2520 (2001)

Analysis of ground-based and VIRTIS-M/ROSETTA reflectance spectra of asteroid 2687 Šteins: A comparison

NASA Astrophysics Data System (ADS)

Markus, K.; Arnold, G.; Hiesinger, H.; Capaccioni, F.

2012-04-01

The asteroid 2687 Šteins was encountered by Rosetta in 2008. Prior to the fly-by, ground-based observations of Šteins were performed [1, 2, 3, 4, 5, 6]. We present a summary of ground-based VIS and NIR reflectance spectra of Šteins and compare them with VIRTIS-M-spectra obtained during the fly-by. On the basis of these spectral data we discuss the relationship to meteorite materials, and the classification of Šteins. The ground-based spectra cover a wavelength range from 0.4-2.5 µm. All spectra show a clear absorption feature at ~0.5 µm and a steep spectral slope between ~0.6-0.8 µm. At wavelengths >1 µm the spectra show a neutral to slightly reddish trend. The absorption band at ~0.5 µm is commonly linked to the feature at that wavelength in the oldhamite spectrum [7]. The oldhamite spectrum shows another weaker feature at 0.96 µm. This weaker feature at ~0.96 µm is visible in two of the ground-based spectra. Spectral slopes of most Earth-based spectra are comparable within arrow bars. The uniform spectral characteristics indicate a homogenous surface of Šteins. The VIRTIS-M-spectra of Šteins cover the wavelength range from 0.25-1 µm (VIS) and 1-5 µm (IR). The spectra show an overall flat behavior with a steep red slope at wavelengths <1 µm. The absorption feature located at ~0.5 µm is clearly visible. At wavelengths >3.5 µm thermal emission contributes significantly to the detected radiation. The thermal properties derived from VIRTIS-M long wavelength measurements suggest a thin regolith layer and a low porosity. The shape of the asteroid is consistent with the hypothesis that Šteins is a rubble-pile. Ground-based and fly-by spectra of Šteins are in good agreement with each other considering the overall spectral characteristics and the occurrence of the absorption feature at 0.5 µm. Prior to the Rosetta fly-by Šteins has been classified (by e.g. [1, 5]) as an E[II]-type asteroid (after [8, 9], also Xe after [10]). VIRTIS data suggest that Šteins can be classified as an igneous E-type asteroid, being a member of the E[II]-subclass. E-type asteroids are linked to aubrites, which are nearly monomineralic enstatite achondrites [11]. This interpretation is supported by comparative laboratory reflectance measurements. Although aubrites give the best agreement with Šteins spectra, several spectral features cannot be assigned unambiguously. Ti-rich minerals or space weathering implanted products were alternatively proposed to reproduce the observed spectral characteristics [1, 12]. Currently no meteorite in our present collection fits the Šteins spectra, indicating that Šteins is probably not the parent body of these meteorites. Because Šteins is a reduced anhydrous body, it can be argued that it formed in the inner planetary system and was scattered to the main belt. This opens interesting parallels between the E-type population and the formation of Mercury. [1] Barucci et al. (2005) A&A, 430, 313-317. [2] Dotto et al. (2009) A&A, 494, L29-L32. [3] Fornasier et al. (2007) A&A, 474, L29-L32. [4] Fornasier et al. (2008) Icarus, 196, 119-134. [5] Nedelcu et al. (2007) A&A, 473, L33-L36. [6] Weissman et al. (2008) Met. Planet. Sci, 43, 905-914. [7] Burbine at al. (2002) Met. Planet. Sci., 37, 1233-1244. [8] Tholen D. J. (1989) in Asteroids II, 1139-1150. [9] Gaffey and Kelley (2004) LPSC XXXV. Abstract #1812. [10] Bus and Binzel (2002) Icarus, 158, 146-177. [11] Keil (2010) Chem. Erde-Geochem., 70, 295-317. [12] Shestopalov et al. (2010) Planet. Space Sci., 58, 1400-1403.

An angle encoder for super-high resolution and super-high accuracy using SelfA

NASA Astrophysics Data System (ADS)

Watanabe, Tsukasa; Kon, Masahito; Nabeshima, Nobuo; Taniguchi, Kayoko

2014-06-01

Angular measurement technology at high resolution for applications such as in hard disk drive manufacturing machines, precision measurement equipment and aspherical process machines requires a rotary encoder with high accuracy, high resolution and high response speed. However, a rotary encoder has angular deviation factors during operation due to scale error or installation error. It has been assumed to be impossible to achieve accuracy below 0.1″ in angular measurement or control after the installation onto the rotating axis. Self-calibration (Lu and Trumper 2007 CIRP Ann. 56 499; Kim et al 2011 Proc. MacroScale; Probst 2008 Meas. Sci. Technol. 19 015101; Probst et al Meas. Sci. Technol. 9 1059; Tadashi and Makoto 1993 J. Robot. Mechatronics 5 448; Ralf et al 2006 Meas. Sci. Technol. 17 2811) and cross-calibration (Probst et al 1998 Meas. Sci. Technol. 9 1059; Just et al 2009 Precis. Eng. 33 530; Burnashev 2013 Quantum Electron. 43 130) technologies for a rotary encoder have been actively discussed on the basis of the principle of circular closure. This discussion prompted the development of rotary tables which achieve reliable and high accuracy angular verification. We apply these technologies for the development of a rotary encoder not only to meet the requirement of super-high accuracy but also to meet that of super-high resolution. This paper presents the development of an encoder with 221 = 2097 152 resolutions per rotation (360°), that is, corresponding to a 0.62″ signal period, achieved by the combination of a laser rotary encoder supplied by Magnescale Co., Ltd and a self-calibratable encoder (SelfA) supplied by The National Institute of Advanced Industrial Science & Technology (AIST). In addition, this paper introduces the development of a rotary encoder to guarantee ±0.03″ accuracy at any point of the interpolated signal, with respect to the encoder at the minimum resolution of 233, that is, corresponding to a 0.0015″ signal period after interpolation of 212 (= 4096) divisions through the interpolator.

Smooth pond-like deposits on asteroid 4 Vesta: First results from the Dawn mission.

NASA Astrophysics Data System (ADS)

Hiesinger, H.; Ruesch, O.; Jaumann, R.; Nathues, A.; Raymond, C. A.; Russell, C. T.

2012-04-01

The Dawn spacecraft arrived at Vesta on July 16, 2011 to study the asteroid with a Framing Camera (FC), a Visible & Infrared Spectrometer (VIR), and a Gamma Ray and Neutron Detector (GRaND) [1]. Dawn provides the first high-resolution data from its survey orbit, high-altitude mapping orbit (HAMO), and low-altitude mapping orbit (LAMO). FC data revealed smooth pond-like deposits of ambiguous origin, similar to deposits on other asteroids, including Eros and Itokawa [2,3]. Several scenarios for the origin of these deposits can be tested with Dawn data, including volcanism, impact sedimentation, impact melt deposition, dust levitation and transport, seismic shaking, or landslides. We measured 83 small (~7 km2 average size) smooth deposits distributed across the surface of Vesta. Most ponds on Vesta occur on the floors of impact craters and in irregular depressions. We did not observe inflow of material into the depressions. Most of these deposits have well-defined geological contacts, indicating that they are younger than the surrounding terrain. However, lunar impact melt pools that formed contemporaneously with surrounding ejecta blankets show similar stratigraphic relationships. Sometimes the albedo of these ponds is lower than the surrounding terrain, in other cases the ponds are indistinguishable from the adjacent terrain. The ponds preferentially occur in a band between -10 and 30 degrees latitude with fewer ponds north of ~30 degrees and even fewer ponds in the southern hemisphere, i.e., the Rheasilvia region. The largest cluster of ponds occurs in the vicinity of the Marcia impact crater, which is part of the so-called snowman craters. Similar, but smaller (<230 m diameter) smooth ponds were also reported from the surface of asteroid Eros [2]. Robinson et al. [2] found that most smooth ponds on Eros occur in equatorial regions and concluded that the most likely process for their formation is electrostatic levitation and redistribution of the finest regolith components (<100 µm). Sierks et al. [4] argued that along the terminator, particularly strong electric fields can develop between the sun-lit and shaded areas, e.g., within craters, resulting in particle motion from sun-lit to dark regions. Dust levitation and transport was also discussed for asteroid 25143 Itokawa [3]. [1] Russell et al., (2007), Earth Moon Planets, 101; [2] Robinson et al., (2002), Met. Planet. Sci., 37; [3] Yano et al., (2006), Science, 312; [4] Sierks et al., (2011), Space Sci. Rev., doi:10.1007/s11214-011-9745-4. This research has been supported by the German Space Agency (DLR) and NASA. We would like to thank the Dawn Operations Team for their success-ful planning and acquisition of high-quality Vesta data.

Comparative Study on Hot Atom Coronae of Solar and Extrasolar Planets

NASA Astrophysics Data System (ADS)

Shematovich, Valery

Solar/stellar forcing on the upper atmospheres of the solar and extrasolar planets via both absorption of the XUV (soft X-rays and extreme ultraviolet) radiation and atmospheric sputtering results in the formation of an extended neutral corona populated by the suprathermal (hot) H, C, N, and O atoms (see, e.g., Johnson et al., 2008). The hot corona, in turn, is altered by an inflow of the solar wind/magnetospheric plasma and local pick-up ions onto the planetary exosphere. Such inflow results in the formation of the superthermal atoms (energetic neutral atoms - ENAs) due to the charge exchange with the high-energy precipitating ions and can affect the long-term evolution of the atmosphere due to the atmospheric escape. The origin, kinetics and transport of the suprathermal H, C, N, and O atoms in the transition regions (from thermosphere to exosphere) of the planetary atmospheres are discussed. Reactions of dissociative recombination of the ionospheric ions CO _{2} (+) , CO (+) , O _{2} (+) , and N _{2} (+) with thermal electrons are the main photochemical sources of hot atoms. The dissociation of atmospheric molecules by the solar/stellar XUV radiation and accompanying photoelectron fluxes and the induced exothermic photochemistry are also the important sources of the suprathermal atoms. Such kinetic systems with the non-thermal processes are usually investigated with the different (test particles, DSMC, and hybrid) versions of the kinetic Monte Carlo method. In our studies the kinetic energy distribution functions of suprathermal and superthermal atoms were calculated using the stochastic model of the hot planetary corona (Shematovich, 2004, 2010; Groeller et al., 2014), and the Monte Carlo model (Shematovich et al., 2011, 2013) of the high-energy proton and hydrogen atom precipitation into the atmosphere respectively. These functions allowed us to estimate the space distribution of suprathermals in the planetary transition regions. An application of these numerical models to study the atmospheric gas flow in the transition region from the collision-dominated thermosphere to collisionless exosphere, and the non-thermal escape will be discussed and illustrated with the simple 1D-models of the hot coronae of the solar and extrasolar planets. This work is supported by the RFBR project No. 14-02-00838a and by the Basic Research Program of the Presidium of the Russian Academy of Sciences (Program 22). begin{itemize} Johnson et al., Sp. Sci.Rev., 2008, v. 139, 355. Shematovich, Solar System Res., 2004, v.38, 28. Shematovich, Solar System Res., 2010, v.44, 96. Shematovich et al., J. Geophys. Res., 2011, v.116, A11320; 2013, v. 118, 1231. Groeller et al., Planet. Space Sci., 2014.

Multifactorial Assessment of Depleted Uranium Neurotoxicity

DTIC Science & Technology

2006-12-01

for submission to journals. These are included in the Appendix, and are: 1. Barber et al., Neurological effects of acute uranium exposure with and...also presented) D.S. Barber and M.J. Kopplin. Regional distribution of uranium in rat brain. Toxicol. Sci. 72 (supplement): 19, 2003. (Society of...Toxicology, 2003) J.W. Munson, J.K. Tolson, B.S. Jortner, S.M. Roberts and D.S. Barber . Heat shock proteins and uranium nephrotoxicity. Toxicol. Sci

The Aplacophora: History, Taxonomy, Phylogeny, Biogeography, and Ecology

DTIC Science & Technology

1992-02-01

Great Bay.] Pp. 28-41. In: A. I. Kafanov (ed.), [ Hydrobiological research of bays and inlets of Primorye.] Far East Science Center, USSR Acad. Sci...gonadal products into the sea (Franzdn 1955; Buckland-Nicks and Chia 1989). The Neomeniomorpha have a slightly modified sperm (Scheltema et al in press...Kafanov (ed.), Hydrobiological research of bays and inlets of Primorye. Far East Science Center, USSR Acad. Sci. Vladivostok Morse, M.P. (1979). Meiomenia

Quantifying Slope Effects and Variations in Crater Density across a Single Geologic Unit

NASA Astrophysics Data System (ADS)

Meyer, Heather; Mahanti, Prasun; Robinson, Mark; Povilaitis, Reinhold

2016-10-01

Steep underlying slopes (>~5°) significantly increase the rate of degradation of craters [1-3]. As a result, the density of craters is less on steeper slopes for terrains of the same age [2, 4]. Thus, when age-dating a planetary surface, an area encompassing one geologic unit of constant low slope is chosen. However, many key geologic units, such as ejecta blankets, lack sufficient area of constant slope to derive robust age estimates. Therefore, accurate age-dating of such units requires an accurate understanding of the effects of slope on age estimates. This work seeks to determine if the observed trend of decreasing crater density with increasing slopes [2] holds for craters >1 km and to quantify the effect of slope for craters of this size, focusing on the effect of slopes over the kilometer scale. Our study focuses on the continuous ejecta of Orientale basin, where we measure craters >1 km excluding secondaries that occur as chains or clusters. Age-dating via crater density measurements relies on uniform cratering across a single geologic unit. In the case of ejecta blankets and other impact related surfaces, this assumption may not hold due to the formation of auto- secondary craters. As such, we use LRO WAC mosaics [5], crater size-frequency distributions, absolute age estimates, a 3 km slope map derived from the WAC GLD100 [6], and density maps for various crater size ranges to look for evidence of non-uniform cratering across the continuous ejecta of Orientale and to determine the effect of slope on crater density. Preliminary results suggest that crater density does decrease with increasing slope for craters >1 km in diameter though at a slower rate than for smaller craters.References: [1] Trask N. J. and Rowan L. C. (1967) Science 158, 1529-1535. [2] Basilevsky (1976) Proc. Lunar Sci. Conf. 7th, p. 1005-1020. [3] Pohn and Offield (1970) USGS Prof. Pap., 153-162. [4] Xiao et al. (2013) Earth and Planet. Sci. Lett., 376, pgs. 1-11. doi:10.1016/j.epsl.2013.06.015. [5] Robinson M. S. et al. (2010) Space Sci. Rev. 150, 81 -124. [6] Scholten F. et al. (2011), JGR, 117, doi:10.1029/2011JE003926

Sci-Hub provides access to nearly all scholarly literature.

PubMed

Himmelstein, Daniel S; Romero, Ariel Rodriguez; Levernier, Jacob G; Munro, Thomas Anthony; McLaughlin, Stephen Reid; Greshake Tzovaras, Bastian; Greene, Casey S

2018-03-01

The website Sci-Hub enables users to download PDF versions of scholarly articles, including many articles that are paywalled at their journal's site. Sci-Hub has grown rapidly since its creation in 2011, but the extent of its coverage has been unclear. Here we report that, as of March 2017, Sci-Hub's database contains 68.9% of the 81.6 million scholarly articles registered with Crossref and 85.1% of articles published in toll access journals. We find that coverage varies by discipline and publisher, and that Sci-Hub preferentially covers popular, paywalled content. For toll access articles, we find that Sci-Hub provides greater coverage than the University of Pennsylvania, a major research university in the United States. Green open access to toll access articles via licit services, on the other hand, remains quite limited. Our interactive browser at https://greenelab.github.io/scihub allows users to explore these findings in more detail. For the first time, nearly all scholarly literature is available gratis to anyone with an Internet connection, suggesting the toll access business model may become unsustainable. © 2018, Himmelstein et al.

Infusing Authentic Inquiry into Biotechnology

NASA Astrophysics Data System (ADS)

Hanegan, Nikki L.; Bigler, Amber

2009-10-01

Societal benefit depends on the general public's understandings of biotechnology (Betsch in World J Microbiol Biotechnol 12:439-443, 1996; Dawson and Cowan in Int J Sci Educ 25(1):57-69, 2003; Schiller in Business Review: Federal Reserve Bank of Philadelphia (Fourth Quarter), 2002; Smith and Emmeluth in Am Biol Teach 64(2):93-99, 2002). A National Science Foundation funded survey of high school biology teachers reported that hands-on biotechnology education exists in advanced high school biology in the United States, but is non-existent in mainstream biology coursework (Micklos et al. in Biotechnology labs in American high schools, 1998). The majority of pre-service teacher content preparation courses do not teach students appropriate content knowledge through the process of inquiry. A broad continuum exists when discussing inquiry-oriented student investigations (Hanegan et al. in School Sci Math J 109(2):110-134, 2009). Depending on the amount of structure in teacher lessons, inquiries can often be categorized as guided or open. The lesson can be further categorized as simple or authentic (Chinn and Malhotra in Sci Educ 86(2):175-218, 2002). Although authentic inquiries provide the best opportunities for cognitive development and scientific reasoning, guided and simple inquiries are more often employed in the classroom (Crawford in J Res Sci Teach 37(9):916-937, 2000; NRC in Inquiry and the national science education standards: a guide for teaching and learning, 2000). For the purposes of this study we defined inquiry as "authentic" if original research problems were resolved (Hanegan et al. in School Sci Math J 109(2):110-134, 2009; Chinn and Malhotra in Sci Educ 86(2):175-218, 2002; Roth in Authentic school science: knowing and learning in open-inquiry science laboratories, 1995). The research question to guide this study through naturalistic inquiry research methods was: How will participants express whether or not an authentic inquiry experience enhanced their understanding of biotechnology? As respondents explored numerous ideas in order to develop a workable research question, struggled to create a viable protocol, executed their experiment, and then evaluated their results, they commented on unexpected topics regarding the nature of science as well as specific content knowledge relating to their experiments. Four out of five participants reported they learned the most during authentic inquiry laboratory experience.

Information Processing, Specificity of Practice, and the Transfer of Learning: Considerations for Reconsidering Fidelity

ERIC Educational Resources Information Center

Grierson, Lawrence E. M.

2014-01-01

Much has been made in the recent medical education literature of the incorrect characterization of simulation along a continuum of low to high fidelity (Cook et al. "JAMA" 306(9): 978-988, 2011; Norman et al. "Med Educ" 46(7): 636-647, 2012; Teteris et al. "Adv Health Sci Educ" 17(1): 137-144, 2012). For the most…

Reply to comments by Ahmad et al. on: Shah, A. A., 2013. Earthquake geology of Kashmir Basin and its implications for future large earthquakes International Journal of Earth Sciences DOI:10.1007/s00531-013-0874-8 and on Shah, A. A., 2015. Kashmir Basin Fault and its tectonic significance in NW Himalaya, Jammu and Kashmir, India, International Journal of Earth Sciences DOI:10.1007/s00531-015-1183-1

NASA Astrophysics Data System (ADS)

Shah, A. A.

2016-03-01

Shah (Int J Earth Sci 102:1957-1966, 2013) mapped major unknown faults and fault segments in Kashmir basin using geomorphological techniques. The major trace of out-of-sequence thrust fault was named as Kashmir basin fault (KBF) because it runs through the middle of Kashmir basin, and the active movement on it has backtilted and uplifted most of the basin. Ahmad et al. (Int J Earth Sci, 2015) have disputed the existence of KBF and maintained that faults identified by Shah (Int J Earth Sci 102:1957-1966, 2013) were already mapped as inferred faults by earlier workers. The early works, however, show a major normal fault, or a minor out-of-sequence reverse fault, and none have shown a major thrust fault.

Exploring a Model of Situated Professional Development: Impact on Classroom Practice

NASA Astrophysics Data System (ADS)

Singer, Jonathan; Lotter, Christine; Feller, Robert; Gates, Harry

2011-04-01

A hallmark of current science education reform involves teaching through inquiry. However, the widespread use of inquiry-based instruction in many classrooms has not occurred (Roehrig and Luft in Int J Sci Educ 26:3-24, 2004; Schneider et al. in J Res Sci Teach 42:283-312, 2005). The purpose of this study was to investigate the impact of a professional development program on middle school science teachers' ability to enact inquiry-based pedagogical practices. Data were generated through evaluation of teacher practice using the Reformed Teaching Observation Protocol (RTOP) (Sawada et al. in School Sci Math 102:245-253, 2002) at three distinct junctures, before, during, and after the professional development treatment. Analysis of teacher-participant post-institute reflections was then utilized to determine the perceived role of the various institute components. Statistical significant changes in RTOP scores indicated that the teachers were able to successfully transfer the enactment of the inquiry-based practices into their classrooms. The subsequent discussion provides connection between these pedagogical changes with use of professional development strategies that provide a situated learning environment.

KENNEDY SPACE CENTER, FLA. - The SciSat-1 spacecraft is uncrated at Vandenberg Air Force Base, Calif. SciSat-1 weighs approximately 330 pounds and will be placed in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

NASA Image and Video Library

2003-06-26

KENNEDY SPACE CENTER, FLA. - The SciSat-1 spacecraft is uncrated at Vandenberg Air Force Base, Calif. SciSat-1 weighs approximately 330 pounds and will be placed in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

KENNEDY SPACE CENTER, FLA. - The SciSat-1 spacecraft is revealed after being uncrated at Vandenberg Air Force Base, Calif. SciSat-1 weighs approximately 330 pounds and will be placed in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

NASA Image and Video Library

2003-06-26

KENNEDY SPACE CENTER, FLA. - The SciSat-1 spacecraft is revealed after being uncrated at Vandenberg Air Force Base, Calif. SciSat-1 weighs approximately 330 pounds and will be placed in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

KENNEDY SPACE CENTER, FLA. - Workers at Vandenberg Air Force Base, Calif., prepare to move the SciSat-1 spacecraft. SciSat-1 weighs approximately 330 pounds and will be placed in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

NASA Image and Video Library

2003-06-26

KENNEDY SPACE CENTER, FLA. - Workers at Vandenberg Air Force Base, Calif., prepare to move the SciSat-1 spacecraft. SciSat-1 weighs approximately 330 pounds and will be placed in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

Accessing the Asymmetric Collisionless Reconnection Regime in the Terrestrial Reconnection Experiment (TREX)

NASA Astrophysics Data System (ADS)

Greess, S.; Egedal, J.; Olson, J.; Millet-Ayala, A.; Myers, R.; Wallace, J.; Clark, M.; Forest, C.

2017-12-01

Kinetic effects are expected to dominate the collisionless reconnection regime, where the mean free path is large enough that the anisotropic electron pressure can develop without being damped away by collisional pitch angle scattering. In simulations, the anisotropic pressure drives the formation of outflow jets [1]. These jets are expected to play a role in the reconnection layer at the Earth's magnetopause, which is currently being explored by Magnetospheric Multiscale Mission (MMS) [2]. Until recently, this regime of anisotropic pressure was inaccessible by laboratory experiments, but new data from the Terrestrial Reconnection Experiment (TREX) shows that fully collisionless reconnection can now be achieved in the laboratory. Future runs at TREX will delve deeper into this collisionless regime in both the antiparallel and guide-field cases. [1] Le, A. et al. JPP, 81(1). doi: 10.1017/S0022377814000907. [2] Burch, J. L. et al. Space Sci. Rev. 199,5. doi: 10.1007/s11214-015-0164-9 Supported in part by NSF/DOE award DE-SC0013032.

Laser-driven, magnetized quasi-perpendicular collisionless shocks on the Large Plasma Device

DOE Office of Scientific and Technical Information (OSTI.GOV)

Schaeffer, D. B., E-mail: dschaeffer@physics.ucla.edu; Everson, E. T.; Bondarenko, A. S.

2014-05-15

The interaction of a laser-driven super-Alfvénic magnetic piston with a large, preformed magnetized ambient plasma has been studied by utilizing a unique experimental platform that couples the Raptor kJ-class laser system [Niemann et al., J. Instrum. 7, P03010 (2012)] to the Large Plasma Device [Gekelman et al., Rev. Sci. Instrum. 62, 2875 (1991)] at the University of California, Los Angeles. This platform provides experimental conditions of relevance to space and astrophysical magnetic collisionless shocks and, in particular, allows a detailed study of the microphysics of shock formation, including piston-ambient ion collisionless coupling. An overview of the platform and its capabilitiesmore » is given, and recent experimental results on the coupling of energy between piston and ambient ions and the formation of collisionless shocks are presented and compared to theoretical and computational work. In particular, a magnetosonic pulse consistent with a low-Mach number collisionless shock is observed in a quasi-perpendicular geometry in both experiments and simulations.« less

Involvement and Regulation of Heparanase in Prostate Cancer Progression

DTIC Science & Technology

2007-02-01

1995). On the other hand, some promoters are negatively regulated by wt p53. These include MMP-1 (Sun et al., 1999), alpha - fetoprotein (Lee et al...necrosis factor alpha is formed from the extracellular matrix by the enzyme heparanase. Proc Natl Acad Sci U S A. 1995;92: 5037-5041. 29. Zcharia E

Observing terrestrial water storage and land-atmosphere dynamics from space: Implications for forecasting and climate projections

NASA Astrophysics Data System (ADS)

Seneviratne, S. I.; Humphrey, V.; Nicolai-Shaw, N.; Gudmundsson, L.; Guillod, B.; Hirschi, M.; Michel, D.; Orth, R.; Zscheischler, J.

2016-12-01

In recent years, several new satellite products have been derived which allow an unprecendented assessment of terrestrial water storage and land-atmosphere dynamics. This presentation will review some of these new developments, with a focus on drought dynamics, plant-water interactions, and soil moisture-atmosphere feedbacks. Results derived based on the Gravity Recovery and Climate Experiment (GRACE, Humphrey et al. 2016) and the European Space Agency Climate Change Initiative (ESA CCI) Soil Moisture dataset (Nicolai-Shaw et al. 2015, 2016; Hirschi et al. 2014) will be highlighted, as well as assessments using satellite-based estimates of evapotranspiration (Mueller and Seneviratne 2014, Michel et al. 2016), vegetation activity (Zscheischler et al. 2015), and combined soil moisture and precipitation analyses (Guillod et al. 2015). These findings provide new insights on the development of prediction capabilities for droughts, precipitation events, and heat waves, and the reduction of uncertainties in climate model projections. References: Guillod, B.P., B. Orlowsky, D.G. Miralles, A.J. Teuling, and S.I. Seneviratne, 2015. Nature Communications, 6:6443, DOI: 10.1038/ncomms7443 Hirschi, M., B. Mueller, W. Dorigo, and S.I. Seneviratne, 2014. Remote Sensing of Environment, 154, 246-252. Humphrey, V., L. Gudmundsson, and S.I. Seneviratne, 2016. Surv. Geophysics, 37, 357-395, DOI 10.1007/s10712-016-9367-1. Michel, D., et al. 2016. Hydrol. Earth Syst. Sci. 20, 803-822, doi:10.5194/hess-20-803-2016. Mueller, M., and S.I. Seneviratne, 2014. Geophys. Res. Lett., 41, 1-7, doi:10.1002/2013GL058055. Nicolai-Shaw, N., L. Gudmundsson, M. Hirschi, and S.I. Seneviratne, 2016. Geophys. Res. Lett., in review. Nicolai-Shaw, N., M. Hirschi, H. Mittelbach, and S.I. Seneviratne, 2015. Journal of Geophysical Research, 120, doi:10.1002/2015JD023305. Zscheischler, J., R. Orth, and S.I. Seneviratne, 2015. Geophys. Res. Lett., 42, 9816-9824, doi:10.1002/2015GL066563.

Mantle Mineral/Silicate Melt Partitioning

NASA Astrophysics Data System (ADS)

McFarlane, E. A.; Drake, M. J.

1992-07-01

Introduction: The partitioning of elements among mantle phases and silicate melts is of interest in unraveling the early thermal history of the Earth. It has been proposed that the elevated Mg/Si ratio of the upper mantle of the Earth is a consequence of the flotation of olivine into the upper mantle (Agee and Walker, 1988). Agee and Walker (1988) have generated a model via mass balance by assuming average mineral compositions to generate upper mantle peridotite. This model determines that upper mantle peridotite could result from the addition of 32.7% olivine and 0.9% majorite garnet into the upper mantle, and subtraction of 27.6% perovskite from the upper mantle (Agee and Walker, 1988). The present contribution uses experimental data to examine the consequences of such multiple phase fractionations enabling an independent evaluation of the above mentioned model. Here we use Mg-perovskite/melt partition coefficients from both a synthetic and a natural system (KLB-1) obtained from this laboratory. Also used are partition coefficient values for majorite garnet/melt, beta spinel/melt and olivine/melt partitioning (McFarlane et al., 1991b; McFarlane et al., 1992). Multiple phase fractionations are examined using the equilibrium crystallization equation and partition coefficient values. The mineral proportions determined by Agee and Walker (1988) are converted into weight fractions and used to compute a bulk partition coefficient value. Discussion: There has been a significant debate concerning whether measured values of trace element partition coefficients permit large-scale fractionation of liquidus phases from an early terrestrial magma ocean (Kato et al., 1988a,b; Walker and Agee, 1989; Drake, 1989; Drake et al., 1991; McFarlane et al., 1990, 1991). It should be noted that it is unclear which, if any, numerical values of partition coefficients are appropriate for examining this question, and certainly the assumptions for the current model must be more fully examined. However, our preliminary calculations do not appear to be consistent with large scale fractionation of phases in the proportions postulated from an early ocean, because approximately chondritic ratios and abundances of refractory lithophile elements inferred for the primitive upper mantle of the Earth would not be preserved. References: Agee, C.B. and Walker, D. (1988) Earth. Planet. Sci. Lett. 90, 144-156. Drake, M.J. (1989) Z. Naturforsch., 44a, 883-890. Drake, M.J. et al. (1991) Magma Oceans Workshop. Drake, M.J. et al. (1989) Geochim. Cosmochim. Acta, 53, 2101-2111. Kato, T. et al. (1988a) Earth. Planet. Sci. Lett. 89, 123-145. Kato, T. et al. (1988b) Earth. Planet. Sci. Lett. 90, 65-68. McFarlane, E.A. et al. (1990) Lunar and Planetary Science 21, 759-760. McFarlane, E.A. et al. (199la) Magma Oceans Workshop. McFarlane, E.A. et al. (199lb) Lunar and Planetary Science 22, 875-876. McFarlane, E.A. et al. (1992) Lunar and Planetary Science 23, 883-884. Walker, D. and Agee, C.B. (1989) Earth. Planet. Sci. Lett. 96, 49-60.

Spectroscopic imaging of limiter heat and particle fluxes and the resulting impurity sources during Wendelstein 7-X startup plasmas

DOE PAGES

Stephey, L.; Wurden, G. A.; Schmitz, O.; ...

2016-08-08

A combined IR and visible camera system [G. A. Wurden et al., “A high resolution IR/visible imaging system for the W7-X limiter,” Rev. Sci. Instrum. (these proceedings)] and a filterscope system [R. J. Colchin et al., Rev. Sci. Instrum. 74, 2068 (2003)] were implemented together to obtain spectroscopic data of limiter and first wall recycling and impurity sources during Wendelstein 7-X startup plasmas. Both systems together provided excellent temporal and spatial spectroscopic resolution of limiter 3. Narrowband interference filters in front of the camera yielded C-III and Hα photon flux, and the filterscope system provided H α, H β, He-I,more » He-II, C-II, and visible bremsstrahlung data. The filterscopes made additional measurements of several points on the W7-X vacuum vessel to yield wall recycling fluxes. Finally, the resulting photon flux from both the visible camera and filterscopes can then be compared to an EMC3-EIRENE synthetic diagnostic [H. Frerichs et al., “Synthetic plasma edge diagnostics for EMC3-EIRENE, highlighted for Wendelstein 7-X,” Rev. Sci. Instrum. (these proceedings)] to infer both a limiter particle flux and wall particle flux, both of which will ultimately be used to infer the complete particle balance and particle confinement time τ P.« less

Homozygous Expression of Mutant ELOVL4 Leads to Seizures and Death in a Novel Animal Model of Very Long-Chain Fatty Acid Deficiency.

PubMed

Hopiavuori, Blake R; Deák, Ferenc; Wilkerson, Joseph L; Brush, Richard S; Rocha-Hopiavuori, Nicole A; Hopiavuori, Austin R; Ozan, Kathryn G; Sullivan, Michael T; Wren, Jonathan D; Georgescu, Constantin; Szweda, Luke; Awasthi, Vibhudutta; Towner, Rheal; Sherry, David M; Anderson, Robert E; Agbaga, Martin-Paul

2018-02-01

Lipids are essential components of the nervous system. However, the functions of very long-chain fatty acids (VLC-FA; ≥ 28 carbons) in the brain are unknown. The enzyme ELOngation of Very Long-chain fatty acids-4 (ELOVL4) catalyzes the rate-limiting step in the biosynthesis of VLC-FA (Agbaga et al., Proc Natl Acad Sci USA 105(35): 12843-12848, 2008; Logan et al., J Lipid Res 55(4): 698-708, 2014), which we identified in the brain as saturated fatty acids (VLC-SFA). Homozygous mutations in ELOVL4 cause severe neuropathology in humans (Ozaki et al., JAMA Neurol 72(7): 797-805, 2015; Mir et al., BMC Med Genet 15: 25, 2014; Cadieux-Dion et al., JAMA Neurol 71(4): 470-475, 2014; Bourassa et al., JAMA Neurol 72(8): 942-943, 2015; Aldahmesh et al., Am J Hum Genet 89(6): 745-750, 2011) and are post-natal lethal in mice (Cameron et al., Int J Biol Sci 3(2): 111-119, 2007; Li et al., Int J Biol Sci 3(2): 120-128, 2007; McMahon et al., Molecular Vision 13: 258-272, 2007; Vasireddy et al., Hum Mol Genet 16(5): 471-482, 2007) from dehydration due to loss of VLC-SFA that comprise the skin permeability barrier. Double transgenic mice with homozygous knock-in of the Stargardt-like macular dystrophy (STDG3; 797-801_AACTT) mutation of Elovl4 with skin-specific rescue of wild-type Elovl4 expression (S + Elovl4 mut/mut mice) develop seizures by P19 and die by P21. Electrophysiological analyses of hippocampal slices showed aberrant epileptogenic activity in S + Elovl4 mut/mut mice. FM1-43 dye release studies showed that synapses made by cultured hippocampal neurons from S + Elovl4 mut/mut mice exhibited accelerated synaptic release kinetics. Supplementation of VLC-SFA to cultured hippocampal neurons from mutant mice rescued defective synaptic release to wild-type rates. Together, these studies establish a critical, novel role for ELOVL4 and its VLC-SFA products in regulating synaptic release kinetics and epileptogenesis. Future studies aimed at understanding the molecular mechanisms by which VLC-SFA regulate synaptic function may provide new targets for improved seizure therapies.

Precision measurements with atom interferometry

NASA Astrophysics Data System (ADS)

Schubert, Christian; Abend, Sven; Schlippert, Dennis; Ertmer, Wolfgang; Rasel, Ernst M.

2017-04-01

Interferometry with matter waves enables precise measurements of rotations, accelerations, and differential accelerations [1-5]. This is exploited for determining fundamental constants [2], in fundamental science as e.g. testing the universality of free fall [3], and is applied for gravimetry [4], and gravity gradiometry [2,5]. At the Institut für Quantenoptik in Hannover, different approaches are pursued. A large scale device is designed and currently being set up to investigate the gain in precision for gravimetry, gradiometry, and fundamental tests on large baselines [6]. For field applications, a compact and transportable device is being developed. Its key feature is an atom chip source providing a collimated high flux of atoms which is expected to mitigate systematic uncertainties [7,8]. The atom chip technology and miniaturization benefits from microgravity experiments in the drop tower in Bremen and sounding rocket experiments [8,9] which act as pathfinders for space borne operation [10]. This contribution will report about our recent results. The presented work is supported by the CRC 1227 DQ-mat, the CRC 1128 geo-Q, the RTG 1729, the QUEST-LFS, and by the German Space Agency (DLR) with funds provided by the Federal Ministry of Economic Affairs and Energy (BMWi) due to an enactment of the German Bundestag under Grant No. DLR 50WM1552-1557. [1] P. Berg et al., Phys. Rev. Lett., 114, 063002, 2015; I. Dutta et al., Phys. Rev. Lett., 116, 183003, 2016. [2] J. B. Fixler et al., Science 315, 74 (2007); G. Rosi et al., Nature 510, 518, 2014. [3] D. Schlippert et al., Phys. Rev. Lett., 112, 203002, 2014. [4] A. Peters et al., Nature 400, 849, 1999; A. Louchet-Chauvet et al., New J. Phys. 13, 065026, 2011; C. Freier et al., J. of Phys.: Conf. Series 723, 012050, 2016. [5] J. M. McGuirk et al., Phys. Rev. A 65, 033608, 2002; P. Asenbaum et al., arXiv:1610.03832. [6] J. Hartwig et al., New J. Phys. 17, 035011, 2015. [7] H. Ahlers et al., Phys. Rev. Lett. 116, 173601, 2016; S. Abend et al., Phys. Rev. Lett. 117, 203003, 2016. [8] J. Rudolph et al., New J. Phys. 17, 065001, 2015. [9] H. Müntinga et al., Phys. Rev. Lett., 110, 093602, 2013. [10] O. Carraz et al., Microgravity Sci. Technol. 26, 139, 2014; D. Aguilera et al., Class. Quantum Grav. 31, 115010, 2014.

The PHITS code for space applications: status and recent developments

NASA Astrophysics Data System (ADS)

Sihver, Lembit; Ploc, Ondrej; Sato, Tatsuhiko; Niita, Koji; Hashimoto, Shintaro; El-Jaby, Samy

Since COSPAR 2012, the Particle and Heavy Ion Transport code System, PHITS, has been upgraded and released to the public [1]. The code has been improved and so has the contents of its package, such as the attached data libraries. In the new version, the intra-nuclear cascade models INCL4.6 and INC-ELF have been implemented as well as the Kurotama model for the total reaction cross sections. The accuracies of the new reaction models for transporting the galactic cosmic-rays were investigated by comparing with experimental data. The incorporation of these models has improved the capabilities of PHITS to perform particle transport simulations for different space applications. A methodology for assessing the pre-mission exposure of space crew aboard the ISS has been developed in terms of an effective dose equivalent [2]. PHITS was used to calculate the particle transport of the GCR and trapped radiation through the hull of the ISS. By using the predicted spectra, and fluence-to-dose conversion factors, the semi-empirical ISSCREM [3,4,5] code was then scaled to predict the effective dose equivalent. This methodology provides an opportunity for pre-flight predictions of the effective dose equivalent, which can be compared to post-flight estimates, and therefore offers a means to assess the impact of radiation exposure on ISS flight crew. We have also simulated [6] the protective curtain experiment, which was performed to test the efficiency of water-soaked hygienic tissue wipes and towels as a simple and cost-effective additional spacecraft shielding. The dose from the trapped particles and low energetic GCR, was significantly reduced, which shows that the protective curtains are efficient when they are applied on spacecraft at LEO. The results of these benchmark calculations, as well as the mentioned applications of PHITS to space dosimetry, will be presented. [1] T. Sato et al. J. Nucl. Sci. Technol. 50, 913-923 (2013). [2] S. El-Jaby, et al. Adv. Space Res. doi: http://dx.doi.org/10.1016/j.asr.2013.12.022 (2013). [3] S. El-Jaby, et al. Adv. Space Res. doi: http://dx.doi.org/10.1016/j.asr.2013.10.006 (2013). [4] S. El-Jaby, et al. In proc. to the IEEE Aerospace Conference, Big Sky, MN, USA (2013). [5] S. El-Jaby, PhD Thesis, Royal Military College of Canada (2012). [6] O. Ploc, et al., Adv. Space Res. 52, 1911-1918 (2013).

Effect of the presence of chlorates and perchlorates on the pyrolysis of organic compounds: implications for measurements done with the SAM experiment onboard the Curiosity rover

NASA Astrophysics Data System (ADS)

Millan, Maeva; Szopa, Cyril; Buch, Arnaud; Belmahdi, Imène; Coll, Patrice; Glavin, Daniel P.; Freissinet, Caroline; Archer, Doug; Sutter, Brad; Summons, Roger E.; Navarro-Gonzalez, Rafael; Cabane, Michel; Mahaffy, Paul

2016-04-01

The Sample Analysis at Mars (SAM) experiment onboard the Curiosity rover of the Mars Science Laboratory mission is partly devoted to the in situ molecular analysis of gases evolving from solid samples collected on Mars surface/sub-surface. SAM has a gas-chromatograph coupled to a quadrupole mass spectrometer (GC-QMS) devoted to the separation and identification of organic and inorganic material [1]. Before proceeding to the GC-QMS analysis, the solid sample collected by Curiosity is subjected to a thermal treatment thanks to the pyrolysis oven to release the volatiles into the gas processing system. As the Viking landers in 1976 [2], SAM detected chlorohydrocarbons with the pyrolysis GC-QMS experiment [3,4]. The detection of perchlorates salts in soil at the Phoenix Landing site [6] suggests that these chlorohydrocarbons could come from the reaction of organics with oxychlorines. Oxychlorines indeed decomposed into molecular oxygen and volatile chlorine when heated and react with the organic matter in the samples by oxidation and/or chlorination processes. [3,5,7,8]. During SAM pyrolysis, samples are heated to 850°C. SAM detected C1 to C3 chloroalkanes, entirely attributed to reaction products occurring during the pyrolysis experiment between oxychlorines and organic carbon from instrument background [3] and chlorobenzene and C2 to C4 dichloroalkanes produced by reaction between Mars endogenous organics with oxychlorines [4]. To help understanding the influence of perchlorate and chlorate salts on organic matter during SAM pyrolysis, we systemically study the reaction products formed during pyrolysis of various organic compounds mixed with various perchlorates and chlorates. We selected organics from simple molecule forms as for instance PAHs and amino acids to complex material (>30 carbon atoms) such as kerogen. The perchlorate and chlorate salts are prepared at 1 wt % concentration in silica and mixed with the organics to study the potential qualitative and/or quantitative effects. The experiments are performed on a laboratory GC-QMS with a Restek Rxi-5 column (30m x 0.25mm x 0.25μm) and an Intersciences pyrolyser. The mixture is pyrolyzed at different temperatures up to 900°C to cover the SAM temperature range. Different experiments are done to discriminate the pyrolysis products directly coming from the organics, and those produced from the reaction with oxychlorine. These experiments are under progress and should bring key information on the potential to identify Martian organics when pyrolyzing solid samples. Depending on the organic families studied, we may find recurring molecules, which are potentially present in Mars' surface samples. This work could thus highlight some organic precursors of the chlorinated compounds found on Mars, and support the interpretation of SAM measurements. References: [1] Mahaffy, P. et al. (2012) Space Sci Rev, 170, 401-478. [2] Biemann, K. et al (1977) JGR, 82, 4641-4658. [3] Glavin, D. et al. (2013), JGR 118, 1955-1973. [4] Freissinet, C. et al. (2015) JGR. [5] Leshin L. et al. (2013), Science. [6] Hecht, (2009), Science, 325 64-67. [7] Navarro-Gonzalez et al. (2010) JGR 115, EI12010. [8] Steninger, H. et al (2012) Planet. Space Sci. 71, 9-17. Acknowledgments: French Space Agency (CNES) support for SAM-GC development and exploitation.

Numerical modelling of volatiles in the deep mantle

NASA Astrophysics Data System (ADS)

Eichheimer, Philipp; Thielmann, Marcel; Golabek, Gregor J.

2017-04-01

The transport and storage of water in the mantle significantly affects several material properties of mantle rocks and thus water plays a key role in a variety of geodynamical processes (tectonics, magmatism etc.). The processes driving transport and circulation of H2O in subduction zones remain a debated topic. Geological and seismological observations suggest different inflow mechanisms of water e.g. slab bending, thermal cracking and serpentinization (Faccenda et al., 2009; Korenaga, 2017), followed by dehydration of the slab. On Earth both shallow and steep subduction can be observed (Li et al., 2011). However most previous models (van Keken et al., 2008; Wilson et al., 2014) did not take different dip angles and subduction velocities of slabs into account. To which extent these parameters and processes influence the inflow of water still remains unclear. We present 2D numerical models simulating the influence of the various water inflow mechanisms on the mantle with changing dip angle and subduction velocity of the slab over time. The results are used to make predictions regarding the rheological behavior of the mantle wedge, dehydration regimes and volcanism at the surface. References: van Keken, P. E., et al. A community benchmark for subduction zone modeling. Phys. Earth Planet. Int. 171, 187-197 (2008). Faccenda, M., T.V. Gerya, and L. Burlini. Deep slab hydration induced by bending-related variations in tectonic pressure. Nat. Geosci. 2, 790-793 (2009). Korenaga, J. On the extent of mantle hydration caused by plate bending. Earth Planet. Sci. Lett. 457, 1-9 (2017). Wilson, C. R., et al. Fluid flow in subduction zones: The role of solid rheology and compaction pressure. Earth Planet. Sci. Lett. 401, 261-274 (2014). Li, Z. H., Z. Q. Xu, and T. V. Gerya. Flat versus steep subduction: Contrasting modes for the formation and exhumation of high- to ultrahigh-pressure rocks in continental collision zones. Earth Planet. Sci. Lett. 301, 65-77 (2011).

SciBox, an end-to-end automated science planning and commanding system

NASA Astrophysics Data System (ADS)

Choo, Teck H.; Murchie, Scott L.; Bedini, Peter D.; Steele, R. Josh; Skura, Joseph P.; Nguyen, Lillian; Nair, Hari; Lucks, Michael; Berman, Alice F.; McGovern, James A.; Turner, F. Scott

2014-01-01

SciBox is a new technology for planning and commanding science operations for Earth-orbital and planetary space missions. It has been incrementally developed since 2001 and demonstrated on several spaceflight projects. The technology has matured to the point that it is now being used to plan and command all orbital science operations for the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission to Mercury. SciBox encompasses the derivation of observing sequences from science objectives, the scheduling of those sequences, the generation of spacecraft and instrument commands, and the validation of those commands prior to uploading to the spacecraft. Although the process is automated, science and observing requirements are incorporated at each step by a series of rules and parameters to optimize observing opportunities, which are tested and validated through simulation and review. Except for limited special operations and tests, there is no manual scheduling of observations or construction of command sequences. SciBox reduces the lead time for operations planning by shortening the time-consuming coordination process, reduces cost by automating the labor-intensive processes of human-in-the-loop adjudication of observing priorities, reduces operations risk by systematically checking constraints, and maximizes science return by fully evaluating the trade space of observing opportunities to meet MESSENGER science priorities within spacecraft recorder, downlink, scheduling, and orbital-geometry constraints.

Evidence for Adsorbate-Enhanced Field Emission from Carbon Nanotube Fibers (Postprint)

DTIC Science & Technology

2013-07-31

information if it does not display a currently valid OMB control number. PLEASE DO NOT RETURN YOUR FORM TO THE ABOVE ADDRESS. 1. REPORT DATE (DD-MM...indi- cate no detectable change in partial pressure of either species during FE within regime I. However, the data do exhibit a threshold for...Thien Binh , et al., J. Vac. Sci. Techno!. B 21, 693 (2003). 3B. Diop and Vu Thien Binh , Rev. Sci . Instrum. 83, 094704 (2012). 4J. Zhang, G. Yang, Y

Poly (acrylonitrile - co -1-vinylimidazole): A New Melt Processable Carbon Fiber Precursor

DTIC Science & Technology

2011-01-01

changed fromwhite to brown and then black during stabilization as expected. The stabi- lized black copolymers were insoluble in DMF, showing good...Paliwal DK, Bajaj P. J Appl Polym Sci 1996;59:1819. [9] Bhanu VA, Rangarajan P, Wiles K, Bortner M, Sankarpandian M, Godshall D, et al. Polymer 2002;43:4841...AA. Carbon 2005;43:1065e72. [23] Bajaj P, Roopanwal AK. J Macromol Sci Rev Macromol Chem Phys 1997;C37:97. [24] Mukundan T, Bhanu VA, Wiles KB, Johnson

26Al-26Mg systematics in chondrules from Kaba and Yamato 980145 CV3 carbonaceous chondrites

NASA Astrophysics Data System (ADS)

Nagashima, Kazuhide; Krot, Alexander N.; Komatsu, Mutsumi

2017-03-01

We report the mineralogy, petrography, and in situ measured 26Al-26Mg systematics in chondrules from the least metamorphosed CV3 (Vigarano-type) chondrites, Kaba and Yamato (Y) 980145. Two Y 980145 chondrules measured show no resolvable excesses in 26Mg (26Mg∗), a decay product of a short-lived (t1/2 ∼0.7 Ma) radionuclide 26Al. Plagioclase in one of the chondrules is replaced by nepheline, indicative of thermal metamorphism. The lack of 26Mg∗ in the Y 980145 chondrules is most likely due to disturbance of their 26Al-26Mg systematics during the metamorphism. Although Kaba experienced extensive metasomatic alteration (<300 °C), it largely avoided subsequent thermal metamorphism, and the 26Al-26Mg systematics of its chondrules appear to be undisturbed. All eight Kaba chondrules measured show 26Mg∗, corresponding to the initial 26Al/27Al ratios [(26Al/27Al)0] ranging from (2.9 ± 1.7) × 10-6 to (6.3 ± 2.7) × 10-6. If CV parent asteroid accreted rapidly after chondrule formation, the inferred (26Al/27Al)0 ratios in Kaba chondrules provide an upper limit on 26Al available in this asteroid at the time of its accretion. The estimated initial abundance of 26Al in the CV asteroid is too low to melt it and contradicts the existence of a molten core in this body suggested from the paleomagnetic records of Allende [Carporzen et al. (2011) Magnetic evidence for a partially differentiated carbonaceous chondrite parent body. Proc. Natl. Acad. Sci. USA108, 6386-6389] and Kaba [Gattacceca et al. (2013) More evidence for a partially differentiated CV parent body from the meteorite Kaba. Lunar Planet. Sci.44, abstract#1721].

Mutation of Breast Cancer Cell Genomic DNA by APOBEC3B

DTIC Science & Technology

2013-09-01

lethal prostate cancers. Proc. Natl Acad. Sci. USA 108, 17087–17092 (2011). 5. Parsons, D. W. et al. The genetic landscape of the childhood cancer...7. Stransky, N. et al. The mutational landscape of head and neck squamous cell carcinoma. Science 333, 1157–1160 (2011). 8. Nik-Zainal, S. et al...Mutational processes molding the genomes of 21 breast cancers. Cell 149, 979–993 (2012). 9. Stephens, P. J. et al. The landscape of cancer genes and

Stable two-plane focusing for emittance-dominated sheet-beam transport

NASA Astrophysics Data System (ADS)

Carlsten, B. E.; Earley, L. M.; Krawczyk, F. L.; Russell, S. J.; Potter, J. M.; Ferguson, P.; Humphries, S.

2005-06-01

Two-plane focusing of sheet electron beams will be an essential technology for an emerging class of high-power, 100 to 300 GHz rf sources [Carlsten et al., IEEE Trans. Plasma Sci. 33, 85 (2005), ITPSBD, 0093-3813, 10.1109/TPS.2004.841172]. In these devices, the beam has a unique asymmetry in which the transport is emittance dominated in the sheet’s thin dimension and space-charge dominated in the sheet’s wide dimension. Previous work has studied the stability of the transport of beams in the emittance-dominated regime for both wiggler and periodic permanent magnet (PPM) configurations with single-plane focusing, and has found that bigger envelope scalloping occurs for equilibrium transport, as compared to space-charge dominated beams [Carlsten et al., this issue, Phys. Rev. ST Accel. Beams 8, 062001 (2005), PRABFM, 1098-4402]. In this paper, we describe the differences in transport stability when two-plane focusing is included. Two-plane wiggler focusing degrades the transport stability slightly, whereas two-plane PPM focusing greatly compromises the transport. On the other hand, single-plane PPM focusing can be augmented with external quadrupole fields to provide weak focusing in the sheet’s wide dimension, which has stability comparable to two-plane wiggler transport.

Investigation of Shapes and Spins of Reaccumulated Remnants from Asteroid Disruption Simulations

NASA Astrophysics Data System (ADS)

Michel, Patrick; Ballouz, R.; Richardson, D. C.; Schwartz, S. R.

2012-10-01

Evidence that asteroids larger than a few hundred meters diameter can be gravitational aggregates of smaller, cohesive pieces comes, for instance, from images returned by the Hayabusa spacecraft of asteroid 25143 Itokawa (Fujiwara et al., 2006, Science 312, 1330). These images show an irregular 500-meter-long body with a boulder-strewn surface, as might be expected from reaccumulation following catastrophic disruption of a larger parent asteroid (Michel et al., 2001, Science 294, 1696). However, numerical simulations of this process to date essentially focus on the size/mass and velocity distributions of reaccumulated fragments, matching asteroid families. Reaccumulation was simplified by merging the objects into growing spheres. However, understanding shapes, spins and surface properties of gravitational aggregates formed by reaccumulation is required to interpret information from ground-based observations and space missions. E.g., do boulders on Itokawa originate from reaccumulation of material ejected from a catastrophic impact or from other processes (such as the Brazil-nut effect)? How does reaccumulation affect the observed shapes? A model was developed (Richardson et al., 2009, Planet. Space Sci. 57, 183) to preserve shape and spin information of reaccumulated bodies in simulations of asteroid disruption, by allowing fragments to stick on contact (and optionally bounce or fragment further, depending on user-selectable parameters). Such treatments are computationally expensive, and we could only recently start to explore the parameter space. Preliminary results will be presented, showing that some observed surface and shape features may be explained by how fragments produced by a disruption reaccumulate. Simulations of rubble pile collisions without particle cohesion, and an investigation of the influence of initial target rotation on the outcome will also be shown. We acknowledge the National Science Foundation (AST1009579) and NASA (NNX08AM39G).

The Ionosphere Real-Time Assimilative Model, IRTAM - A Status Report

NASA Astrophysics Data System (ADS)

Reinisch, Bodo; Galkin, Ivan; Huang, Xueqin; Vesnin, Artem; Bilitza, Dieter

2014-05-01

Ionospheric models are generally unable to correctly predict the effects of space weather events on the ionosphere. Taking advantage of today's real-time availability of measured electron density profiles of the bottomside ionosphere, we have developed a technique "IRTAM" to specify real-time foF2 and hmF2 global maps. The measured data arrive at the Lowell GIRO Data Center (LGDC) from some ~70 ionosonde stations of the Global Ionosphere Radio Observatory (GIRO) [Reinisch and Galkin, 2011], usually at a 15 min cadence, and are ingested in LGDC's databases (http://ulcar.uml.edu/DIDBase/). We use the International Reference Ionosphere (IRI) electron density model [Bilitza et al., 2011] as the background model. It is an empirical monthly median model that critically depends on the correct values of the F2 layer peak height hmF2 and density NmF2 (or critical frequency foF2). The IRI model uses the so-called CCIR (or URSI) coefficients for the specification of the median foF2 and hmF2 maps. IRTAM assimilates the measured GIRO data in IRI by "adjusting" the CCIR coefficients on-the-fly. The updated maps of foF2 and hmF2 for the last 24 hours before now-time are continuously displayed on http://giro.uml.edu/RTAM [Galkin et al., 2012]. The "adjusted" bottomside profiles can be extended to the topside by using the new Vary-Chap topside profile model [Nsumei et al., 2012] which extends the profile from hmF2 to the plasmasphere. References Bilitza D., L.-A. McKinnell, B. Reinisch, and T. Fuller-Rowell (2011), The International Reference Ionosphere (IRI) today and in the future, J. Geodesy, 85:909-920, DOI 10.1007/s00190-010-0427-x Galkin, I. A., B. W. Reinisch, X. Huang, and D. Bilitza (2012), Assimilation of GIRO Data into a Real-Time IRI, Radio Sci., 47, RS0L07, doi:10.1029/2011RS004952. Nsumei, P., B. W. Reinisch, X. Huang, and D. Bilitza (2012), New Vary-Chap profile of the topside ionosphere electron density distribution for use with the IRI Model and the GIRO real time data, Radio Sci., doi:10.1029/2012RS004989. Reinisch, B. W. and I. A. Galkin (2011), Global Ionospheric Radio Observatory (GIRO), Earth, Planets and Space, 63(4), 377-381.

Studies of Turbulence and Transport in Alcator C-Mod H-Mode Plasmas with Phase Contrast Imaging and Comparisons with GYRO

NASA Astrophysics Data System (ADS)

Porkolab, M.; Lin, L.; Edlund, E. M.; Rost, J. C.; Fiore, C. L.; Greenwald, M.; Mikkelsen, D.

2008-11-01

We present recent experimental measurements of turbulence and transport in C-Mod H-Mode plasmas with and without internal transport barriers (ITB) using the phase contrast imaging (PCI) diagnostic and compare the results with GYRO predictions. In plasmas without ITB, the fluctuation above 300 kHz observed by PCI agrees with ITG in GYRO simulation, including the direction of propagation, wavenumber spectrum, and absolute intensity within experimental uncertainly (+/-75%). After transition to ITBs, the observed overall fluctuation intensity increases. GYRO simulation in the core shows that ITG dominates in ITBs but its intensity is lower than the overall experimental measurements which may also include contributions from the plasma edge. These results, as well as the impact of varying ∇Ti, ∇n, and ExB shear on turbulence will be discussed. C.L. Fiore et al., Fusion Sci. Technol., 51, 303 (2007). M. Porkolab et al., IEEE Trans. Plasma Sci. 34, 229 (2006). J. Candy et al., Phys. Rev. Lett., 91, 045001 (2003).

Methods of editing cloud and atmospheric layer affected pixels from satellite data

NASA Technical Reports Server (NTRS)

Nixon, P. R. (Principal Investigator); Wiegand, C. L.; Richardson, A. J.; Johnson, M. P.; Goodier, B. G.

1981-01-01

The location and migration of cloud, land and water features were examined in spectral space (reflective VIS vs. emissive IR). Daytime HCMM data showed two distinct types of cloud affected pixels in the south Texas test area. High altitude cirrus and/or cirrostratus and "subvisible cirrus" (SCi) reflected the same or only slightly more than land features. In the emissive band, the digital counts ranged from 1 to over 75 and overlapped land features. Pixels consisting of cumulus clouds, or of mixed cumulus and landscape, clustered in a different area of spectral space than the high altitude cloud pixels. Cumulus affected pixels were more reflective than land and water pixels. In August the high altitude clouds and SCi were more emissive than similar clouds were in July. Four-channel TIROS-N data were examined with the objective of developing a multispectral screening technique for removing SCi contaminated data.

In-situ Measurements Of The Radiolytic Destruction Of Glycine In Ices: Applications To The Martian Subsurface

NASA Astrophysics Data System (ADS)

Gerakines, Perry A.; Hudson, R. L.

2012-10-01

Amino acids and other organic molecules are thought to be easily destroyed on the surface of Mars by the high flux of incident ultraviolet rays or by chemical interactions with oxidizing substances in the soil. However, organic molecules may survive in the subsurface, where chemical processes are driven by penetrating galactic cosmic rays such as MeV protons. Models of the radiation dose as a function of depth on Mars have shown that the contribution of galactic cosmic rays dominates from about one centimeter to a few meters [1]. Theoretical models have also been published to aid in understanding molecular destruction at these depths, but these usually are based on room-temperature laboratory data, studies of single-component samples, and ex-situ methods of chemical analysis. Recent studies of amino-acid survivability include those involving UV photolysis [2, 3] and gamma radiolysis [4], but nearly all chemical and kinetic analyses from such experiments involved room-temperature measurements on samples irradiated and then removed from sealed containers. We report new laboratory studies of the radiation-induced destruction of glycine-containing ices. In-situ infrared spectroscopy was used to study decay rates as a function of temperature and initial glycine concentrations. Our results indicate that glycine's destruction rate depends on temperature, the presence of H2O-ice, and the initial relative abundance of glycine. These trends are not obvious in previous work, suggesting that room-temperature measurements on pure glycine's radiation stability are not directly applicable to Mars and other environments. This work has been supported by the Goddard Center for Astrobiology. [1] Dartnell, L. R., et al., 2007. Geophys. Res. Letters 34:L02207. [2] ten Kate, I. L., et al., 2006. Planet. Space Sci. 54, 296-302. [3] Orzechowska, G. E., et al., 2007. Icarus 187, 584-591. [4] Kminek, G., Bada, J. L., 2006. Earth Planet. Sci. Lett. 245, 1-5.

Analysis on establishing Chang'E-3 landing site as a reflectance calibration target

NASA Astrophysics Data System (ADS)

Liu, Bin; Fu, Xiaohui; Zeng, Xingguo; Yao, Meijuan; Zhang, Hongbo; Su, Yan; Zhao, Shu; Xue, Xiping; Li, Chunlai; Zou, Yongliao

2015-04-01

Recent lunar orbital observations suggested that the surface reflectance calculated based on the Apollo 16 standard area and Apollo 16 sample laboratory measurement is significantly different from its true value [1-3], one reason is the composition and maturity differences between the 62231 sampling site and the Apollo 16 standard site existed, the other reason is the physical properties of the returned lunar sample, such as porosity, have been changed during the sampling operations. So more new standard targets on the Moon, besides the widely used Apollo 16 area, are needed for imaging spectrometers on lunar missions to improve their reflectance calibration accuracies. The Chang'E-3 VIS/NIR Imaging Spectrometer (VNIS), which is just fixed at the front of the Yutu rover [4], equipped with a white spectralon panel as reflectance calibration standard, can perform in situ multispectral observations around the Chang'E-3 landing site without altering the physical and mineralogical natures of lunar soils. Therefore, it provides an opportunity to establish a new reliable standard target for in-flight reflectance calibration. The reflectance calibration target should be compositional homogeneous, the topography of which must be flat, and the reflectance should be identical with no nearby units of other different materials. As we have known, Chang'e-3 probe landed on the Mare Imbrium basin in the east part of Sinus Iridum, the landing site is relatively flat at a spatial coverage of ~660km2, and this region belongs to Eratosthenian low-Ti/high-Ti mare basalts [5-6]. According to much higher resolution topography data, elemental data and reflectance data of Chang'E-2 and Chang'E-3[7-8], we preliminary analyse the possibility on establishing Chang'E-3 landing site as a reflectance calibration target. Firstly, the overall terrain of the 4 km×4 km area around the landing site is flat, but there are still three bigger craters existed. Secondly, the composition on Chang'E-3 landing site is homogeneous according to the two detection results of APXS on elements in lunar soil. At last, we compare and scale the four detection points' reflectance of VNIS, which demonstrate that the reflectance of the landing site are quite similar at the spectral range 450nm-1750nm, but differences still existed beyond 1750nm. Future work is still needed, such as photometric calibration of VNIS data, and errors estimation on reflectance calculation. Besides, the location and spatial coverage of the reflectance calibration target should be determined and its calibration accuracy should be evaluated. Acknowledgements: This work was supported by the National Natural Science Foundation of China (No.11403049 and 41490633). References: [1] J. K. Hillier et al., (1999) Icarus, 141, 205-225. [2] M. Ohtake et al., (2010) Space Sci. Rev., 154, 57-77. [3] M. Ohtake et al., (2010) Icarus, 226, 364-374. [4] B. Liu et al., (2014) RAA, 14, 1674. [5] L. Qiao et al., (2013) Sci Sin-Phys Mech Astron, 43, 1370-1386. [6] J. N. Zhao et al., (2014) Sci China-Phys Mech Astron, 57, 569-576. [7] C. L. Li et al., (2014) RAA, 14, 1514. [8] X. H. Fu et al., (2014) RAA, 14, 1595.

Depth of Formation of Ferropericlase Included in Super-Deep Diamonds

NASA Astrophysics Data System (ADS)

Anzolini, C.; Nestola, F.; Gianese, A.; Nimis, P.; Harris, J. W.

2017-12-01

Super-deep diamonds are believed to have formed at depths of at least 300 km depth (Harte, 2010). A common mineral inclusion in these diamonds is ferropericlase, (Mg,Fe)O (see Kaminsky, 2012 and references therein). Ferropericlase (fPer) is the second most abundant mineral in the lower mantle, comprising approximately 16-20 wt% (660 to 2900 km depth), and inclusions of fPer in diamond are often considered to indicate a lower-mantle origin (Harte et al., 1999). Samples from São Luiz/Juina, Brazil, are noteworthy for containing nanometer-sized magnesioferrite (Harte et al., 1999; Wirth et al., 2014; Kaminsky et al., 2015; Palot et al., 2016). Based upon a phase diagram valid for 1 atm, such exsolutions would place the origin of this assemblage in the uppermost part of the lower mantle. However, a newly reported phase diagram for magnesioferrite demonstrates that the latter is not stable at such pressures and, thus, it cannot exsolve directly from fPer at lower-mantle conditions (Uenver-Thiele et al., 2017). Here we report the investigation of two fPer inclusions, extracted from a single São Luiz diamond, by single-crystal X-ray diffraction and field emission scanning electron microscopy. Both techniques showed micrometer-sized exsolutions of magnesioferrite within the two fPers. We also completed elastic geobarometry (see Angel et al., 2015), which determined an estimate for the depth of entrapment of the two ferropericlase - diamond pairs. In the temperature range between 1273 and 1773 K, pressures varied between 9.88 and 12.34 GPa (325-410 km depth) for one inclusion and between 10.69 and 13.16 GPa (350-440 km depth) for the other one. These results strengthen the hypothesis that solitary fPer inclusions might not be reliable markers for a lower-mantle provenance. This work was supported by Fondazione CaRiPaRo and ERC-2012-StG 307322 to FN. Angel, R.J., et al. (2015) Russ Geol Geophys, 56, 211-220; Harte, B. (2010) Mineral Mag, 74, 189-215; Harte, B., et al. (1999) The Geochemical Society, Special Publication, 6, 125-153; Kaminsky, F. (2012) Earth-Sci Rev, 110, 127-147; Kaminsky, F., et al. (2015) Earth Planet Sci Lett, 417, 49-56; Palot, M., et al. (2016) Lithos, 265, 237-243; Uenver-Thiele, L., et al. (2017) Am Mineral, 102, 632-642; Wirth, R., et al. (2014) Earth Planet Sci Lett, 404, 365-375.

TrkB Activators for the Treatment of Traumatic Vision Loss

DTIC Science & Technology

2015-10-01

immunemodulator fingolimod on acute ischemic stroke . Proc Natl Acad Sci USA 111:18315-20. Gauthier R., Joly S., Pernet V., Lachapelle P. and Di Polo A...it has shown clinical efficacy in the treatment of stroke and multiple sclerosis patients (Noda et al., 2013; Yang et al., 2014; Fu et al., 2014...prevents inflammation-sensitized hypoxic- ischemic brain injury in newborns. J Neurosci. 34: 16467-81. Appendix 1. Copy of ARVO abstract

Microphysical Model Studies of Venus Clouds

NASA Astrophysics Data System (ADS)

Meade, P. E.; Bullock, M. A.; Grinspoon, D. H.

2004-11-01

We have adapted a standard cloud microphysics model to construct a self-consistent microphysical model of Venus' cloud layer which reproduces and extends previous studies (e.g. James et al. 1997). Our model is based on the Community Aerosol and Radiation Model Atmosphere (CARMA), which is a widely used computer code for terrestrial cloud microphysics, derived from the work of Toon et al. (1988). The standard code has been adapted to treat H2O and H2SO4 as co-condensing vapor species onto aqueous H2SO4 cloud droplets, as well as the nucleation of condensation nuclei to droplets. Vapor condensation and evaporation follows the method of James et al. (1997). Microphysical processes included in this model include nucleation of condensation nuclei, condensation and evaporation of H2O and H2SO4 vapor, and droplet coagulation. Vertical transport occurs though advection, eddy diffusion, sedimentation for both droplets and condensation nuclei. The cloud model is used to explore the sensitivity of Venus' cloud layer to environmental changes. Observations of the Venus' lower cloud from the Pioneer Venus, Venera, and Galileo spacecraft have suggested that the properties of the lower cloud may be time-variable, and at times may be entirely absent (Carlson et al. 1993, Grinspoon et al. 1993, Esposito et al. 1997). Our model explores the dependence of such behavior on environment factors such as variations in water or SO2 abundance. We have also calculated the optical properties of the model atmosphere using both the conventional optical constants for H2SO4 (Palmer and Williams, 1975), and the new data of Tisdale et al. (1998). This work has been supported by NASA's Exobiology Program. References Carlson, R.W., et al., 1993. Planetary and Space Science, 41, 477-486. Esposito, L.W., et al., 1997. In Venus II, eds. S.W. Bougher et al., pp. 415-458, University of Arizona Press, Tucson. Grinspoon, D.H., et al., 1993. Planetary and Space Science, 41 (July 1993), 515-542. James, E. P., et al., 1997. Icarus, 129, 147-171. Palmer, K.F., and D. Williams, 1975. Applied Optics, 14, 208-219. Tisdale, R.T., et al., 1998. Journal of Geophysical Research, 103, 25,353-25,370. Toon , O. B., et al., 1988. J. Atmos. Sci., 45, 2123-2143.

Rapid high-silica magma generation in basalt-dominated rift settings

NASA Astrophysics Data System (ADS)

Berg, Sylvia E.; Troll, Valentin R.; Burchardt, Steffi; Deegan, Frances M.; Riishuus, Morten S.; Whitehouse, Martin J.; Harris, Chris; Freda, Carmela; Ellis, Ben S.; Krumbholz, Michael; Gústafsson, Ludvik E.

2015-04-01

The processes that drive large-scale silicic magmatism in basalt-dominated provinces have been widely debated for decades, with Iceland being at the centre of this discussion [1-5]. Iceland hosts large accumulations of silicic rocks in a largely basaltic oceanic setting that is considered by some workers to resemble the situation documented for the Hadean [6-7]. We have investigated the time scales and processes of silicic volcanism in the largest complete pulse of Neogene rift-related silicic magmatism preserved in Iceland (>450 km3), which is a potential analogue of initial continent nucleation in early Earth. Borgarfjörður Eystri in NE-Iceland hosts silicic rocks in excess of 20 vol.%, which exceeds the ≤12 vol% usual for Iceland [3,8]. New SIMS zircon ages document that the dominantly explosive silicic pulse was generated within a ≤2 Myr window (13.5 ± 0.2 to 12.2 ± 03 Ma), and sub-mantle zircon δ18O values (1.2 to 4.5 ± 0.2‰, n=337) indicate ≤33% assimilation of low-δ18O hydrothermally-altered crust (δ18O=0‰), with intense crustal melting at 12.5 Ma, followed by rapid termination of silicic magma production once crustal fertility declined [9]. This silicic outburst was likely caused by extensive rift flank volcanism due to a rift relocation and a flare of the Iceland plume [4,10] that triggered large-scale crustal melting and generated mixed-origin silicic melts. High-silica melt production from a basaltic parent was replicated in a set of new partial melting experiments of regional hydrated basalts, conducted at 800-900°C and 150 MPa, that produced silicic melt pockets up to 77 wt.% SiO2. Moreover, Ti-in-zircon thermometry from Borgarfjörður Eystri give a zircon crystallisation temperature ~713°C (Ti range from 2.4 to 22.1 ppm, average=7.7 ppm, n=142), which is lower than recorded elsewhere in Iceland [11], but closely overlaps with the zircon crystallisation temperatures documented for Hadean zircon populations [11-13], hinting at crustal recycling as a key process. Our results therefore provide a mechanism and a time-scale for rapid, voluminous silicic magma generation in modern and ancient basalt-dominated rift setting, such as Afar, Taupo, and potentially early Earth. The Neogene plume-related rift flank setting of NE-Iceland may thus constitute a plausible geodynamic and compositional analogue for generating silicic (continental) crust in the subduction-free setting of a young Earth (e.g. ≥3 Ga [14]). [1] Bunsen, R. 1851. Ann. Phys. Chem. 159, 197-272. [2] MacDonald R., et al., 1987. Mineral. Mag. 51, 183-202. [3] Jonasson, K., 2007. J. Geodyn. 43, 101-117. [4] Martin, E., et al., 2011. Earth Planet. Sci. Lett. 311, 28-38. [5] Charreteur, G., et al., 2013.Contrib. Mineral. Petr. 166, 471- 490. [6] Willbold, E., et al., 2009. Earth Planet. Sci. Lett. 279, 44-52. [7] Reimink, J.R., et al., 2014. Nat. Geosci. 7, 529-533. [8] Gústafsson, L.E., et al., 1989. Jökull 39, 75-89. [9] Meade, F.C., et al., 2014. Nat. comm. 5. [10] Óskarsson, B.V., Riishuus, M.S., 2013. J. Volcanol. Geoth. Res. 267, 92-118. [11] Carley, T.L., et al., 2014. Earth Planet. Sci. Lett. 405, 85-97. [12] Trail, D., et al., 2007. Geochem. Geophys. Geosyst.8, Q06014. [13] Harrison, T.M. et al., 2008. Earth Planet. Sci. Lett.268, 476-486. [14] Kamber, B. S., et al., 2005. Earth Planet. Sci. Lett. 240, 276-290.

78 FR 13383 - Public Availability of the National Aeronautics and Space Administration FY 2012 Service Contract...

Federal Register 2010, 2011, 2012, 2013, 2014

2013-02-27

... NATIONAL AERONAUTICS AND SPACE ADMINISTRATION Public Availability of the National Aeronautics and Space Administration FY 2012 Service Contract Inventory (SCI) AGENCY: Office of Procurement, National Aeronautics and Space Administration. ACTION: Notice of Public Availability of the FY 2012 Service Contract...

Fatigue of muscles weakened by death of motoneurons.

PubMed

Thomas, Christine K; Zijdewind, Inge

2006-01-01

Weakness is a characteristic of muscles influenced by the postpolio syndrome (PPS), amyotrophic lateral sclerosis (ALS), and spinal cord injury (SCI). The strength deficits relate to changes in muscle use and to the chronic denervation that can follow the spinal motoneuron death common to these disorders. PPS, ALS, and SCI also involve variable amounts of supraspinal neuron death, the effects of which on muscle weakness remains unclear. Nevertheless, weakness of muscle itself defines the functional consequences of these disorders. A weaker muscle requires an individual to work that muscle at higher than usual intensities relative to its maximal capacity, inducing progressive fatigue and an increased sense of effort. Little evidence is available to suggest that the fatigue commonly experienced by individuals with these disorders relates to an increase in the intrinsic fatigability of the muscle fibers. The only exception is when SCI induces chronic muscle paralysis. To reduce long-term functional deficits in these disorders, studies must identify the signaling pathways that influence neuron survival and determine the factors that encourage and limit sprouting of motor axons. This may ensure that a greater proportion of the fibers in each muscle remain innervated and available for use.

Concentration Waves in High-Entropy Alloys - a new alloy design approach

NASA Astrophysics Data System (ADS)

Singh, Prashant; Johnson, Duane D.

2015-03-01

Chemical short-range order (SRO) in solid solutions can be interpreted as a ``concentration wave'' - a Fourier decomposition of nascent order - identified experimentally via Warren-Cowley SRO parameters. We present a rigorous thermodynamic theory to predict and uniquely interpret the SRO in N -component alloys. Based on KKR-CPA electronic structure, we implemented this method using thermodynamic linear-response to include all alloying effects, e.g., band-filling, hybridization, Fermi -surface nesting and van Hove instabilities. We apply this first-principles method to high-entropy alloys (HEAs), i.e., solid solutions with N >4 that inhibit small-cell order due to large entropy competing against ordering enthalpy, as their properties are sensitive to SRO. We validated theory with comparison to experiments in A2 Nb-Al-Ti and A1 Cu-Ni-Zn . We then predict and analyze SRO and mechanical trends in Ni-Ti-Zr-Cu-Al and Co-Cr-Fe-Mn-Ni systems - showcasing this new first-principles-based alloy design method. Work was supported by the USDoE, Office of Sci., Basic Energy Sci., Materials Sci. and Eng. Division for `Materials Discovery.' Research was performed at Ames Lab, operated by Iowa State University under Contract #DE-AC02-07CH11358.

Large eddy simulation study of spanwise spacing effects on secondary flows in turbulent channel flow

NASA Astrophysics Data System (ADS)

Aliakbarimiyanmahaleh, Mohammad; Anderson, William

2015-11-01

The structure of turbulent flow over a complex topography composed of streamwise-aligned rows of cones with varying spanwise spacing, s is studied with large-eddy simulation (LES). Similar to the experimental study of Vanderwel and Ganapathisubramani, 2015: J. Fluid Mech., we investigate the relationship between secondary flow and s, for 0 . 25 <= s / δ <= 5 . For cases with s / δ > 2 , domain-scale rollers freely exist. These had previously been called ``turbulent secondary flows'' (Willingham et al., 2014: Phys. Fluids; Barros and Christensen, 2014: J. Fluid Mech.; Anderson et al., 2015: J. Fluid Mech.), but closer inspection of the statistics indicates these are a turbulent tertiary flow: they only remain ``anchored'' to the conical roughness elements for s / δ > 2 . For s / δ < 2 , turbulent tertiary flows are prevented from occupying the domain by virtue of proximity to adjacent, counter-rotating tertiary flows. Turbulent secondary flows are associated with the conical roughness elements. These turbulent secondary flows emanate from individual conical topographic elements and set the roughness sublayer depth. The turbulent secondary flows remain intact for large and small spacing. For s / δ < 1 , a mean tertiary flow is not present. This work was supported by the Air Force Office of Sci. Research, Young Inv. Program (PM: Dr. R. Ponnoppan and Ms. E. Montomery) under Grant # FA9550-14-1-0394. Computational resources were provided by the Texas Adv. Comp. Center at the Univ. of Texas.

Detecting Organic Compounds Released from Iron Oxidizing Bacteria using Sample Analysis at Mars (SAM)-like Instrument Protocols

NASA Astrophysics Data System (ADS)

Glavin, D. P.; Popa, R.; Martin, M. G.; Freissinet, C.; Fisk, M. R.; Dworkin, J. P.; Mahaffy, P. R.

2012-12-01

Mars is a planet of great interest for Astrobiology since its past environmental conditions are thought to have been favourable for the emergence life. At present, the Red Planet is extremely cold and dry and the surface is exposed to intense UV and ionizing radiation, conditions generally considered to be incompatible with life as we know it on Earth. It was proposed that the shallow subsurface of Mars, where temperatures can be above freezing and liquid water can exist on rock surfaces, could harbor chemolithoautotrophic bacteria such as the iron oxidizing microorganism Pseudomonas sp. HerB [Popa et al. 2012]. The Mars Science Laboratory (MSL) mission will provide the next opportunity to carry out in situ measurements for organic compounds of possible biological origin on Mars. One instrument onboard MSL, called the Sample Analysis at Mars (SAM) instrument suite, will carry out a broad and sensitive search for organic compounds in surface samples using either high temperature pyrolysis or chemical extraction followed by gas chromatography mass spectrometry [Mahaffy et al. 2012]. We present gas chromatograph mass spectrometer (GC/MS) data on crushed olivine rock powders that have been inoculated with Pseudomonas sp. HerB at different concentrations ranging from ~102 to 107 cells per gram. The inoculated olivine samples were heated under helium carrier gas flow at 500°C and the pyrolysis products concentrated using a SAM-like hydrocarbon trap set at -20°C followed by trap heating and analysis by GC/MS. In addition, the samples were also extracted using a low temperature "one-pot" chemical extraction technique using N-methyl, N-(tert-butyldimethylsilyl) trifluoroacetamide (MTBSTFA) as the silylating agent prior to GC/MS analysis [Stalport et al. 2012]. We identified several aldehydes, thiols, and alkene nitriles after pyrolysis GC/MS analysis of the bacteria that were not found in the olivine control samples that had not been inoculated with bacteria. The distribution of pyrolysis products extracted from the bacteria was clearly distinct from similar GC/MS analyses of the carbonaceous meteorite Murchison that was dominated by sulfur containing aromatic compounds. A similar comparison, if organic compounds are detected by SAM on Mars, could be useful to help discriminate between meteoritic or biological origins. References: Popa, R. et al. (2012), Olivine-respiring bacteria isolated from the rock-ice interface in a lava-tube cave, a Mars analog environment. Astrobiology 12, 9-18; Mahaffy, P. R. et al. (2012), The Sample Analysis at Mars investigation and instrument suite. Planet. Space Sci., doi: 10.1007/s11214-012-9879-z; Stalport, F. et al. (2012) The influence of mineralogy on recovering organic acids from Mars analogue materials using the ''one-pot'' derivatization experiment on the Sample Analysis at Mars (SAM) instrument suite. Planet. Space Sci., doi:10.1016/j.pss.2012.02.010.

Navigating "thorny" issues

NASA Astrophysics Data System (ADS)

Hutchinson, Kashema; Gilbert, Aderinsola; Malyukova, Anna

2016-09-01

In their article Mindfulness and discussing ` thorny' issues in the classroom Konstantinos Alexakos et al. (Cult Stud Sci Educ, 2016. doi: 10.1007/s11422-015-9718-0) describe "thorny" issues as "difficult topics to discuss because they are more personal to some perhaps even cause pain and violence." As women from different backgrounds, we engage in a metalogue, which expands on our thoughts and emotions the thorny issues evoked. Our discussion is grounded in theoretical frameworks of mindfulness, wellness, and safe space for learning. We also reflect on our experiences of facing some of the thorny issues in our academic and personal lives. Having trust and respect for one another and being aware of thorny issues allows for a meaningful conversation about the complexity and nuances involved in discussing difficult topics in a classroom setting.

Spin and Wind Directions I: Identifying Entanglement in Nature and Cognition.

PubMed

Aerts, Diederik; Arguëlles, Jonito Aerts; Beltran, Lester; Geriente, Suzette; Sassoli de Bianchi, Massimiliano; Sozzo, Sandro; Veloz, Tomas

2018-01-01

We present a cognitive psychology experiment where participants were asked to select pairs of spatial directions that they considered to be the best example of Two different wind directions . Data are shown to violate the CHSH version of Bell's inequality with the same magnitude as in typical Bell-test experiments with entangled spins. Wind directions thus appear to be conceptual entities connected through meaning, in human cognition, in a similar way as spins appear to be entangled in experiments conducted in physics laboratories. This is the first part of a two-part article. In the second part (Aerts et al. in Found Sci, 2017) we present a symmetrized version of the same experiment for which we provide a quantum modeling of the collected data in Hilbert space.

MONTE: the next generation of mission design and navigation software

NASA Astrophysics Data System (ADS)

Evans, Scott; Taber, William; Drain, Theodore; Smith, Jonathon; Wu, Hsi-Cheng; Guevara, Michelle; Sunseri, Richard; Evans, James

2018-03-01

The Mission analysis, Operations and Navigation Toolkit Environment (MONTE) (Sunseri et al. in NASA Tech Briefs 36(9), 2012) is an astrodynamic toolkit produced by the Mission Design and Navigation Software Group at the Jet Propulsion Laboratory. It provides a single integrated environment for all phases of deep space and Earth orbiting missions. Capabilities include: trajectory optimization and analysis, operational orbit determination, flight path control, and 2D/3D visualization. MONTE is presented to the user as an importable Python language module. This allows a simple but powerful user interface via CLUI or script. In addition, the Python interface allows MONTE to be used seamlessly with other canonical scientific programming tools such as SciPy, NumPy, and Matplotlib. MONTE is the prime operational orbit determination software for all JPL navigated missions.

The geologic history of the Galilean satellite Callisto. (Invited)

NASA Astrophysics Data System (ADS)

Wagner, R. J.; Neukum, G.; Wolf, U.; Greeley, R.

2009-12-01

Introduction: Callisto, the second-largest Galilean satellite of Jupiter, is a Mercury-sized icy moon with a diameter of 4816 km and an average density of 1.83 gcm-3. Despite its size the images returned by the Voyager cameras in two flybys in 1979 showed a densely cratered surface with little geologic diversity, in contrast to its neighbor Ganymede [1][2][3][4]. Between 1995 and 2003 the SSI camera aboard the Galileo spacecraft has extended but not completed the existing Voyager image data base of Callisto [2][3]. Geologic processes: Galileo SSI has shown that the two dominant geological processes are impact craters and surface degradation [2][3][4]. Abundant but less important are landforms created by tectonism, such as fractures and lineaments [1][2][3][4]. Surface ages are obtained by impact chronology models either with a lunar-like cratering rate, mostly by asteroids [5], or with a constant cratering rate, mostly by comets [6]. Geologic history: Various aspects of Callisto’s geologic history, based on Voyager and SSI data, were discussed in detail by [1][2][3][4]. Cratering chronology models [5][6] agree that Callisto’s densely cratered plains are mostly old, on the order of 4 Ga and older. The morphology of craters and basins is much like that on Ganymede, implying similar subsurface structure at the time of their formation. Palimpsests as on Ganymede occur, but most of them are heavily degraded and not easily recognizable. Callisto could have experienced an early period of heavy bombardment, as inferred from the lunar-like chronology model [5], and large impact structures (e.g., Valhalla, Lofn) could have formed towards its end, 3.8 - 4.0 Ga ago. All topographically high-standing landforms (e.g., crater rims) were affected by sublimation degradation, triggered by a substantial amount of CO2 in the icy crust [7]. Degradation started along pre-existing zones of weakness, caused by early tectonic stress. On-going sublimation and separation of highly volatile from less volatile materials created a globally abundant dark layer. It remains an unsolved question if degradation and the accumulation of dark material was going on at a fast rate during a time of heavy bombardment but went on at a considerably slow rate since 3.4 - 3.6 ago [4][5], or has continued at a constant rate until more recent times [4][6]. References: [1] Schenk, P. M. (1995), J. Geophys. Res. 100 (E9), 19,023 - 19,040. [2] Greeley, R. et al. (2000), Planet. Space Sci. 48, 829 - 853. [3] Moore, J. M. et al. (2004), in: Jupiter (F. Bagenal et al., eds.), Cambridge Planet. Sci., Vol. 1, p. 397 - 426. [4] Wagner R. (2007), PhD. Dissertation (in german), Free University of Berlin, Germany, http://www.diss.fu-berlin.de/2007/806. [5] Neukum G. et al. (1998), Lunar Planet. Sci. Conf. XXIX, abstr. #1992 [CD-Rom]. [6] Zahnle K. et al. (2003), Icarus 163, 263 - 289. [7] Moore J. M. et al. (1999), Icarus 140, 294 - 312.

Posttraumatic growth in people with traumatic long-term spinal cord injury: predictive role of basic hope and coping.

PubMed

Byra, S

2016-06-01

Participants with spinal cord injury (SCI) sustained at least 15 years before the study completed questionnaires measuring posttraumatic growth (PTG), basic hope and coping strategies. To determine contribution of basic hope and coping strategies to accounting for PTG variability in participants with traumatic long-term SCI. Polish rehabilitation centres, foundations and associations implementing social inclusion and professional activation programmes. Participants were enrolled based on their medical history by trained rehabilitation specialists and psychologists. The set of questionnaires included the following: The Post-traumatic Growth Inventory; The Coping Orientations to Problems Experienced (COPE); and Basic Hope Inventory. A study of 169 individuals with paraplegia in the range of PTG showed the highest degree of positive changes in appreciation of life (AL) and the lowest in self-perception. Regression analysis showed that coping strategies such as religion (REL), focus on the problem, humour, alcohol/drug use ideation and basic hope jointly account for 60% of variance of PTG. The highest contribution to accounting for this variability had REL. Also, it was found that coping strategies and basic hope allow to predict variance of individual growth aspects. Age at trauma exposure positively correlated with changes in AL and spiritual change. No significant relationship between growth and age of participants was confirmed. PTG occurring in people with long-term traumatic SCI is primarily manifested in increased AL. Specific coping strategies and basic hope have a significant role in fostering positive changes.

Wind Profiling in a Cloudy Convective Atmospheric Boundary Layer Over Land

DTIC Science & Technology

1992-12-01

Albrecht Professor of Meteorology Thesis Advisor / 2 / / 9 /z George S. Young Associate Professor of Meteorology Dennis W. Thomson Professor of...Schubert et al., 1979; Brost et al., 1982; Albrecht et al., 1985). The eastern Pacific, off the California coast, for example, is an area of persistent...Publications, Inc., 435 pp. Brost , R. A., D. H. Lenschow and J.C. Wyngaard, 1982: Marine stratocumulus layers. Part I: Mean conditions. J Atmos. Sci., 39

Ceres composition as inferred by the VIR-Dawn imaging spectrometer

NASA Astrophysics Data System (ADS)

Longobardo, Andrea

2016-07-01

The NASA's Dawn spacecraft [1] is orbiting around Ceres since early 2015. The Dawn mission to Ceres is divided in five stages, characterized by different altitudes above the Ceres mean surface. These five stages correspond with the different phases of the mission,, i.e. Approach, Rotational Characterization, Survey, High Altitude Mapping Orbit (HAMO) and Low Altitude Mapping Orbit (LAMO). Each phase is characterized by an increasing spatial resolution linked with the spacecraft altitude. The VIR imaging spectrometer [2] on board the Dawn spacecraft is providing a huge amount of data and giving an essential contribution to understand the Ceres composition and to give constraint about its evolution. VIR observations revealed that Ceres is a dark body, with an average albedo of 0.08 measured at 1.2 mm [3]. However, specific features seen at the local scale may show substantially higher albedo (i.e. greater than 0.2), especially in Occator, Haulani and Oxo craters [4]. VIR data reveal that the Ceres visible and near-infrared spectra (wavelength range from 0.25 to 5 mm) are mainly characterized by the following absorptions: - 2.7 mm band, ascribed to OH-bearing materials [5] and distributed across the Ceres surface; - 3.05 mm band, ascribed to NH4-bearing materials [5] and also ubiquitous on the Ceres surface; - 3.3-3.5 mm complex and 3.9 mm band, ascribed to carbonates [4] and observed only at some locations [6]. The presence of these features, in particular the 3.05 mm band, indicate widespread occurrence of ammoniated phyllosilicates [5], which could be mixed with carbonates in specific regions. The phyllosilicates composition is basically homogeneous across the Ceres surface, as suggested by the low variation of 2.7 mm and 3.05 mm band centers [7]. The presence of ammonia suggests the presence of outer Solar System materials, which could have been brought in the Main Asteroid Belt and accreted during the Ceres formation [8]. Alternatively, Ceres itself could have been formed in the outer Solar System before to migrate in its actual location [9]. References [1] Russell, C.T. et al., Science, 336, 684, 2012 [2] De Sanctis M.C. et al., Space Sci. Rev., 163, 329-336, 2011 [3] Longobardo, A. et al., LPSC abstract, #2239, 2016 [4] De Sanctis, M.C. et al., LPSC abstract, #1832, 2016 [5] De Sanctis, M.C. et al., Nature, 528, 241-244, 2015 [6] Palomba, E. et al., LPSC abstract, #2166, 2016 [7] Ammannito, E. et al., LPSC abstract, #3020, 2016 [8] Johansen, A. et al., Sci. Adv. 1, 1500109, 2015 [9] McKinnon, W.B. et al., Proc. Conf. Asteroids, Comets, Meteors, # 6475, 2012

Electrolytic Transformation of Hexahydro-1,3,5-Trinitro-1,3,5-Triazine (RDX) and 2,4,6-Trinitrotoluene (TNT) in Aqueous Solutions

DTIC Science & Technology

2005-08-01

several years (Bunce et al. 1997; de Lima Leite et al. 2003; Panizza and Cerisola 2004). Treatment is achieved by either oxidation (anodic) or...and mixed anaerobic cultures," Environ. Sci. Technol. 35, 4341-4346. Panizza , M., and Cerisola, G. (2004). "Influence of anode material on the

Search and Neutralize Factors (CSPGs) that Induce Decline in Transmission to Neurons from Spared Fibers after Chronic Spinal Cord Injury

DTIC Science & Technology

2012-10-01

damaged spinal cord after chronic HX are the result of reduced conduction in uncut axons (Hunanyan et al. 2011). Since elevated level of chondroitin ... sulfate proteoglycans (CSPGs) in the vicinity of the injury has been reported to be a major obstacle for recovery after SCI (Snow et al., 1990; Jones

A Nonlinear Transfer Operator Theorem

NASA Astrophysics Data System (ADS)

Pollicott, Mark

2017-02-01

In recent papers, Kenyon et al. (Ergod Theory Dyn Syst 32:1567-1584 2012), and Fan et al. (C R Math Acad Sci Paris 349:961-964 2011, Adv Math 295:271-333 2016) introduced a form of non-linear thermodynamic formalism based on solutions to a non-linear equation using matrices. In this note we consider the more general setting of Hölder continuous functions.

Identifying new surface constituents of icy moons using mid-infrared spectroscopy

NASA Astrophysics Data System (ADS)

Young, Cindy L.; Wray, James J.; Hand, Kevin P.; Poston, Michael J.; Carlson, Robert W.; Clark, Roger N.; Spencer, John R.; Jennings, Donald E.

2015-11-01

Spectroscopic compositional studies of the icy satellites can help us to better understand the formation and evolution of material in the outer solar system. The spectral complexity of the Saturnian satellite system as seen in reflected visible light suggests additional complexity may be present at mid-infrared wavelengths from which unique compositional information can be gleaned [1]. In addition, the mid-infrared is the region of the stronger fundamental diagnostic vibrational modes of many compounds. However, Cassini Composite Infrared Spectrometer (CIRS) surface compositional studies have received little attention to date.We are exploring the suitability of mid-infrared spectroscopy for discovering non-H2O compounds on icy moon surfaces. On the dark terrain of Iapetus, we find an emissivity feature at ~855 cm-1 and a potential doublet at 660 and 690 cm-1 that do not correspond to any known instrument artifacts [2]. We attribute the 855 cm-1 feature to fine-grained silicates, similar to those found in dust on Mars and in meteorites, which are nearly featureless at shorter wavelengths [3]. Although silicates on the dark terrains of Saturn’s icy moons have been suspected for decades, there have been no definitive prior detections. Serpentines measured at ambient conditions have features near 855 cm-1 and 660 cm-1 [4]. However, peaks can shift depending on temperature, pressure, and grain size, so measurements at Iapetus-like conditions are necessary for more positive identifications [e.g., 5].We measured the vacuum, low temperature (125 K) spectra of various fine-grained powdered silicates. We find that some of these materials do have emissivity features near 855 cm-1 and match the doublet. Identifying a specific silicate would provide clues into the sources and sinks of the dark material in the Saturnian system. We report on our ongoing exploration of the CIRS icy moon dataset and plans for future measurements in JPL’s Icy Worlds Simulation Lab.[1] Flasar, F.M., et al. (2004), Space Sci Rev, 115, 169.[2] Young, C.L., et al. (in review), ApJ Lett.[3] Christensen, P.R., et al. (2004), Sci, 306, 1733.[4] Bishop, J.L., et al. (2008), Clay Minerals, 43, 35.[5] Wray, J.J., et al. (2014), DPS 46th Meeting, Vol. 46.

Fundamental considerations of water repellancy in soil, and related effects on other natural and man-made materials

NASA Astrophysics Data System (ADS)

Matthews, G. Peter

2010-05-01

This presentation will concern the understanding of soil water repellancy and wettability at a fundamental level, and the difficulties of relating the very small, micron scale at which the repellancy and wettability characteristics are produced to the much larger, field scale at which they are normally observed. The presentation will not be a review of past work, but rather will concentrate on recent publications, publications in press, and speculative considerations which may lead to future work in this area. There are three fundamental components of water repellancy - the nature of the soil surfaces themselves, the effect of organic matter and microbiologically produced substances, and the topology of the resultant surfaces. The effects of hydrophobic surfaces will be illustrated by a consideration of the wettability of substances such as commercially produced talc grades. The faces of these platey mineral particles are hydrophobic, whereas their edges are hydrophilic, and the combination not only causes water repellency in itself, but also causes unusual adsorption effects from aqueous solution. The effect of organic matter on soil wettability has been widely studied, often by core-scale wettability experiments. It will be shown how a consideration of micro-wetting effects has led to a more robust data analysis method for such studies (Matthews, G. P. et al, European J.Soil Sci., 2008). Traditionally wetting fronts are assumed to advance in proportion to the square root of time (as predicted by the Washburn equation), but micro-modelling shows that, once inertial effects are taken into account, low-volume fingers of wetting fluid track through porous substances in advance of the observed Washburn wetting front (Bodurtha, P. et al, J.Colloid Interface Sci., 2005). The effects of micro-topology are also well known (Ridgway, C. J. et al, J.Colloid Interface Sci., 2001), but need to be integrated and upscaled, as described below. Soil water repellency is not only dependant on the soil mineral characteristics, surface topology and organic matter content, but is also influenced by microbiological activity. The production of hydrophobic microbial biomass and exudates alter the hydrological characteristics of soil (Chan, K. Y., Soil Sci.Soc.Am.J., 1992) and strengthen the bonds between soil particles. Amongst these are extracellular polymeric substances (EPS), which are produced as a result of microbial activity and increase during periods of substrate utilisation and microbial growth (Hallett, P. D. et al, European J.Soil Sci., 1999). They form part of a wide spectrum of soil organic species, many produced by the soil's bacterial and fungal biomass. EPS provides a living protective membrane between changing hydrological conditions and the micro-organisms. It comprises polysaccharides and smaller amounts of protein, lipids and humic substances, with masses ranging from 103 to 108 kDaltons (Allison, D. G. et al, Fems Microbiology Letters, 1998). The small amounts of EPS in soil have a disproportionately large effect on soil hydraulic properties, and the response of EPS to major perturbations, such as wetting and drying cycles, has recently been well characterised (Or, D. et al, Vadose Zone J, 2007). Therefore, as will be described, the use of EPS as an analogue to the wider range of organic species can lead to an understanding of climatic effects on soil wettability. The upscaling of the effects from micron to field scale requires a highly detailed modelling approach, using a dual -porous void structure model (a modification of the previous ‘Pore-Cor' model) which takes into account both the soil micro-matrix and the macroscopic percolation and wetting pathways (Laudone, G. M. et al, European J.Soil Sci., submitted). Super-hydrophobicity in natural materials (the ‘lotus' effect) and man-made materials (micro-structured arrays) will also be explained and illustrated, and the condition under which super-hydrophobicity can flip to super-wettability. Super-hydrophobicity gives an unusual insight into the less extreme examples of water repellancy found in many soils.

Nitrogen isotopic fractionation during plasma synthesis of Titan's aerosols analogues

NASA Astrophysics Data System (ADS)

Kuga, M.; Carrasco, N.; Marty, B.; Marrocchi, Y.; Bernard, S.; Rigaudier, T.

2013-12-01

The Cassini-Huygens mission recently provided measurements of the abundance of nitrogen isotopes in Titan's atmosphere. The 14N/15N ratio in the two most abundant N-bearing molecules in Titan's atmosphere was found to be 183×5 for N2 [1] and 56×8 for HCN [2]. Those two molecules are greatly enriched in the heavier isotope 15N compared to our terrestrial atmosphere and Titan's HCN is about three times richer in 15N than its potential photochemical precursor N2. This implies an important fractionation process in the HCN production chain, which is tentatively attributed to an isotopic selectivity of the photodissociation of N2 in Titan's ionosphere [3-4]. The organic aerosols, forming the Titan's orange characteristic haze layers, also contain large amounts of nitrogen [5], and thus represent a third important nitrogen reservoir in Titan's atmosphere. These organic aerosols are presumably produced in the upper atmosphere by chemical reactions between N2 and CH4 induced by solar radiation and electron bombardment from Saturn's magnetosphere. As HCN is a possible precursor for aerosol polymerization [6-7], the 15N enrichment observed in HCN may be linked to the polymerization process. Unfortunately, no data exists on the isotopic nitrogen abundance in Titan's aerosols, and this question remains open. To address this issue, laboratory aerosols analogues have been produced in a N2-CH4 plasma and their nitrogen isotopic composition have been investigated. In this study, the experimental aerosols, called " tholins ", have been synthetized in the PAMPRE reactor (LATMOS, France). This setup is dedicated to simulate chemical processes occurring in Titan's atmosphere and consists in an RF plasma discharge initiated in a N2-CH4 gas mixture at room temperature [8-9]. For our purpose, tholins were produced at different initial CH4 percentages (1, 2, 5, 10%), representative of the variation of the CH4 concentration in Titan's atmosphere. 15N/14N ratio of the N2 gas used in the initial gas mixture was analyzed by dual-inlet and tholins nitrogen isotopes were measured by EA-IRMS. PAMPRE tholins are depleted in 15N by -15 to -25‰ relative to the initial N2. Comparison of this nitrogen isotopic fractionation with a N2-CO-H2O plasma experiment done in very similar experimental conditions and resulting in a very close 15N depletion, has led us to interpret this 15N depletion between N2 and organic aerosols as a kinetic isotopic fractionation occurring during N2 dissociation in the plasma. This nitrogen isotopic fractionation, although important and larger than what is observed in natural terrestrial samples, is weak compared to what is measured in Titan's atmosphere for N2 and HCN. This apparent inconsistency will be discussed. [1] Niemann et al. (2010) JGR, 115, 1151-1154. [2] Vinatier et al. (2007) Icarus, 191, 712-721. [3] Liang et al. (2007) Ap.J. Lett., 664, L115. [4] Croteau et al. (2011) Ap.J. Lett., 728, L32. [5] Israel et al. (2005) [6] Lebonnois et al. (2002) Icarus, 159, 505-517. [7] Lavvas et al. 2008) Planet. Space Sci., 56, 67-99. [8] Szopa et al. (2006) Planet. Space. Sci., 54, 394-404. [9] Sciamma-O'Brien et al. (2010) Icarus, 209, 704-714.

Insolation and Resulting Surface Temperatures of the Kuiper-Rudaki Study Region on Mercury.

NASA Astrophysics Data System (ADS)

Bauch, Karin E.; Hiesinger, Harald; D'Amore, Mario; Helbert, Jörn; Weinauer, Julia

2016-04-01

The imaging spectrometer MERTIS (Mercury Radiometer and Thermal Infrared Spectrometer) is part of the payload of ESA's BepiColombo mission, which is scheduled for launch in 2017 [1]. The instrument consists of an IR-spectrometer and radiometer, which observe the surface in the wavelength range of 7-14 and 7-40μm, respectively. The four scientific objectives are to a) study Mercury's surface composition, b) identify rock-forming minerals, c) globally map the surface mineralogy and d) study surface temperature and thermal inertia [1, 2]. In preparation of the MERTIS experiment, we performed detailed thermal models of the lunar surface, which we extrapolated to Mercury. In order to calculate insolation and surface temperatures, we use a numerical model, which has been described by [7]. Surface temperatures are dependent on the surface and subsurface bulk thermophysical properties, such as bulk density, heat capacity, thermal conductivity, emissivity, topography, and albedo. Lunar and Mercurian surface temperatures show the same general characteristics. Both have very steep temperature gradients at sunrise and sunset, due to the lack of an atmosphere. However, there are major differences due to the orbital characteristics. On Mercury the 3:2 resonant rotation rate and the eccentric orbit causes local noon at longitudes 0° and 180° to coincide with perihelion, which leads to "hot poles". At longitudes 90° and 270° , local noon coincides with aphelion, which results in "cold poles" [8]. At these longitudes brief secondary sunrises and sunsets are visible, when Mercury's orbital angular velocity exceeds the spin rate during perihelion [8]. Here we present diurnal temperature curves of the Kuiper-Rudaki study region, based on thermophysical estimates and MESSENGER (Mercury Surface, Space Environment, Geochemistry, and Ranging [9]) albedo data with a resolution of 1000m/px. Our study region spans more than 90° along the equator, thus allowing us to study both, hot and cold poles along the equator. The region shows smooth plains surrounding crater Rudaki (˜120km), as well as cratered terrain around the prominent crater Kuiper (˜60km) and has been extensively covered by measurements during the MESSENGER mission. Temperatures range from about 100K during the night to 570K (cold pole) and 700K (hot pole) at local noon. The floor of Kuiper crater reaches temperatures of ˜660K at local noon, while those at Rudaki crater are 625K (+/-5K). Due to their higher albedo, the rays of Kuiper crater are about 5K colder than the surrounding regions. These temperature estimates will aid the accurate interpretation of future MERTIS spectra of the region obtained during the BepiColombo mission [10]. References: [1] Hiesinger, H. et al. (2010), PSS 58, 144-165. [2] Helbert, J. et al. (2005), LPSC XXXVI, #1753. [3] Keihm, S.J. and Langseth, M.G. (1973), Proc. Lunar Sci. Conf. 4th, 2503-2513. [4] Lawson, S.L. et al. (2000), JGR 105, E5, 4273-4290. [5] Pieters, C.M. et al. (2009), Science 326, 568-572. [6] Paige, D.A. et al. (2010), Space Sci. Rev 150, 125-160. [7] Bauch, K.E. et al. (2014), PSS 101, 27-36. [8] Vasavada, A. et al. (1999), Icarus 141, 179-193. [9] Solomon, S.C. et al. (2008), Science 321, 59-62. [10] D'Amore et al. (2013), AGU, #P13A-1735.

Asteroids and Meteorites from Venus? Only the Earth Goddess Knows

NASA Astrophysics Data System (ADS)

Dones, Henry; Zahnle, Kevin J.; Alvarellos, José L.

2018-04-01

No meteorites from Venus have been found; indeed, some find theirexistence unlikely because of the perceived difficulty of launchingrocks at speeds above 10 km/s and traversing the planet's 93 baratmosphere. [1] Nonetheless, we keep hope alive, since cosmochemistssay they can identify Cytherean meteorites, should candidates be found[2]. Gladman et al. [3] modeled the exchange of impact ejecta betweenthe terrestrial planets, but did not consider meteorites launched fromVenus in any detail. At the time of Gladman's work, no asteroids thatremained entirely within Earth's orbit were known. 14 suchEarth-interior objects with good orbits have now been discovered, andare known as Atiras, for the Pawnee goddess of the Earth. The largestknown member of the class is 163693 Atira, a binary whose componentshave diameters of approximately 4.8 and 1 km. Discovery of Atiras isvery incomplete because they can only be seen at small solarelongations [4]. Greenstreet et al. [5] modeled the orbitaldistribution of Atiras from main-belt asteroidal and cometary sourceregions, while Ribeiro et al. [6] mapped the stability region ofhypothetical Atiras and integrated the orbits of clones of 12 realAtiras for 1 million years. 97% of the clones survived for 1 Myrimpact with Venus was the most common fate of those that met theirends. We have performed orbital integrations of 1000 clones of each ofthe known Atiras, and of hypothetical ejecta that escape Venus afterasteroid impacts, for 10-100 Myr. The latter calculations usetechniques like those of Alvarellos et al. [7] and Zahnle et al. [8]for transfer amongst Jupiter's galilean satellites. Our goals are toestimate the fraction of Atiras that are ejecta launched from Venus,the time spent in space by hypothetical meteorites from Venus, and therate at which such meteorites strike the Earth.[1] Gilmore M., et al (2017). Space Sci. Rev. 212, 1511. [2] JourdanF., Eroglu E. (2017). MAPS 52, 884. [3] Gladman B.J., etal. (1996). Science 271, 1387. [4] Masi G. (2003). Icarus 163,389. [5] Greenstreet S., Ngo H., Gladman B. (2012). Icarus 217,355. [6] Ribeiro A.O., et al. (2016). MNRAS 458, 4471. [7] Alvarellos,J.L., et al. (2008). Icarus 194, 636. [8] Zahnle, K., etal. (2008). Icarus 194, 660.

76 FR 55070 - Government-Owned Inventions; Availability for Licensing

Federal Register 2010, 2011, 2012, 2013, 2014

2011-09-06

...). Publications: 1. Robbins JB, et al. Synthesis, characterization, and immunogenicity in mice of Shigella sonnei O-specific oligosaccharide- core-protein conjugates. Proc Natl Acad Sci U S A. 2009 May 12;106(19...

Reconstruction of the Exposure Histories of 20 Allan Hills Ordinary Chondrites on the Basis of Cosmogenic 10Be, 26Al, Noble Gases, and Cosmic Ray Tracks

NASA Astrophysics Data System (ADS)

Neupert, U.; Knauer, M.; Michel, R.; Loeken, Th.; Schultz, L.; Dittrich-Hannen, B.; Suter, M.; Kubik, P. W.; Metzler, K.; Romstedt, J.

1995-09-01

Twenty ordinary chondrites from the 1988/89 meteorite search (ALH 88004, 88008, 88010, 88011, 88013, 88016 to 88021, 88026 to 88031, 88033, 88039, 88042) [1,2] were investigated for 10Be and 26Al, and for He, Ne and Ar by accelerator and rare gas mass spectrometry, respectively. Cosmic ray tracks were measured in samples of ALH 88019. Using theoretical production rates calculated by a physical model [3] the experimental data are interpreted with respect to the reconstruction of the preatmospheric exposure conditions and exposure histories of the meteoroids. Ordinary chondrites are particularly well suited to exemplify the capabilities of an interpretation of many cosmogenic nuclides measured in one sample. Model calculations of GCR production rates were performed for 10Be, 26Al, 3He, 21Ne, 22Ne and 38Ar as reported elsewhere [4,5]. For all meteorites, except for ALH 88019, the cosmogenic nuclide data can be explained by simple one stage exposure histories between 3 Ma and 44 Ma in meteoroids with radii between 5 cm and 85 cm. Exposure ages were derived from cosmogenic 3He, 21Ne and 38Ar on the basis of the theoretical production rates as function of3He/21Ne and 22Ne/21Ne as well as on the empirical ones proposed by Eugster [6]. The average ratios of exposure ages determined from theoretical production rates to those calculated according to Eugster [6] were 1.08+/-0.11, 1.11+/-0.25 and 1.12+/-0.17 in case of 3He, 21Ne and 38Ar, respectively. Repeated measurements of 10Be and 26Al in ALH 88019 resulted in 10.4+/-1.3 dpm/kg and 5.6+/-0.5 dpm/kg, respectively. But, the cosmogenic rare gas concentrations point to a (single stage) exposure age of 39 Ma in a meteoroid. This is in accordance with a measured cosmic ray track density in olivine of 2.8 * 10^6 cm^-2. The samples are from depths betwen 3 cm and 8 cm. Based on the track data we obtain a minimum meteoroid radius of 8 cm. The low 10Be and 26Al cannot be explained by a one stage exposure history and a long terrestrial age. Possible other exposure scenarios are discussed. Using the theoretical 10Be production rates and the 3He/21Ne and 22Ne/21Ne ratios, constraints about the sizes of the meteoroids and about the shielding depths in the samples were derived. 26Al was not used for this purpose since in four meteorites it is evidently affected by SCR production and since, generally, it could be changed due to long terrestrial residence times. However, most of the observed 26Al concentrations which are not affected by SCR production are consistent within experimental uncertainties with the expected GCR production rates. Substantial terrestrial age are proposed for ALH 88008, ALH 88029 and ALH 88030. Pairing among the investigated meteorites is discussed on the basis of rare gas data, 10Be and 26Al, and NTL data by Benoit et al. [7,8]. It can be concluded that the 20 meteorites result from at least 16 different falls. Acknowledgement: This work was supported by the Deutsche Forschungsgemeinschaft and the Swiss National Science Foundation. References: [1] Meteoritical Bulletin (1990) Meteoritics, 25, 237. [2] Meteoritical Bulletin (1991) Meteoritics, 26, 68. [3] Michel R. et al. (1991) Meteoritics, 26, 221-242. [4] Michel R. et al. (1995) Planet. Space Sci., in press. [5] Herpers U. et al. (1995) Planet. Space Sci., in press. [6] Eugster O. (1988) GCA, 52, 1649-1662. [7] Benoit P. H. et al. (1991) Meteoritics, 26, 262. [8] Benoit P. H. et al. (1992) Meteoritics, 27, 110.

Effects of Silver and Other Metals on the Cytoskeleton

NASA Technical Reports Server (NTRS)

Conrad, Gary W.

1997-01-01

Directly or indirectly, trace concentrations of silver ion (Ag(+)) stabilize microtubules (Conrad, A.H., et al. Cell Motil. & Cytoskel. 27:117-132), as does taxol (Conrad, A.H., et al. J. Exp. Zool. 262:154-165), an effect with major consequences for cellular shape changes and development. Polymerization of microtubules is gravity-sensitive (Tabony and Job, Proc. Natl. Acad. Sci. USA 89:6948-6952), so trace amounts of Ag(+) may alter cellular ability to respond to gravity. If Ag electrolysis is used to purify water on NASA space vehicles, plants and animals/astronauts will be exposed continuously to Ag(+), a regimen with unknown cellular and developmental consequences. Fertilized eggs of the marine mudsnail, Ilyanassa obsoleta, are the cells in which the effects of A(+) on microtubules were discovered. They distribute visible cytoplasmic contents according to gravity and contain cytoplasmic morphogenetic determinants for heart development. The objectives are to determine if the effects of Ag(+), AU(3+), (of biosensor relevance), or Gd(3+) (inhibitor of some stretch-activated ion channels) on the cytoskeleton (in the presence and absence of mechanical loading) will affect cellular responses to gravity.

Resistive sensitivity functions for van der Pauw astroid and rounded crosses and cloverleafs

NASA Astrophysics Data System (ADS)

Koon, Daniel; Hansen, Ole

2014-03-01

We have calculated the sensitivity of van der Pauw resistances to local resistive variations for circular, square and astroid discs of infinitesimal thickness, as well as for the families of rounded crosses and cloverleafs, as a function of specimen parameters, using the direct formulas of our recent paper (Koon et al. 2013 J. Appl. Phys.114 163710) applied to ``reciprocally dual geometries'' (swapped Dirichlet and Neumann boundary conditions) described by Mareš et al.(2012 Meas. Sci. Technol. 23 045004). These results show that (a) the product of any such sensitivity function times differential area, and thus (b) the ratio of any two sensitivities, is invariant under conformal mapping, allowing for the pointwise determination of the conformal mapping function. The family of rounded crosses, which is bounded in parameter space by the square, the astroid and an ``infinitesimally thin'' cross, seems to represent the best geometry for focusing transport measurements on the center of the specimen while minimizing errors due to edge- or contact-effects. Made possible by an SLU Faculty research grant.

Rapid Repairs: Surface Preparation of Ti-3 Al-2.5V Alloy Tubes by Fiber Laser and Welding

DTIC Science & Technology

2008-11-01

processing of titanium 6Al - 4V alloy for potential aerospace component cleaning application, Appl Surf Sci 2005;247:623-630. [11] Turner MW, Crouse...Debroy T, Heat transfer and fluid flow during keyhole mode laser welding of tantalum, Ti- 6Al - 4V , 304 Stainless Steel and Vanadium, J Phy D : Appl Phy...14Titanium alloys are used extensively in aerospace applications mainly due to their superior strength to weight ratio. Different grades of titanium

Major depressive disorder and factorial dimensions among individuals with recent-onset spinal cord injury.

PubMed

Williamson, Meredith L C; Elliott, Timothy R

2013-02-01

We examine the rates of major depressive disorder, single episode determined by the Inventory to Diagnose Depression (IDD) in a clinical sample of persons with recent-onset spinal cord injury (SCI; ≤52 weeks) participating in an inpatient SCI rehabilitation program. We also analyzed the factor structure of the IDD measure in an attempt to replicate the factor structure reported by Frank et al. (1992), and we examined item endorsement patterns. A retrospective chart review was conducted. Participants were 354 individuals (93 women, 261 men) in an inpatient SCI rehabilitation program. Fifteen percent of the sample met criteria for a major depressive disorder (MDD). A higher rate of depression was observed among women. A "dysphoria" factor accounted for 24% of the variance in the final four-factor model. The four-factor solution explained a total of 35.5% of the variance, with an "anhedonia" factor contributing 4.6%, a "sleep" factor contributing 3.5%, and an "appetite" factor contributing 3.5%, respectively. Items assessing symptoms of insomnia, weight loss, worrying about health, and decreased energy had the highest percentage of endorsement to meet Diagnostic and Statistical Manual of Mental Disorders, Fourth Edition, Text Revision (DSM-IV-TR) criteria for clinical significance. The rate of single episodes of MDD determined by the IDD parallels the rate observed with the Patient Health Questionnaire-9 (PHQ-9). The factor structure of the IDD was similar to that reported by Frank et al. (1992). Information provided by the IDD about the presence and severity of MDD symptoms can inform interventions for persons with SCI.

Electrolytic Transformation of Hexyhydro-1,3,5-Trinitro-1,3,5-Triazine (RDX) and 2,4,6-Trinitrotoluene (TNT) in Aqueous Solutions

DTIC Science & Technology

2005-08-01

several years (Bunce et al. 1997; de Lima Leite et al. 2003; Panizza and Cerisola 2004). Treatment is achieved by either oxidation (anodic) or reduction...Hexahydro-1,3,5-trinitro- 1,3,5-triazine mineralization by zerovalent iron and mixed anaerobic cultures,” Environ. Sci. Technol. 35, 4341-4346. Panizza

Electrolytic Transformation of Hexahydro-1,3,5-Trinitro-1,3,5-Triazine (RDX) and 2,4,6-Trintrotoluene (TNT) in Aqueous Solutions

DTIC Science & Technology

2005-08-01

several years (Bunce et al. 1997; de Lima Leite et al. 2003; Panizza and Cerisola 2004). Treatment is achieved by either oxidation (anodic) or reduction...Hexahydro-1,3,5-trinitro- 1,3,5-triazine mineralization by zerovalent iron and mixed anaerobic cultures,” Environ. Sci. Technol. 35, 4341-4346. Panizza

Manufacturable Tri-Stack AlSb/InAs HEMT Low-Noise Amplifiers Using Wafer-Level-Packaging Technology for Light-Weight and Ultralow-Power Applications

DTIC Science & Technology

2009-05-01

shown in Fig. 1 was grown by molecular - beam epitaxy (MBE) on 3-inch semi-insulating GaAs substrates. AlGaSb was used as a buffer. AlSb was used as... beam epitaxy for low-power applications,” J. Vac. Sci. Technol. B. 24, pp. 2581-2585, 2006. [12] Y. C. Chou, L. J. Lee, J. M. Yang, M. D. Lange, P...passivation AlGaSb buffer Figure 1: Cross section of an AlSb/InAs HEMT device on a 3-inch GaAs substrate. The interface region between the

The gap of the area-weighted Motzkin spin chain is exponentially small

NASA Astrophysics Data System (ADS)

Levine, Lionel; Movassagh, Ramis

2017-06-01

We prove that the energy gap of the model proposed by Zhang et al (2016 arXiv:1606.07795) is exponentially small in the square of the system size. In Movassagh and Shor (2016 Proc. Natl Acad. Sci. USA) a class of exactly solvable quantum spin chain models was proposed that have integer spins (s), with a nearest neighbors Hamiltonian, and a unique ground state. The ground state can be seen as a uniform superposition of all s-colored Motzkin walks. The half-chain entanglement entropy provably violates the area law by a square root factor in the system’s size (˜\\sqrt{n} ) for s  >  1. For s  =  1, the violation is logarithmic (Bravyi et al 2012 Phys. Rev. Lett. 109 207202). Moreover in Movassagh and Shor (2016 Proc. Natl Acad. Sci. USA) it was proved that the gap vanishes polynomially and is O(n -c ) with c≥slant2 . Recently, a deformation of Movassagh and Shor (2016 Proc. Natl Acad. Sci. USA), which we call ‘weighted Motzkin quantum spin chain’ was proposed Zhang et al (2016 arXiv:1606.07795). This model has a unique ground state that is a superposition of the s-colored Motzkin walks weighted by tarea\\{Motzkin walk\\} with t  >  1. The most surprising feature of this model is that it violates the area law by a factor of n. Here we prove that the gap of this model is upper bounded by 8ns t-n2/3 for t  >  1 and s  >  1.

Halogen content in Lesser Antilles arc volcanic rocks : exploring subduction recycling

NASA Astrophysics Data System (ADS)

Thierry, Pauline; Villemant, Benoit; Caron, Benoit

2016-04-01

Halogens (F, Cl, Br and I) are strongly reactive volatile elements which can be used as tracers of igneous processes, through mantle melting, magma differentiation and degassing or crustal material recycling into mantle at subduction zones. Cl, Br and I are higly incompatible during partial melting or fractional cristallization and strongly depleted in melts by H2O degassing, which means that no Cl-Br-I fractionation is expected through magmatic differenciation [current thesis]. Thus, Cl/Br/I ratios in lavas reflect the halogen content of their mantle sources. Whereas these ratios seemed quite constant (e.g. Cl/Br =300 as seawater), recent works suggest significant variations in arc volcanism [1,2]. In this work we provide high-precision halogen measurements in volcanic rocks from the recent activity of the Lesser Antilles arc (Montserrat, Martinique, Guadeloupe, Dominique). Halogen contents of powdered samples were determined through extraction in solution by pyrohydrolysis and analysed by Ion Chromatography for F and Cl and high performance ICP-MS (Agilent 8800 Tripe Quad) for Cl, Br and I [3,4]. We show that lavas - and mantle sources - display significant vraiations in Cl/Br/I ratios along the Lesser Antilles arc. These variations are compared with Pb, Nd and Sr isotopes and fluid-mobile elements (Ba, U, Sr, Pb etc.) compositions which vary along the arc from a nothern ordinary arc compositions to a southern 'crustal-like' composition [5,6]. These characteristics are attributed to subducted sediments recycling into the mantle wedge, whose contribution vary along the arc from north to south [7,8]. The proportion of added sediments is also related to the distance to the trench as sediment melting and slab dehydration may occur depending on the slab depth [9]. Further Cl-Br-I in situ measurements by LA-ICP-MS in Lesser Antilles arc lavas melt inclusions will be performed, in order to provide better constraints on the deep halogen recycling cycle from crust to mantle. 1. Villemant, B., Mouatt, J. & Michel, A., 2008. Earth Planet. Sci. Lett. 269(1), 212-229. 2. Kutterolf, S. et al., 2015. Earth Planet. Sci. Lett. 429, 234-246. 3. Michel, A. & Villemant, B., 2003. Geostand. Geoanalytical Res. 27(2), 163-171. 4. Balcone-Boissard, H., Michel, A. & Villemant, B., 2009. Geostand. Geoanalytical Res. 33(4), 477-485. 5. White, W. M. & Dupré, B., 1986. J. Geophys. Res. 91(B6), 5927. 6. Labanieh, S. et al., 2010. Earth Planet. Sci. Lett. 298(1-2), 35-46. 7. Turner, S. et al., 1996. Earth Planet. Sci. Lett. 142(1-2), 191-207. 8. Carpentier, M., Chauvel, C. & Mattielli, N., 2008. Earth Planet. Sci. Lett. 272(1-2), 199-211. 9. Labanieh, S. et al., 2012. J. Petrol. 53(12), 2441-2464.

Mars Analog Mission: Glacier Simulation AMADEE-15 by Austrian Space Forum

NASA Astrophysics Data System (ADS)

Groemer, Gernot; Losiak, Anna; Soucek, Alexander; Plank, Clemens; Zanardini, Laura; Sejkora, Nina; Sams, Sebastian

2016-04-01

Austrian Space Forum: The Austrian Space Forum (OeWF, Österreichisches Weltraum Forum) is a non-profit, citizen-science organization of aerospace specialists and enthusiasts. One of its specialisations is Mars analog research. Analog studies and analog instrument validation supported all planetary surface missions so far [1] and are considered as an effective tool to prepare for future missions to Mars [2,3,4,5,6,7]. Since 2006, OeWF has conducted 11 Mars analog field campaigns in diverse locations that represented: 1) average current Mars conditions (the Mars Desert Research Station (MDRS) in Utah in 2006 [8] and the Northern Sahara near Erfoud, Morocco in 2013 [9]); 2) the early and wet Mars (analog site of Rio Tinto Spain in 2011 [10]); and 3) subsurface exploration (Dachstein Ice Caves in 2012). During these campaigns, 68 experiments and major engineering tests were performed, whichwere mostly focused on astrobiology, robotics, human factors, geoscience and spacesuit operations. Major assets of OeWF include two advanced spacesuit simulators Aouda [11], an increasingly evolving Mission Support Center, a dedicated Remote Science Support team [12], and a growing set of Standard Operating Procedures defining major workflows within a mission team. The spacesuit simulators were operated by a total of 18 analog astronauts, who were selected and trained during a >6 month program. Total EVA time is nearly 600 hours, leading to a significant experience in analog field simulations. AMADEE-15: The mission took place between August 2nd and 14th 2015 at the Kaunertal Glacier in Tyrol, Austria. This glacier was selected as a study site because of its accessibility and high number of micro-landscapes analogous to those expected on Mars in locations where abundant water ice is present. As such it is considered a first-tier Mars analog [13]. The Base station was located at N 46.86320, E 10.71401 at 2800 masl, the highest reached location was on elevation of 2887 m. Eleven experiments were conducted by a field crew at the test site under simulated Martian surface exploration conditions, coordinated by the Mission Support Center in Innsbruck, Austria. A 10-minute satellite communication delay and other limitations pertinent to human planetary surface activities were introduced. A detailed description of the mission should be soon published in [14]. References: [1] Preston & Dartnell 2014. Int. J. Astrobiol. 13:81-98. [2] Drake et al. 2009. NASA-SP-2009-566.pdf. [3] Ross et al. 2013. Act. Astronaut. 90:182-202. [4] Abercromby et al. 2013. Act. Astronaut. 91:34-48. [5] Binstead et al. 2015. Human Research Program Investigators Workshop. [6] Imhof et al. 2015. AIAA SPACE 2015 Conference and Exposition. [7] Bessone et al. 2015. 10.1007/978-3-319-15982-9_37. [8] Groemer et al. 2007. AustroMars Sci. Worksh.:4-12. [9] Groemer et al. 2014. Astrobiol. 14:360-376. [10] Orgel et al. 2013. Act. Astronaut. 94:736-748. [11] Groemer et al. 2012. Astrobiol. 12(2):125-134. [12] Losiak et al. 2014. Astrobiol. 14:417-430. [13] Soare et al. 2001. EOS82, 501. [14] Gernot et al. 2016. Act. Astronaut. (in review).

Determining the Magnitude of Neutron and Galactic Cosmic Ray (GCR) Fluxes at the Moon using the Lunar Exploration Neutron Detector during the Historic Space-Age Era of High GCR Flux

NASA Astrophysics Data System (ADS)

Chin, G.; Sagdeev, R.; Boynton, W. V.; Mitrofanov, I. G.; Milikh, G. M.; Su, J. J.; Livengood, T. A.; McClanahan, T. P.; Evans, L.; Starr, R. D.; litvak, M. L.; Sanin, A.

2013-12-01

The Lunar Reconnaissance Orbiter (LRO) was launched June 18, 2009 during an historic space-age era of minimum solar activity [1]. The lack of solar sunspot activity signaled a complex set of heliospheric phenomena [2,3,4] that also gave rise to a period of unprecedentedly high Galactic Cosmic Ray (GCR) flux [5]. These events coincided with the primary mission of the Lunar Exploration Neutron Detector (LEND, [6]), onboard LRO in a nominal 50-km circular orbit of the Moon [7]. Methods to calculate the emergent neutron albedo population using Monte Carlo techniques [8] rely on an estimate of the GCR flux and spectra calibrated at differing periods of solar activity [9,10,11]. Estimating the actual GCR flux at the Moon during the LEND's initial period of operation requires a correction using a model-dependent heliospheric transport modulation parameter [12] to adjust the GCR flux appropriate to this unique solar cycle. These corrections have inherent uncertainties depending on model details [13]. Precisely determining the absolute neutron and GCR fluxes is especially important in understanding the emergent lunar neutrons measured by LEND and subsequently in estimating the hydrogen/water content in the lunar regolith [6]. LEND is constructed with a set of neutron detectors to meet differing purposes [6]. Specifically there are two sets of detector systems that measure the flux of epithermal neutrons: a) the uncollimated Sensor for Epi-Thermal Neutrons (SETN) and b) the Collimated Sensor for Epi-Thermal Neutrons (CSETN). LEND SETN and CSETN observations form a complementary set of simultaneous measurements that determine the absolute scale of emergent lunar neutron flux in an unambiguous fashion and without the need for correcting to differing solar-cycle conditions. LEND measurements are combined with a detailed understanding of the sources of instrumental back-ground, and the performance of CSETN and SETN. This comparison allows us to calculate a constant scale factor that determines the absolute flux of neutrons at the Moon and then subsequently to deduce the proper scale of the GCR flux. References: [1] H. S. Ahluwakia and R. C. Ygbuhay (2010) Twelfth International Solar Wind Conference, 699-702. [2] F. B. McDonald et al. (2010) JRL, 37, L18101. [3] H. Moraal and P. H. Stoker (2010) JGR, 115, 12109-12118. [4] R. Kataoka et al. (2012) Space Weather, 10, 11001-11007. [4] C-L. Huang et al. (2009), JRL, 37, L09109-L09104. [5] R. A. Mewaldt et al. (2010) Ap. J Lett., 723, L1-L6. [6] I. G. Mitrofanov et al. (2010) Space Science Rev., 150, 283-207. [7] C. R. Tooley et al. (2010) Space Science Rev., 150, 23-62. [8] G. W. McKinney et al. (2006) JGR, 111, 6004-6018. [9] P. M. O'Neil (2010) IEEE Trans. Nucl. Sci., 57(6), 3148-3153. [10] American National Standards Institute Tech. Rep. ISO 15390 (2004). [11] I. G. Usokin et al. (2008) JGR, 110, A12108. [12] M. D. Looper et al. (2013) Space Weather, 11, 142-152. [13] A. I. Mrigakshi et al. (2012) JGR, 117, A08109-A08121.

Chemical Bonding, Interdiffusion and Electronic Structure at InP, GaAs, and Si-Metal Interfaces.

DTIC Science & Technology

1985-10-01

4. H.H. Wieder, J. Vac. Sci. Technol. 15, 1498 (1978). C. 5. W.E. Spicer, 1. Lindau, P. Skeath, C.Y. Su, and P. Chye , Phys. Rev. Lett. 44, 10 420...Spicer, Solid State Electron. 28 307 (1985). 25. N. Newman, K.K. Chin , W.G. Petro, T. Kendelewicz, M.D. Williams, C.E. McCants, and W.E. Spicer, J. Vac...Technol. 19, 661 (1981). 11. Y. Shapira, L.J. Brillson and A. Heller, J. Vac. Sci. U Technol., Al, 766 (1983). 12. P.W. Chye , I. Lindau, P. Pianetta, C.M

Municipal solid waste and dung cake burning: discoloring the Taj Mahal and human health impacts in Agra

NASA Astrophysics Data System (ADS)

Lal, Raj M.; Nagpure, Ajay S.; Luo, Lina; Tripathi, Sachchida N.; Ramaswami, Anu; Bergin, Michael H.; Russell, Armistead G.

2016-10-01

The Taj Mahal—an iconic World Heritage monument built of white marble—has become discolored with time, due, in part, to high levels of particulate matter (PM) soiling its surface (Bergin et al 2015 Environ. Sci. Technol. 49 808-812). Such discoloration has required extensive and costly treatment (2015 Two Hundred Sixty Second Report on Effects of Pollution on Taj Parliament of India Rajya Sabha, New Delhi) and despite previous interventions to reduce pollution in its vicinity, the haze and darkening persists (Bergin et al 2015 Environ. Sci. Technol. 49 808-812 2015 Two Hundred Sixty Second Report on Effects of Pollution on Taj Parliament of India Rajya Sabha, New Delhi). PM responsible for the soiling has been attributed to a variety of sources including industrial emissions, vehicular exhaust and biomass burning, but the contribution of the emissions from the burning of open municipal solid waste (MSW) may also play an important role. A recent source apportionment study of fine particulate matter (PM2.5) at the Taj Mahal showed biomass burning emissions, which would include MSW emissions, accounted for nearly 40% of organic matter (OM)—a component of PM—deposition to its surface (Bergin et al 2015 Environ. Sci. Technol. 49 808-812) dung cake burning, used extensively for cooking in the region, was the suggested culprit and banned within the city limits (2015 Two Hundred Sixty Second Report on Effects of Pollution on Taj Parliament of India Rajya Sabha, New Delhi), although the burning of MSW, a ubiquitous practice in the area (Nagpure et al 2015 Environ. Sci. Technol. 49 12904-12), may play a more important role in local air quality. Using spatially detailed emission estimates and air quality modeling, we find that open MSW burning leads to about 150 (±130) mg m-2 yr-1 of PM2.5 being deposited to the surface of the Taj Mahal compared to about 12 (±3.2) mg m-2 yr-1 from dung cake burning. Those two sources, combined, also lead to an estimated 713 (377-1050) premature mortalities in Agra each year, dominated by waste burning in socioeconomically lower status neighborhoods. An effective MSW management strategy would reduce soiling of the Taj Mahal, improve human health, and have additional aesthetic benefits.

A new version of Scilab software package for the study of dynamical systems

NASA Astrophysics Data System (ADS)

Bordeianu, C. C.; Felea, D.; Beşliu, C.; Jipa, Al.; Grossu, I. V.

2009-11-01

This work presents a new version of a software package for the study of chaotic flows, maps and fractals [1]. The codes were written using Scilab, a software package for numerical computations providing a powerful open computing environment for engineering and scientific applications. It was found that Scilab provides various functions for ordinary differential equation solving, Fast Fourier Transform, autocorrelation, and excellent 2D and 3D graphical capabilities. The chaotic behaviors of the nonlinear dynamics systems were analyzed using phase-space maps, autocorrelation functions, power spectra, Lyapunov exponents and Kolmogorov-Sinai entropy. Various well-known examples are implemented, with the capability of the users inserting their own ODE or iterative equations. New version program summaryProgram title: Chaos v2.0 Catalogue identifier: AEAP_v2_0 Program summary URL:http://cpc.cs.qub.ac.uk/summaries/AEAP_v2_0.html Program obtainable from: CPC Program Library, Queen's University, Belfast, N. Ireland Licensing provisions: Standard CPC licence, http://cpc.cs.qub.ac.uk/licence/licence.html No. of lines in distributed program, including test data, etc.: 1275 No. of bytes in distributed program, including test data, etc.: 7135 Distribution format: tar.gz Programming language: Scilab 5.1.1. Scilab 5.1.1 should be installed before running the program. Information about the installation can be found at http://wiki.scilab.org/howto/install/windows. Computer: PC-compatible running Scilab on MS Windows or Linux Operating system: Windows XP, Linux RAM: below 150 Megabytes Classification: 6.2 Catalogue identifier of previous version: AEAP_v1_0 Journal reference of previous version: Comput. Phys. Comm. 178 (2008) 788 Does the new version supersede the previous version?: Yes Nature of problem: Any physical model containing linear or nonlinear ordinary differential equations (ODE). Solution method: Numerical solving of ordinary differential equations for the study of chaotic flows. The chaotic behavior of the nonlinear dynamical system is analyzed using Poincare sections, phase-space maps, autocorrelation functions, power spectra, Lyapunov exponents and Kolmogorov-Sinai entropies. Numerical solving of iterative equations for the study of maps and fractals. Reasons for new version: The program has been updated to use the new version 5.1.1 of Scilab with new graphical capabilities [2]. Moreover, new use cases have been added which make the handling of the program easier and more efficient. Summary of revisions: A new use case concerning coupled predator-prey models has been added [3]. Three new use cases concerning fractals (Sierpinsky gasket, Barnsley's Fern and Tree) have been added [3]. The graphical user interface (GUI) of the program has been reconstructed to include the new use cases. The program has been updated to use Scilab 5.1.1 with the new graphical capabilities. Additional comments: The program package contains 12 subprograms. interface.sce - the graphical user interface (GUI) that permits the choice of a routine as follows 1.sci - Lorenz dynamical system 2.sci - Chua dynamical system 3.sci - Rosler dynamical system 4.sci - Henon map 5.sci - Lyapunov exponents for Lorenz dynamical system 6.sci - Lyapunov exponent for the logistic map 7.sci - Shannon entropy for the logistic map 8.sci - Coupled predator-prey model 1f.sci - Sierpinsky gasket 2f.sci - Barnsley's Fern 3f.sci - Barnsley's Tree Running time: 10 to 20 seconds for problems that do not involve Lyapunov exponents calculation; 60 to 1000 seconds for problems that involve high orders ODE, Lyapunov exponents calculation and fractals. References: C.C. Bordeianu, C. Besliu, Al. Jipa, D. Felea, I. V. Grossu, Comput. Phys. Comm. 178 (2008) 788. S. Campbell, J.P. Chancelier, R. Nikoukhah, Modeling and Simulation in Scilab/Scicos, Springer, 2006. R.H. Landau, M.J. Paez, C.C. Bordeianu, A Survey of Computational Physics, Introductory Computational Science, Princeton University Press, 2008.

Methods of editing cloud and atmospheric layer affected pixels from satellite data

NASA Technical Reports Server (NTRS)

Nixon, P. R. (Principal Investigator); Wiegand, C. L.; Richardson, A. J.; Johnson, M. P.

1982-01-01

Practical methods of computer screening cloud-contaminated pixels from data of various satellite systems are proposed. Examples are given of the location of clouds and representative landscape features in HCMM spectral space of reflectance (VIS) vs emission (IR). Methods of screening out cloud affected HCMM are discussed. The character of subvisible absorbing-emitting atmospheric layers (subvisible cirrus or SCi) in HCMM data is considered and radiosonde soundings are examined in relation to the presence of SCi. The statistical characteristics of multispectral meteorological satellite data in clear and SCi affected areas are discussed. Examples in TIROS-N and NOAA-7 data from several states and Mexico are presented. The VIS-IR cluster screening method for removing clouds is applied to a 262, 144 pixel HCMM scene from south Texas and northeast Mexico. The SCi that remain after cluster screening are sited out by applying a statistically determined IR limit.

Pits and Gullies on Vesta: Potential Insights from Terrestrial Analogs

NASA Astrophysics Data System (ADS)

Sears, D. W.; Tornabene, L. L.; Osinski, G. R.; Hughes, S. S.; Heldmann, J. L.

2013-12-01

Arguably the most surprising discovery of the Dawn mission during its observations of Vesta were the pitted terrain [1,2], low albedo regions [3,4], and hydrogen abundances [5,6]. The presence of pitted terrain at the floors of craters on Vesta has been ascribed to the release of volatiles during impact, following the discovery of similar features on Mars where they are interpreted as volatile-rich impact melt deposits [7]. The numerous dark regions and the H abundance have been ascribed to the presence of infall material resembling CM chondrites. CM chondrite clasts are relatively common in brecciated meteorites [8], including the HED meteorites that are presumed to have come from Vesta (or Vesta fragments) [9,10], and contain up to about 10 vol% water [11]. On the walls of craters associated with the pitted terrain in craters, but also observed outside craters, are features resembling gullies [12,13]. The nature of these features, the amount of fluids required, and - especially - the relationship between the pits and gully-like features is unclear. Pit-like structures are commonly observed at terrestrial impact craters (hydrothermal pipes, [14]) and in volcanic fields (phreatic craters, [15]) in which water was present during the active phases of these processes. They are usually well-studied and offer a range of 'ground truths' which might help us understand the features on Vesta. The number, morphology, and locations of the features provide temporal information on their histories. The number, size and distribution of boulders around the features, provides information on energetics and water content. We expect such structures to be present in water-bearing C and X asteroids, where the water in endogenous, and S asteroids where, like Vesta, the water is exogenous. Such features, if present, were generally obscured by regolith on Eros [16], but a search in regolith-poor areas might be worthwhile. In summary, we suggest that new insights into volatile behavior on near-Earth asteroids, with its relevance to geological evolution, astrobiology, and space resources, will be possible through the study of terrestrial analogs. [1] Denevi et al 2012. Science 338, 246-249. [2] Boyce et al 2012. Icarus 221 262-275. [3] McCord et al., 2012. Nature 491, 83-86. [4] Reddy et al 2012. Icarus 221 544-559. [5] De Sanctis et al. 2012. Science 336, 697-700. [6] Prettyman et al 2012. Science 338, 242-246. [7] Tornabene et al (2012). Icarus 220, 348-368. [8] Wilkening et al 1973. Geochim. Cosmochim. Acta 37, 1985-1989. [9] McCord et al 1970. Science 168, 1445-1447. [10] Drake 2001. Meteorit. Planet. Sci. 36, 501-513. [11] Wiik 1969. Commun. Phys. Math. 34 135-145 [12] Scully et al 2012. AGU Meeting, 2012, December 3-7th. [13] Scully et al 2013. 44th LPSC paper #1578. [14] Kirsimäe and Osinski 2013. Chapter 6 in 'Impact Cratering: Processes and Products' eds Osinski and Pierazzo, Blackwell. [15] Hughes et al 1999. Pages 143-168 in 'Guidebook to the Geology of Eastern Idaho' eds Hughes and Thackray, Idaho Museum of Natural History. [16] Robinson et al 2001. Meteorit. Planet. Sci. 37, 1651-1684.

Integrating the perspectives of individuals with spinal cord injuries, their family caregivers and healthcare professionals from the time of rehabilitation admission to community reintegration: protocol for a scoping study on SCI needs.

PubMed

Moreno, Alexander; Zidarov, Diana; Raju, Chandhana; Boruff, Jill; Ahmed, Sara

2017-08-04

There is fragmented information about the different needs following a spinal cord injury (SCI). Expressed SCI needs can be met or unmet, they change along the rehabilitation continuum (eg, acute, rehabilitation and reintegration into the community) and can be different for traumatic and non traumatic SCI. The general objective of this scoping study is to evaluate and integrate the needs of individuals with traumatic and non-traumatic SCI, their family caregivers and those reported by rehabilitation professionals from the time of rehabilitation admission to community reintegration. The specific objectives are to: (A) synthesise the needs of individuals with SCI as perceived by themselves, their family caregivers and rehabilitation professionals using two theoretical models, (B) classify needs as met and unmet, (C) explore the evolution of met/unmet needs from the time of rehabilitation admission to community reintegration and (D) provide recommendations to improve SCI care. METHODS AND ANALYSIS: (A) identifying the most frequent met and unmet needs reported by adults with traumatic and non-traumatic SCI, their family caregivers and their rehabilitation professionals from the time of rehabilitation admission to community reintegration; (B) identifying relevant studies with a search in electronic databases; (C) charting the data based on categories refined and adjusted with a stakeholder group; (D) collating, summarising and reporting the results using two analytical frameworks (Maslow's hierarchical model of human needs and the Ferrans et al 's model of health-related quality of life) and (E) a stakeholder consultation phase. The results of this scoping study will allow understanding SCI needs from the time of rehabilitation admission to community reintegration from the perspective of different stakeholders. An integrated master report combining the needs of individuals with SCI from the perspectives of different stakeholders from the time of rehabilitation admission to community reintegration will follow the consultation meetings. © Article author(s) (or their employer(s) unless otherwise stated in the text of the article) 2017. All rights reserved. No commercial use is permitted unless otherwise expressly granted.

Effects of Chronic Alcohol Exposure on Kainate Receptor-Mediated Neurotransmission in the Hippocampus

DTIC Science & Technology

2004-09-01

hippocampus and hypothalamus. J Neurosci Res 63:200-208. Thorpe GH et al. (1989) Chemiluminescent enzyme immunoassay of alpha - fetoprotein based on an...cells. Proc Natl Acad Sci USA 83:6213-6215. Montpied Pet al. (1991) Prolonged ethanol inhalation decreases gamma-aminobutyric acidA receptor alpha ...potentials mediated via alpha -bungarotoxin-sensitive nico- tinic acetylcholine receptors in rat hippocampal interneurons. J Neurosci 18:8228- 8235

SOFIA Science Imagery

NASA Image and Video Library

2017-09-14

SCI2016_0001: SOFIA/GREAT [O I] spectrum at 4.7 THz (63 μm) superimposed on a picture of Mars. Absorption line depth is approximately 10% of the continuum. The abundance of atomic oxygen computed from the data is less than expected from the Forget et al. 1999 global circulation & photochemical model. Credit: SOFIA/GREAT spectrum: NASA/DLR/USRA/DSI/MPIfR/GREAT Consortium/MPIfS/Rezac et al. 2015; Mars image: NASA

A New Family of Schroder's Method and Its Variants Based on Power Means for Multiple Roots of Nonlinear Equations

ERIC Educational Resources Information Center

Kanwar, V.; Sharma, Kapil K.; Behl, Ramandeep

2010-01-01

In this article, we derive one-parameter family of Schroder's method based on Gupta et al.'s (K.C. Gupta, V. Kanwar, and S. Kumar, "A family of ellipse methods for solving non-linear equations", Int. J. Math. Educ. Sci. Technol. 40 (2009), pp. 571-575) family of ellipse methods for the solution of nonlinear equations. Further, we introduce new…

Probing the biocompatibility of MoS2 nanosheets by cytotoxicity assay and electrical impedance spectroscopy

NASA Astrophysics Data System (ADS)

Shah, Pratikkumar; Narayanan, Tharangattu N.; Li, Chen-Zhong; Alwarappan, Subbiah

2015-08-01

Transition metal dichalgogenides such as MoS2 have recently emerged as hot two-dimensional (2D) materials due to their superior electronic and catalytic properties. Recently, we have reported the usefulness of MoS2 nanosheets toward the electrochemical detection of neurotransmitters and glucose (Narayanan et al 2014 Nanotechnology 25 335702). Furthermore, there are reports available in the literature that demonstrate the usefulness of MoS2 nanosheets for biosensing and energy storage applications (Zhu et al 2013 J. Am. Chem. Soc. 135 5998-6001 Pumera and Loo 2014 Trends Anal. Chem. 61 49-53 Lee et al 2014 Sci. Rep. 4 7352; Stephenson et al 2014 Energy Environ. Sci. 7 209-31). Understanding the cytotoxic effect of any material is very important prior to employing them for any in vivo biological applications such as implantable sensors, chips, or carriers for drug delivery and cell imaging purposes. Herein, we report the cytotoxicity of the MoS2 nanosheets based on the cytotoxic assay results and electrical impedance analysis using rat pheochromocytoma cells (PC12) and rat adrenal medulla endothelial cells (RAMEC). Our results indicated that the MoS2 nanosheets synthesized in our work are safe 2D nanosheets for futuristic biomedical applications.

Complex dynamics of a delayed discrete neural network of two nonidentical neurons

DOE Office of Scientific and Technical Information (OSTI.GOV)

Chen, Yuanlong; Huang, Tingwen; Huang, Yu, E-mail: stshyu@mail.sysu.edu.cn

2014-03-15

In this paper, we discover that a delayed discrete Hopfield neural network of two nonidentical neurons with self-connections and no self-connections can demonstrate chaotic behaviors. To this end, we first transform the model, by a novel way, into an equivalent system which has some interesting properties. Then, we identify the chaotic invariant set for this system and show that the dynamics of this system within this set is topologically conjugate to the dynamics of the full shift map with two symbols. This confirms chaos in the sense of Devaney. Our main results generalize the relevant results of Huang and Zoumore » [J. Nonlinear Sci. 15, 291–303 (2005)], Kaslik and Balint [J. Nonlinear Sci. 18, 415–432 (2008)] and Chen et al. [Sci. China Math. 56(9), 1869–1878 (2013)]. We also give some numeric simulations to verify our theoretical results.« less

Complex dynamics of a delayed discrete neural network of two nonidentical neurons.

PubMed

Chen, Yuanlong; Huang, Tingwen; Huang, Yu

2014-03-01

In this paper, we discover that a delayed discrete Hopfield neural network of two nonidentical neurons with self-connections and no self-connections can demonstrate chaotic behaviors. To this end, we first transform the model, by a novel way, into an equivalent system which has some interesting properties. Then, we identify the chaotic invariant set for this system and show that the dynamics of this system within this set is topologically conjugate to the dynamics of the full shift map with two symbols. This confirms chaos in the sense of Devaney. Our main results generalize the relevant results of Huang and Zou [J. Nonlinear Sci. 15, 291-303 (2005)], Kaslik and Balint [J. Nonlinear Sci. 18, 415-432 (2008)] and Chen et al. [Sci. China Math. 56(9), 1869-1878 (2013)]. We also give some numeric simulations to verify our theoretical results.

The Emerging Pathogen Candida auris: Growth Phenotype, Virulence Factors, Activity of Antifungals, and Effect of SCY-078, a Novel Glucan Synthesis Inhibitor, on Growth Morphology and Biofilm Formation.

PubMed

Larkin, Emily; Hager, Christopher; Chandra, Jyotsna; Mukherjee, Pranab K; Retuerto, Mauricio; Salem, Iman; Long, Lisa; Isham, Nancy; Kovanda, Laura; Borroto-Esoda, Katyna; Wring, Steve; Angulo, David; Ghannoum, Mahmoud

2017-05-01

Candida auris , a new multidrug-resistant Candida spp. which is associated with invasive infection and high rates of mortality, has recently emerged. Here, we determined the virulence factors (germination, adherence, biofilm formation, phospholipase and proteinase production) of 16 C. auris isolates and their susceptibilities to 11 drugs belonging to different antifungal classes, including a novel orally bioavailable 1,3-β-d-glucan synthesis inhibitor (SCY-078). We also examined the effect of SCY-078 on the growth, ultrastructure, and biofilm-forming abilities of C. auris Our data showed that while the tested strains did not germinate, they did produce phospholipase and proteinase in a strain-dependent manner and had a significantly reduced ability to adhere and form biofilms compared to that of Candida albicans ( P = 0.01). C. auris isolates demonstrated reduced susceptibility to fluconazole and amphotericin B, while, in general, they were susceptible to the remaining drugs tested. SCY-078 had an MIC 90 of 1 mg/liter against C. auris and caused complete inhibition of the growth of C. auris and C. albicans Scanning electron microscopy analysis showed that SCY-078 interrupted C. auris cell division, with the organism forming abnormal fused fungal cells. Additionally, SCY-078 possessed potent antibiofilm activity, wherein treated biofilms demonstrated significantly reduced metabolic activity and a significantly reduced thickness compared to the untreated control ( P < 0.05 for both comparisons). Our study shows that C. auris expresses several virulence determinants (albeit to a lesser extent than C. albicans ) and is resistant to fluconazole and amphotericin B. SCY-078, the new orally bioavailable antifungal, had potent antifungal/antibiofilm activity against C. auris , indicating that further evaluation of this antifungal is warranted. Copyright © 2017 Larkin et al.

Report from ILEWG and Cape Canaveral Lunar Declaration 2008

NASA Astrophysics Data System (ADS)

Foing, B. H.

2009-04-01

We shall report on the ILEWG charter, goals and activities, on ICEUM "lunar declarations" and follow-up activities, with focus on societal questions, and the Cape Canaveral Lunar Declaration 2008. ILEWG charter: ILEWG , the International Lunar Exploration Working Group is a public forum created in 1994, sponsored by the world's space agencies to support "international cooperation towards a world strategy for the exploration and utilization of the Moon - our natural satellite". The charter of ILEWG is: - To develop an international strategy for the exploration of the Moon - To establish a forum and mechanisms for the communication and coordination of activities - To implement international coordination and cooperation - In order to facilitate communication among all interested parties ILEWG agrees to establish an electronic communication network for exchange of science, technology and programmatic information related to lunar activities ILEWG meets regularly, at least, once a year, and leads the organization of an International Conference in order to discuss the state of lunar exploration. Formal reports are given at COSPAR meetings and to space agencies. ILEWG is sponsored by the world's space agencies and is intended to serve three relevant groups: - actual members of the ILEWG, ie delegates and repre-sentatives of the participating Space Agencies and organizations - allowing them to discuss and possibly harmonize their draft concepts and plans - team members of the relevant space projects - allowing them to coordinate their internal work according to the guidelines provided by the Charter of the ILEWG - members of the general public and of the Lunar Explorer's Society who are interested and wish to be informed on the progress of the Moon projects and possibly contribute their own ideas ILEWG activities and working groups: ILEWG task groups include science, technology, human aspects, socio-economics, young explorers and outreach, programmatics, roadmaps and synergies with Mars exploration. Users can obtain information on how to participate, as well as details on the latest news and events regarding lunar exploration, forthcoming meetings, relevant reports and documents of importance for the work of the ILEWG, summary descriptions of current lunar exploration projects (such as SMART-1, Chang'E1, Selene, Chandrayaan-1, LRO, LCROSS) funded by various space agencies, and basic data on the Moon itself. Activities of the related space agencies and organizations can also be found. ILEWG has been organising International Conferences on Exploration and Utilisation of the Moon (ICEUM) since 1994, whose proceedings are published. It has also sponsored a number of activities, workshops, tasks groups and publications in collabora-tions with other organisations: COSPAR, space agencies, IAA, IAF, EGU (see references below). In accor-dance with its charter, ILEWG reports to COSPAR, and a summary was given at Montreal COSPAR2008 on ILEWG activities conducted since the previous COSPAR2006 assembly in Beijing. The recent ILEWG International Conference on Exploration and Utilisation of the Moon, were held respectively in Udaipur, India (ICEUM6, 2004), in Toronto, Canada (ICEUM7, 2005), in Beijing (ICEUM8, 2006), Sorrento (ICEUM9, 2007) and Port Canaveral (ICEUM10/LEAG/SRR, 2008 in conjunction with the NASA Lunar Exploration Analysis Groups and Space Resources Roundtable annual meetings). We'll report on the Cape Canaveral Lunar Declaration and on follow-up activities, in particular in coordination with space agencies, COSPAR and IAF. References: [1] 1st International Lunar Workshop, Balsiger H. et al., Editors, European Space Agency, 1994. ESA-SP-1170. [2] 2nd International Lunar Workshop, Kyoto, H. Mizutani, editor, Japan Space Forum Publisher, 1997. [3] 3rd International Lunar Workshop, Moscow 1998, E. Galimov, editor. [4] ICEUM4, ESTEC, 2000, ESA SP-462, B.H. Foing & M. Perry, editors. [5] ICEUM5, Hawaii Nov 2003, Durst S.M. et al, Editors, Vol 108, 1-576 pp, Science and Technology Series, American Astronautical Society, 2004. [6] ICEUM6, Udaipur 2004, Bhandari N., Editor, Journal Earth System Science, India, 114, No6, Dec 2005, pp. 573-841. [7] ICEUM7, Toronto Sept 2005, sci.esa.int/ilewg. [8] ICEUM8, Beijing July 2006, Journal of Chinese Society of Astronautics, Vol. 28 Sup., 2007, Ji W., Editor. [9] ICEUM9, Sorrento, Italy, Foing B., Espinasse S., Kosters G., Editors. http://sci.esa.int/iceum9, Dec. 2007), [11] Ehrenfreund, P., Foing, B.H., Cellino, A. Editors, The Moon and Near Earth Objects, ASR Vol 37, 1, 2006. [12] Foing, B.H. et al editors, 'Astronomy and Space Science from the Moon', ASR 14, 6, 1994. [13] Foing, B.H. et al, editor, Lunar Exploration, Planetary and Space Science, Vol 50, 14-15, 2002. [14] Foing, B.H., Heather, D. editors, 'Lunar Exploration 2000', ASR Vol 30, Nr 8, 2002. [15] Hunt-ress, W. et al 'The next steps in exploring deep space - A cosmic study by the IAA', Acta Astronautica, Vol 58, Issues 6-7, 2006, p302-377. [16] Ip W.-H., Foing, B.H., Masson Ph.L., editors, The Moon and Mars, ASR Vol 23, 11, 1999.

The Role of Microstructural Variability on the Very High-Cycle Fatigue Behavior of Discontinuously-Reinforced Aluminum Metal Matrix Composites using Ultrasonic Fatigue (Preprint)

DTIC Science & Technology

2008-05-01

controlled processing. Bhanu-Prasad et al .37 conducted a systematic study of PM-processed 2124/SiC/30p aluminum composites 4 5 in which matrix alloy...Mater., 27, 173-178. [5] Wang A, Rack HJ (1991). Transition wear behavior of SiC-particulate- and SiC- whisker-reinforced 7091 Al metal matrix...modeling of particle distribution effects on fatigue in Al -SiCp composites. Mater. Sci. Eng. A, Struct. Mater. Prop. Microstruct. Process., 300, 113-124

The Shoreline Vegetation of Lake Oahe a Man Made Fluctuating Water Level Reservoir of the Upper Missouri River Basin.

DTIC Science & Technology

1973-06-01

VANDERVEEN ET AL . UNCLASSIFIED 01 JUN 73 DACW45-73-C-0002 F/G 6/6. NL mmmmmmmmIIIIIIIIIIIIIu IIEIIIEEIIIIEE EEIIIIIIIIIEEE IIIIIIIIIIIIIIfl L 2. i~iIi...fluctuation to be the most impor- tant factor affecting vegetation along reservoir shorelines. Hall et al . (1946) studied reservoirs in the Tennessee Valley...Hall, T. F. et al . 1946. Water level relationships of plants in the Tennessee valley. Tenn. Acad. Sci. 10: 18-60. Houston, W. R. 1960. Effects of water

Constraints on Lunar Heat Flow Rates from Diviner Lunar Radiometer Polar Observations

NASA Astrophysics Data System (ADS)

Paige, D. A.; Siegler, M. A.; Vasavada, A. R.

2010-12-01

The heat flow rate from the lunar interior is a fundamental property of the moon that is related to its composition, interior structure and history. Lunar heat flow rates have been measured at the Apollo 15 and 17 landing sites [1], but it is widely believed that the measured values of 0.021 Wm-2 and 0.016 Wm-2 respectively may not be representative of the moon as a whole due to the presence of enhanced radiogenic elements at these landing sites [2]. The Diviner Lunar Radiometer Experiment on the Lunar Reconnaissance Orbiter [3] has acquired an extensive set of thermal emission from the lunar surface at infrared wavelengths, including the first radiometric measurements of surface temperatures at the lunar poles [4]. Due to its low obliquity and rough topography, the moon has extensive cryogenic regions at high latitudes that never receive direct sunlight. The temperatures of the coldest of these regions can be used to place upper limits on the heat flow rate from the lunar interior because if other heat sources are neglected, then surface thermal emission is balanced by heat flow from warmer lunar interior [5]. Diviner has mapped the north and south polar regions over a complete annual cycle and we have identified a 4 km2 area within Hermite Crater in the north polar region that has a winter season nighttime Channel 9 (100-400 micron) brightness temperatures in of less than 20K. These low temperatures would imply a lunar heat flow rate of less than 0.010 Wm-2, which may be consistent with expectations for regions of the moon that do not contain enhanced concentrations of radiogenic elements [2,6], as is the case for the north polar region of the moon [7]. [1] Langseth, M. G. et al, Proc. Lunar Sci. Conf, 7th, 3143-3171, 1976. [2] Warren, P. H. and K. K. L. Rasmussen, JGR 92, 3453-3465, 1987. [3] Paige, D. A. et al, Space Sci. Rev, 150:125-160, 2010. [4] Paige, D. A. et al., Science, in press, 2010. [5] Watson, K. JGR 72, 3301-3302, 1967. [6] Wieczorek, M. A. and R. J. Phillips, JGR 105, 20,417-20,430, 2000. [7] Lawrence, D. J. et al., Scence 281, 1484-1489, 1998.

Mid-infrared spectroscopy to better characterize icy moon surface compositions

NASA Astrophysics Data System (ADS)

Young, Cindy L.; Wray, James J.; Hand, Kevin P.; Poston, Michael; Carlson, Robert W.; Clark, Roger Nelson; Spencer, John R.; Jennings, Donald

2016-10-01

Previous spectroscopy work on icy moons has focused primarily on the visible and near-IR portion of the spectrum due to challenges presented by a low signal to noise ratio at the longer wavelengths. However, the mid-IR is the region of the strongest fundamental vibrations of many important types of molecules (e.g., organics) and has the potential to reveal unique compositional information [1]. We use the wealth of data that is now available from Cassini's Composite Infrared Spectrometer (CIRS) to average spectra over similar regions to improve the signal to noise, helping to reveal spectral features never before observed.Our initial work has already led to the detection and tentative laboratory identification of the first spectral features observed for any icy moon in the mid-IR [2]. On Iapetus' dark terrain, we found an emissivity feature at ~855 cm-1 and a possible doublet at 660 and 690 cm-1 that does not correspond to any known instrument artifacts. We attributed the 855 cm-1 feature to fine-grained silicates, similar to those found in dust on Mars and in meteorites, which are nearly featureless at shorter wavelengths [e.g., 3, 4]. Silicates on the dark terrains of Saturn's icy moons have been suspected for decades, but there have been no definitive detections until this work.We measured the vacuum, low temperature mid-IR spectra of various fine-grained powdered silicates, including Mg-rich serpentines, often present in meteorites. Some of these materials do have emissivity features near 855 cm-1 and exhibit a doublet. Presently, we are continuing to comb the CIRS icy moon database for spectral features (particularly focusing on the warmer surfaces in the Saturn system) and are performing further vacuum chamber measurements to experiment with more sample types and ice/sample mixtures to determine the impacts of changing conditions in the chamber on features. We are also working to understand how surface porosity and mixing with various darkening agents may impact our spectra.[1] Flasar, F. M., et al. (2004), Space Sci Rev, 115, 169.[2] Young, C. L., et al. (2015), ApJ Lett., 811, L27.[3] Christensen, P. R., et al. (2004), Sci, 306, 1733.[4] McAdam, M. M., et al. (2015), Icar, 245, 320.

Development of a Short-Form Measure of Science and Technology Self-efficacy Using Rasch Analysis

NASA Astrophysics Data System (ADS)

Lamb, Richard L.; Vallett, David; Annetta, Leonard

2014-10-01

Despite an increased focus on science, technology, engineering, and mathematics (STEM) in U.S. schools, today's students often struggle to maintain adequate performance in these fields compared with students in other countries (Cheek in Thinking constructively about science, technology, and society education. State University of New York, Albany, 1992; Enyedy and Goldberg 2004; Mandinach and Lewis 2006). In addition, despite considerable pressure to promote the placement of students into STEM career fields, U.S. placement is relatively low (Sadler et al. in Sci Educ 96(3):411-427, 2012; Subotnik et al. in Identifying and developing talent in science, technology, engineering, and mathematics (STEM): an agenda for research, policy and practice. International handbook, part XII, pp 1313-1326, 2009). One explanation for the decline of STEM career placement in the U.S. rests with low student affect concerning STEM concepts and related content, especially in terms of self-efficacy. Researchers define self-efficacy as the internal belief that a student can succeed in learning, and that understanding student success lies in students' externalized actions or behaviors (Bandura in Psychol Rev 84(2):191-215, 1977). Evidence suggests that high self-efficacy in STEM can result in student selection of STEM in later educational endeavors, culminating in STEM career selection (Zeldin et al. in J Res Sci Teach 45(9):1036-1058, 2007). However, other factors such as proficiency play a role as well. The lack of appropriate measures of self-efficacy can greatly affect STEM career selection due to inadequate targeting of this affective trait and loss of opportunity for early intervention by educators. Lack of early intervention decreases selection of STEM courses and careers (Valla and Williams in J Women Minor Sci Eng 18(1), 2012; Lent et al. in J Couns Psychol 38(4), 1991). Therefore, this study developed a short-form measure of self-efficacy to help identify students in need of intervention.

Detailed spectroscopic analysis of chloride salt deposits in Terra Sirenum, Mars

NASA Astrophysics Data System (ADS)

Osterloo, M. M.; Glotch, T. D.; Bandfield, J. L.

2015-12-01

Chloride salt-bearing deposits have been identified throughout the southern highlands of Mars [1] based on the lack of diagnostic spectral features of anhydrous chlorides in both the visible near infrared (VNIR) and middle infrared (MIR) wavelength ranges [1,2]. A puzzling aspect of martian chloride deposits is the apparent lack of other weathering or evaporite phases associated with most of the deposits. A global analysis over the chloride salt sites conducted by [3] found that only ~9% of the deposits they analyzed were associated with minerals such as phyllosilicates. Most of these occurrences are in Terra Sirenum where [4] noted that salt-bearing deposits lie stratigraphically above Noachian phyllosilicates. Although a variety of formation mechanisms have been proposed for these intriguing deposits, detailed geologic mapping by [5] suggests that surface water and evaporation played a dominant role. On Earth, evaporative settings are often characterized by a multitude of evaporite and phyllosilicate phases including carbonates, sulfates, and nitrates. [6] evaluated chemical divides and brine evolution for martian systems and their results indicate three pathways wherein late-stage brines favor chloride precipitation. In each case the pathway to chloride formation includes precipitation of carbonates (calcite, siderite, and/or magnesite) and sulfates (gypsum, melanterite, and/or epsomite). Here, we present the results of our detailed and systematic spectroscopic study to identify additional evaporite phases associated with salt/silicate mixtures in Terra Sirenum. [1] Osterloo et al. (2008) Science, 319, [2] Glotch, T. D. et al. (2013) Lunar and Planet. Sci. XLIV, abstract #1549 [3] Ruesch, O. et al. (2012), J. Geophys. Res., 117, E00J13 [4] Glotch, T. D. et al. (2010) Geophys. Res. Lett. 37, L16202, [5] Osterloo, M. M. and B. M Hynek (2015) Lunar and Planet. Sci XLVI. Abstract #1054 [6] Tosca, N. J. and S. M. McLennan (2006), Earth and Planet. Sci. Lett., 241.

Report from ILEWG to the COSPAR Panel on Exploration

NASA Astrophysics Data System (ADS)

Foing, Bernard H.

The International Lunar Exploration Working Group (ILEWG) was established in April 1995 at a meeting in Hamburg, Germany. As established in its charter, this working group reports to COSPAR and is charged with developing an international strategy for the exploration of the Moon. It discusses coordination between missions, and a road map for future international lunar exploration and utilisation. It fosters information exchange or potential and real future lunar robotic and human missions, as well as for new scientific and exploration information about the Moon. ILEWG was used to feed forward results from lunar missions such as SMART1 to the next ones, and we look now to integrate lessons from all recent orbiters and landers, for the upcoming landers, sample return missions, and human activities. We give a report on ILEWG community activities, refer to COSPAR and ILEWG ICEUM and lunar conferences and declarations [1-18], and discuss the follow-up of GLUC/ICEUM11 declaration relevant to COSPAR PEX*. References: [1] 1st International Lunar Workshop, Balsiger H. et al., Editors, European Space Agency, 1994. ESA-SP-1170. [2] 2nd International Lunar Workshop, Kyoto, H. Mizutani, editor, Japan Space Forum Publisher, 1997. [3] 3rd International Lunar Workshop, Moscow 1998, E. Galimov, editor. [4] ICEUM4, ESTEC, 2000, ESA SP-462, B.H. Foing & M. Perry, editors. [5] ICEUM5, Hawaii Nov 2003, Durst S.M. et al, Editors, Vol 108, 1-576 pp, Science and Technology Series, American Astronautical Society, 2004. [6] ICEUM6, Udaipur 2004, Bhandari N., Editor, Journal Earth Sys-tem Science, India, 114, No6, Dec 2005, pp. 573-841. [7] ICEUM7, Toronto Sept 2005, sci.esa.int/ilewg. [8] ICEUM8, Beijing July 2006, Journal of Chinese Society of Astronautics, Vol. 28 Sup., 2007, Ji W., Editor. [9] ICEUM9, Sorrento, Italy, Foing B., Espinasse S., Kosters G., Editors. http://sci.esa.int/iceum9, Dec. 2007), [11] Ehrenfreund, P., Foing, B.H., Cellino, A. Editors, The Moon and Near Earth Objects, ASR Vol 37, 1, 2006. [12] Foing, B.H. et al editors, 'Astronomy and Space Science from the Moon', ASR 14, 6, 1994. [13] Ip W.-H., Foing, B.H., Masson Ph.L., editors, The Moon and Mars, ASR Vol 23, 11, 1999. [14] Foing, B.H. et al, editor, Lunar Exploration, Planetary and Space Science, Vol 50, 14-15, 2002. [15] Foing, B.H., Heather, D. editors, 'Lunar Exploration 2000', ASR Vol 30, Nr 8, 2002. [16] Huntress, W. et al 'The next steps in exploring deep space - A cosmic study by the IAA', Acta Astronautica, Vol 58, Issues 6-7, 2006, p302-377. [17] http://sci.esa.int/ilewg/43654-declaration-iceum10-leag-srr-florida-2008/ [18] Ehrenfreund P. et al (COSPAR planetary exploration panel report) 2012, ASR Vol 49, Nr 1, pp. 2-48. *Relevant extract from GLUC/ICEUM11 declaration: “467 International Lunar Explorers, registered delegates from 26 countries, assembled at GLUC Global Lunar Conference including the 11th ILEWG Conference on Exploration and Utilisation of the Moon (ICEUM11) in Beijing." "1. Science and exploration (related GLUC/ICEUM11 recommendations will be addressed at COSPAR B0.1 Lunar science and exploration session) 2. Technologies and resources - A number of robotic missions to the Moon are now undertaken independently by various nations, with a degree of exchange of information and co-ordination. That should increase towards real co-operation, still allowing areas of competition for keeping the process active, cost-effective and faster. - Lunar landers, pressurized lunar rover projects as presented from Europe, Asia and America are important steps that can create opportunities for international collaboration, within a coordinated village of robotic precursors and assistants to crew missions. - We have to think about development, modernization of existing navigation capabilities, and provision of lunar positioning, navigation and data relay assets to support future robotic and human exploration. New concepts and new methods for transportation have attracted much attention and are of great potential. 3. Infrastructures and human aspects - It is recommended to have technical sessions and activities dealing with different aspects of human adaptation to space environments, the modeling of sub-systems, microbial protection and use of inflatable technologies - While the Moon is the best and next logical step in human exploration, we should make best use of the space stations as stepping stones for exploration and human spaceflight beyond Low Earth Orbit. - Further research is needed on lunar dust aspects in regard to humans and interaction with habitats. We note high interest in CELSS for Moon and Mars bases, and recommend further research and development. - We recommend the development and use of terrestrial analogues research sites and facilities, for technology demonstrations, comparative geology and human performance research, and public engagement. We endorse the proposal of development of a site at La Reunion for international Moon-Mars analogue research. 4. Moon, Space, Society and Young Explorers - We consider that the current legal regime as set out in the Outer Space Treaty and the Moon agreement are satisfactory for current and future missions, but may require further clarification for future exploration. Issues of transparency and security will need to be addressed. - Great things are happening for Young Lunar Explorers, with inspiring missions and hands-on activities as coordinated by ILEWG. Lunar exploration is encouraging students of all ages to pursue higher education. - More possibilities for participatory engagement should be offered to the society for example via inter-disciplinary activities with the humanities. - We appreciate the work from COSPAR panel on Exploration PEX that should be shared further. - Continued cooperation should be enforced at all levels. The space community feels strongly that joining the forces of space faring nations to explore the Moon should be seriously implemented, with the views of expanding a Global Robotic Village and building in the long run a Manned International Lunar Base.” “We, the participants of the GLUC-ICEUM11 conference, commit to an enhanced global cooperation towards international lunar exploration for the benefit of humankind. Endorsed by the delegates of GLUC-ICEUM11”

Scaling of Dielectric Breakdown Thresholds in Earth's and CO2-rich atmospheres: Impact for Predictions of Extraterrestrial Transient Luminous Events and Lightning Discharges

NASA Astrophysics Data System (ADS)

Riousset, J. A.

2016-12-01

Earth's atmospheric electricity manifests itself in the form of glow, corona, streamer, and leader discharges observed as Saint Elmo's fire, sprites, lightning and jets discharges, and other Transient Luminous Events (TLEs). All of these are types of dielectric breakdown, but are governed by different physics. In particular, their initiation is associated with the crossing of specific electric field thresholds: relativistic runaway, streamer propagation, conventional breakdown, or thermal runaway thresholds, some better understood than others. For example, the initiation of a lightning discharge is known to occur when the local electric field exceeds a value similar to relativistic runaway field, but the exact threshold, as well as the physical mechanisms at work, remain rather unclear to date. Scaling laws for electric fields (and other quantities) have been established by Pasko et al. [GRL, 25(12), 2123-2126, 1998] and Pasko [NATO Sci. Series, Springer, 253-311, 2006]. In this work, we develop profiles for initiation criteria in air and in other atmospheric environments. We further calculate their associated scaling laws to determine the ability to trigger lightning flashes and TLEs in our solar system. This lets us predict the likelihood of electrical discharges on, e.g., Mars, Venus and Titan, and calculate the expected electric field conditions, under which discharges have been observed on Jupiter, Saturn, Uranus, and Neptune [Leblanc et al., ISSI Spa. Sci. Series, Springer, 2008, Yair, Adv. Space Res., 50(3), 293-310, 2012]. Our results anticipate the arrival of ExoMars 2016's Schiaparelli module, which will provide the first records of electric field at the surface of the planet [Déprez et al., EGU GA, 16, 16613, 2014]. This research is also motived by the increasing probability of manned missions to Mars and the potential electrostatic hazards it may face [Yair, 2012], and by the role of electrical discharges in the creation of active radicals, some of which may be of biological importance [Miller, Science, 117, 528-529, 1953; Biochem. Biophys. Acta, 23, 480-489, 1957].

Response to Julian et al. (2015) "comment on and reinterpretation of Gabriel et al. (2014) 'fish mercury and surface water sulfate relationships in the everglades protection area'".

PubMed

Gabriel, Mark C; Axelrad, Don; Orem, William; Osborne, Todd Z

2015-06-01

The purpose of this forum is to respond to a rebuttal submitted by Julian et al., Environ Manag 55:1-5, 2015 where they outlined their overall disagreement with the data preparation, methods, and interpretation of results presented in Gabriel et al. (Environ Manag 53:583-593, 2014). Here, we provide background information on the research premise presented in Gabriel et al. (Environ Manag 53:583-593, 2014) and provide a defense for this work using five themes. In spite of what Julian et al. perceive as limitations in the sampling methods and analytical tools used for this work, the relationships found between fish total mercury and surface water sulfate concentrations in Gabriel et al. (Environ Manag 53:583-593, 2014) are comparable to relationships between pore water methylmercury (MeHg) and pore water sulfate found in past studies indicating that sulfate is important to MeHg production and bioaccumulation in the Everglades. Julian et al. state "…there is no way to justify any ecosystem-wide sulfur strategy as a management approach to reduce mercury risk in the (Everglades) as suggested by Gabriel et al. (Environ Manag 53:583-593, 2014), Corrales et al. (Sci Tot Environ 409:2156-2162, 2011) and Orem et al. (Rev Environ Sci Technol 41 (S1):249-288, 2011)." We disagree, and having stated why sulfate input reduction to the Everglades may be the most effective means of reducing mercury in Everglades fish, it is important that research on sulfur and mercury biogeochemistry continues. If further studies support the relationship between sulfate loading reduction and MeHg reduction, sulfur mass balance studies should commence to (1) better quantify agricultural and connate seawater sulfate inputs and (2) define opportunities to reduce sulfate inputs to the Everglades ecosystem.

Characterization of meningeal type 2 innate lymphocytes and their response to CNS injury

PubMed Central

Overall, Christopher C.

2017-01-01

The meningeal space is occupied by a diverse repertoire of immune cells. Central nervous system (CNS) injury elicits a rapid immune response that affects neuronal survival and recovery, but the role of meningeal inflammation remains poorly understood. Here, we describe type 2 innate lymphocytes (ILC2s) as a novel cell type resident in the healthy meninges that are activated after CNS injury. ILC2s are present throughout the naive mouse meninges, though are concentrated around the dural sinuses, and have a unique transcriptional profile. After spinal cord injury (SCI), meningeal ILC2s are activated in an IL-33–dependent manner, producing type 2 cytokines. Using RNAseq, we characterized the gene programs that underlie the ILC2 activation state. Finally, addition of wild-type lung-derived ILC2s into the meningeal space of IL-33R−/− animals partially improves recovery after SCI. These data characterize ILC2s as a novel meningeal cell type that responds to SCI and could lead to new therapeutic insights for neuroinflammatory conditions. PMID:27994070

Comparing Time-Dependent Geomagnetic and Atmospheric Effects on Cosmogenic Nuclide Production Rate Scaling

NASA Astrophysics Data System (ADS)

Lifton, N. A.

2014-12-01

A recently published cosmogenic nuclide production rate scaling model based on analytical fits to Monte Carlo simulations of atmospheric cosmic ray flux spectra (both of which agree well with measured spectra) (Lifton et al., 2014, Earth Planet. Sci. Lett. 386, 149-160: termed the LSD model) provides two main advantages over previous scaling models: identification and quantification of potential sources of bias in the earlier models, and the ability to generate nuclide-specific scaling factors easily for a wide range of input parameters. The new model also provides a flexible framework for exploring the implications of advances in model inputs. In this work, the scaling implications of two recent time-dependent spherical harmonic geomagnetic models spanning the Holocene will be explored. Korte and Constable (2011, Phys. Earth Planet. Int. 188, 247-259) and Korte et al. (2011, Earth Planet. Sci. Lett. 312, 497-505) recently updated earlier spherical harmonic paleomagnetic models used by Lifton et al. (2014) with paleomagnetic measurements from sediment cores in addition to archeomagnetic and volcanic data. These updated models offer improved accuracy over the previous versions, in part to due to increased temporal and spatial data coverage. With the new models as input, trajectory-traced estimates of effective vertical cutoff rigidity (RC- the standard method for ordering cosmic ray data) yield significantly different time-integrated scaling predictions when compared to the earlier models. These results will be compared to scaling predictions using another recent time-dependent spherical harmonic model of the Holocene geomagnetic field by Pavón-Carrasco et al. (2014, Earth Planet. Sci. Lett. 388, 98-109), based solely on archeomagnetic and volcanic paleomagnetic data, but extending to 14 ka. In addition, the potential effects of time-dependent atmospheric models on LSD scaling predictions will be presented. Given the typical dominance of altitudinal over latitudinal scaling effects on cosmogenic nuclide production, incorporating transient global simulations of atmospheric structure (e.g., Liu et al., 2009, Science 325, 310-314) into scaling frameworks may contribute to improved understanding of long-term production rate variations.

Public aquaria as long-term enrichments for investigating planktonic Archaea

NASA Astrophysics Data System (ADS)

Goldenstein, Nadine I.; Warren, Courtney E.; Lipp, Julius S.; Pagani, Mark; Hinrichs, Kai-Uwe

2016-04-01

The most abundant group of planktonic Archaea , the so-called Thaumarchaeota, represents 20% of all marine planktonic microorganisms (Karner et al., 2001) and their energy efficient performance of nitrification makes them key players in the global nitrogen- and carbon-cycle (Könneke et al., 2014). Furthermore, planktonic Archaea are considered to be the major producers of specific microbial membrane lipids that are extensively used as paleoproxies in marine climate research (Schouten et al., 2002). Therefore, assessing the parameters controlling the distribution of Archaea in the marine water column is crucial for studies of modern and past marine environments. Although diverse studies utilizing DNA- and biomarker-based approaches have constrained the turnover and distribution of marine Archaea, the environmental factors affecting their abundance and activity (e.g., Wuchter et al., 2006; Bale et al., 2013) are still poorly understood. Further, previous surveys, using enrichment cultivation and pure culture experiments, provided valuable information on adaptation of planktonic Archaea to changes of parameters affecting growth conditions, such as temperature, salinity and growth stage (Elling et al., 2014, 2015). Hence, we know that planktonic Archaea directly adapt their membranes to changing growth conditions, but also that environmental selection for individual phylogenetic groups of these organisms is also reflected in the membrane lipid pool. Extending these studies, this project further aims at constraining the environmental parameters controlling archaeal abundance in the marine environment. Public aquaria, which are comparable to perfectly monitored long-term enrichment cultures, are optimal sampling sites for this task. A comprehensive set of 120 water and substrate samples from fresh, marine and brackish systems exhibiting diverse conditions was selected from 15 public aquaria at the east and west coast of the USA. These samples were examined for their archaeal intact polar and core membrane lipid composition. We detected a set of more than 90 different lipid structures comprised of diverse glyco- as well as phospho- based head groups combined with di- and tetraether cores containing up to 5 cyclopentane rings or unsaturations. The correlation of the variability within the lipid portfolio with the 30 different environmental variables, measured in the individual tanks, like e.g., water chemistry, light availability and temperature will lead to a better understanding of the factors controlling planktonic archaeal distribution in the marine environment and the derived lipid-based proxies. References: Karner et al. (2001). Nature 409, p507-510. Könneke et al. (2014). Proc Natl Acad Sci U S A 111, p8239-44. Schouten et al. (2002). Earth Planet Sci Lett 204, p265-274. Wuchter et al. (2006). Proc Natl Acad Sci U S A 103, p12317-12322. Bale et al. (2013), Biogeosciences Discuss 10, p12593-12624. Elling et al. (2014). Geochim Cosmochim Acta 141, p579-597. Elling et al. (2015). Geochim Cosmochim Acta 171, p238-255.

Simulations of the MATROSHKA experiment at the international space station using PHITS.

PubMed

Sihver, L; Sato, T; Puchalska, M; Reitz, G

2010-08-01

Concerns about the biological effects of space radiation are increasing rapidly due to the perspective of long-duration manned missions, both in relation to the International Space Station (ISS) and to manned interplanetary missions to Moon and Mars in the future. As a preparation for these long-duration space missions, it is important to ensure an excellent capability to evaluate the impact of space radiation on human health, in order to secure the safety of the astronauts/cosmonauts and minimize their risks. It is therefore necessary to measure the radiation load on the personnel both inside and outside the space vehicles and certify that organ- and tissue-equivalent doses can be simulated as accurate as possible. In this paper, simulations are presented using the three-dimensional Monte Carlo Particle and Heavy-Ion Transport code System (PHITS) (Iwase et al. in J Nucl Sci Tech 39(11):1142-1151, 2002) of long-term dose measurements performed with the European Space Agency-supported MATROSHKA (MTR) experiment (Reitz and Berger in Radiat Prot Dosim 120:442-445, 2006). MATROSHKA is an anthropomorphic phantom containing over 6,000 radiation detectors, mimicking a human head and torso. The MTR experiment, led by the German Aerospace Center (DLR), was launched in January 2004 and has measured the absorbed doses from space radiation both inside and outside the ISS. Comparisons of simulations with measurements outside the ISS are presented. The results indicate that PHITS is a suitable tool for estimation of doses received from cosmic radiation and for study of the shielding of spacecraft against cosmic radiation.

A Report of Clouds on Titan

NASA Astrophysics Data System (ADS)

Corlies, Paul; Hayes, Alexander; Adamkovics, Mate; Rodriguez, Sebastien; Kelland, John; Turtle, Elizabeth P.; Mitchell, Jonathan; Lora, Juan M.; Rojo, Patricio; Lunine, Jonathan I.

2017-10-01

We present in this work a detailed analysis of many of the clouds in the Cassini Visual and Infrared Mapping Spectrometer (VIMS) dataset in order to understand their global and seasonal properties. Clouds are one of the few direct observables in Titan’s atmosphere (Griffith et al 2009, Rodriguez et al 2009, Adamkovics et al 2010), and so determining their characteristics allows for a better understanding of surface atmosphere interactions, winds, transport of volatile material, and general circulation. We find the clouds on Titan generally reside in at 5-15km altitude, which agrees with previous modelling efforts (Rafkin et al. 2015), as well as a power law distribution for cloud optical depth. We assume an average cloud droplet size of 100um. No seasonal dependence is observed with either cloud altitude or optical depth, suggesting there is no preferred seasonal formation mechanisms. Combining these characteristics with cloud size (Kelland et al 2017) can trace the transport of volatiles in Titan’s atmosphere, which can be compared against general circulation models (GCMs) (Lora et al 2015). We also present some specific analysis of interesting cloud systems including hypothesized surface fogs (Brown et al 2009) and orographic cloud formation (Barth et al 2010, Corlies et al 2017). In this analysis we use a correlation between Cassini VIMS and RADAR observations as well as an updated topographic map of Titan’s southern hemisphere to better understand the role that topography plays in influencing and driving atmospheric phenomena.Finally, with the end of the Cassini mission, ground based observing now acts as the only means with which to observe clouds on Titan. We present an update of an ongoing cloud campaign to search for clouds on Titan and to understand their seasonal evolution.References:Adamkovics et al. 2010, Icarus 208:868Barth et al. 2010, Planet. Space Sci. 58:1740Corlies et al. 2017, 48th LPSC, 2870CGriffith et al. 2009, ApJ 702:L105Kelland et al. 2017, 48th LPSC, 2748KLora et al. 2015, Icarus 250:516Rafkin et al. 2015, J. Geophys. Res. 120:739Rodriguez et al. 2009, Nature 459:678

Groundbased Observations of sodium at Mercury during the First MESSENGER Flyby

NASA Astrophysics Data System (ADS)

Potter, A. E.; Killen, R. M.; Mouawad, N.

2008-09-01

Abstract Groundbased observations of the sodium exospheric emission at Mercury taken at the McMathPierce Solar Telescope at Kitt Peak, Arizona, were conducted during the period of January 1018, 2008. During these observations, we mapped the distribution of sodium D2 emission over the planet. The procedure for mapping sodium using an image slicer and tiptilt image stabilization has been described by Potter et al. [1]. The emission maps were used to construct maps of sodium column density. Herein we discuss the temporal and spatial variability of the sodium emission on the observed side of planet. Maps of surface reflectance in the continuum near the sodium D2 line (left ) and column abundance of sodium in the exosphere (right) are shown for January 12, 13 and 14, in Figures 1, 2, and 3, respectively. The maximum column density was in the range 1.15 to 1.40 x 1011 atoms/cm2 during this period. The sodium distribution is uneven, with higher values of column density at high southern and northern E P S C EPSC Abstracts, Vol. 3, EPSC2008-A-00311, 2008 European Planetary Science Congress, Author(s) 2008 latitudes. This may be the effect of solar radiation acceleration [2] which was near its maximum value, ranging from 164 to 171 cm/sec2, or 0.44 to 0.46 of surface gravity. As a consequence of high radiation pressure, sodium atoms are driven to high latitudes. However, the distribution for January 12 shows a considerable excess in high southern latitudes, suggesting a source of sodium at those latitudes. This dataset brackets observations taken with the Ultraviolet and Visible Spectrometer (UVVS) on the Mercury Atmospheric and Surface Composition Spectrometer (MASCS) instrument [3] onboard the MESSENGER spacecraft [4] during the first flyby of the planet, January 14, 2008. An analogy between both data sets will be discussed. References [1] Potter, A.E., Plymate C., Keller C., Killen R.M., and Morgan T.H. (2006) Adv. Space Res. 38, 599603. [2] Potter, A.E., R. M. Killen, M. Sarantos. (2006) Icarus, 181, 112. [3] McClintock, W. E., and Lankton, M.R. (2007) Space Sci. Rev. 131, 481522. [4] Solomon, S. C., et al. (2001) Planet. Space Sci. 49, 14451465. Acknowledgements: The National Solar Observatory is funded by the National Science Foundation. Groundbased observations were funded by the NASA Planetary Astronomy Program. MESSENGER is a NASA Discovery mission.

Climate Consensus and `Misinformation': A Rejoinder to Agnotology, Scientific Consensus, and the Teaching and Learning of Climate Change

NASA Astrophysics Data System (ADS)

Legates, David R.; Soon, Willie; Briggs, William M.; Monckton of Brenchley, Christopher

2015-04-01

Agnotology is the study of how ignorance arises via circulation of misinformation calculated to mislead. Legates et al. (Sci Educ 22:2007-2017, 2013) had questioned the applicability of agnotology to politically-charged debates. In their reply, Bedford and Cook (Sci Educ 22:2019-2030, 2013), seeking to apply agnotology to climate science, asserted that fossil-fuel interests had promoted doubt about a climate consensus. Their definition of climate `misinformation' was contingent upon the post-modernist assumptions that scientific truth is discernible by measuring a consensus among experts, and that a near unanimous consensus exists. However, inspection of a claim by Cook et al. (Environ Res Lett 8:024024, 2013) of 97.1 % consensus, heavily relied upon by Bedford and Cook, shows just 0.3 % endorsement of the standard definition of consensus: that most warming since 1950 is anthropogenic. Agnotology, then, is a two-edged sword since either side in a debate may claim that general ignorance arises from misinformation allegedly circulated by the other. Significant questions about anthropogenic influences on climate remain. Therefore, Legates et al. appropriately asserted that partisan presentations of controversies stifle debate and have no place in education.

Variation in 142Nd/144Nd of Archean rocks from southwest Greenland : Implications for early Earth mantle dynamics

NASA Astrophysics Data System (ADS)

Rizo, H.; Boyet, M.; Blichert-Toft, J.; Rosing, M.; Paquette, J. L.

2012-04-01

The short-lived 146Sm-142Nd chronometer (half-life = 103 Ma) has proven successful in bringing constraints on the dynamics of the early Earth mantle. Since the parent isotope, 146Sm, was extant only during the first 300 Ma of the history of the Solar System, the positive 142Nd anomalies measured in southwest Greenland Archean rocks imply that their incompatible element-depleted mantle source formed during the Hadean. Interestingly, the magnitude of these anomalies seems to decrease over time. 3.7-3.8 Ga old rocks from the Amitsoq Complex have revealed +10 to +20 ppm 142Nd anomalies [1, 2, 3, 4, 5, 6, 7], whereas younger 3.0 Ga old samples from the Ivisaartoq greenstone belt yield smaller positive anomalies, ranging from +5.5 to +8.5 ppm [8]. Thus, the chemical heterogeneities detected in the southwest Greenland mantle were formed during the first 150 Ma of Earth's history, and seem to have resisted re-mixing by mantle convection until 3.0 Ga. In this study, we investigate the evolution of the southwest Greenland mantle during the time period of 3.3-3.4 Ga. The samples analyzed come from both the ~3.3 Ga amphibolite unit and the ~3.4 Ga Ameralik basic dyke swarm from the Amitsoq Complex. Coupled Sm-Nd and Lu-Hf bulk-rock ages obtained for seven amphibolites are in good agreement (3351 ± 210 Ma and 3302 ± 260 Ma, respectively) and consistent with the minimum age found by Nutman and Friend (2009) [9] for this formation. We further obtained coherent bulk-rock 147Sm-143Nd and zircon+baddeleyite 207Pb/206Pb ages for the Ameralik dykes (3428 ± 250 Ma and 3421 ± 34 Ma, respectively), in line with ages suggested by Nielsen at al., (2002) [10] and Nutman et al., (2004) [11]. We are currently in the process of analyzing these samples for 142Nd isotopic compositions and the results will be compared with the existing southwest Greenland data in order to shed new light on the evolution and destruction of heterogeneities in the early Earth mantle. [1] Rizo et al., (2011) Earth Planet. Sci. Lett. [2] Bennett et al., (2007b) Science. [3] Boyet et al., (2003) Earth Planet. Sci. Lett. [4] Boyet and Carlson (2006) Earth Planet. Sci. Lett. [5] Caro et al., (2003) Nature. [6] Caro et al., (2006) Geochim. Cosmochim. Acta. [7] Harper and Jacobsen (1992) Nature. [8] Bennett et al., (2010) Goldschmidt 2010. [9] Nutman and Friend (2009) Precamb. Res. [10] Nielsen et al., (2002) Precamb. Res. [11] Nutman et al., (2004) J. Geol. Soc. Lond.

Complete spinal cord injury (SCI) transforms how brain derived neurotrophic factor (BDNF) affects nociceptive sensitization.

PubMed

Huang, Yung-Jen; Lee, Kuan H; Grau, James W

2017-02-01

Noxious stimulation can induce a lasting increase in neural excitability within the spinal cord (central sensitization) that can promote pain and disrupt adaptive function (maladaptive plasticity). Brain-derived neurotrophic factor (BDNF) is known to regulate the development of plasticity and has been shown to impact the development of spinally-mediated central sensitization. The latter effect has been linked to an alteration in GABA-dependent inhibition. Prior studies have shown that, in spinally transected rats, exposure to regular (fixed spaced) stimulation can counter the development of maladaptive plasticity and have linked this effect to an up-regulation of BDNF. Here it is shown that application of the irritant capsaicin to one hind paw induces enhanced mechanical reactivity (EMR) after spinal cord injury (SCI) and that the induction of this effect is blocked by pretreatment with fixed spaced shock. This protective effect was eliminated if rats were pretreated with the BDNF sequestering antibody TrkB-IgG. Intrathecal (i.t.) application of BDNF prevented, but did not reverse, capsaicin-induced EMR. BDNF also attenuated cellular indices (ERK and pERK expression) of central sensitization after SCI. In uninjured rats, i.t. BDNF enhanced, rather than attenuated, capsaicin-induced EMR and ERK/pERK expression. These opposing effects were related to a transformation in GABA function. In uninjured rats, BDNF reduced membrane-bound KCC2 and the inhibitory effect of the GABA A agonist muscimol. After SCI, BDNF increased KCC2 expression, which would help restore GABAergic inhibition. The results suggest that SCI transforms how BDNF affects GABA function and imply that the clinical usefulness of BDNF will depend upon the extent of fiber sparing. Copyright © 2016 Elsevier Inc. All rights reserved.

The eccentric Kozai-Lidov effect as a resonance phenomenon

NASA Astrophysics Data System (ADS)

Sidorenko, Vladislav V.

2018-01-01

Exploring weakly perturbed Keplerian motion within the restricted three-body problem, Lidov (Planet Space Sci 9:719-759, 1962) and, independently, Kozai (Astron J 67:591-598, 1962) discovered coupled oscillations of eccentricity and inclination (the KL cycles). Their classical studies were based on an integrable model of the secular evolution, obtained by double averaging of the disturbing function approximated with its first non-trivial term. This was the quadrupole term in the series expansion with respect to the ratio of the semimajor axis of the disturbed body to that of the disturbing body. If the next (octupole) term is kept in the expression for the disturbing function, long-term modulation of the KL cycles can be established (Ford et al. in Astrophys J 535:385-401, 2000; Naoz et al. in Nature 473:187-189, 2011; Katz et al. in Phys Rev Lett 107:181101, 2011). Specifically, flips between the prograde and retrograde orbits become possible. Since such flips are observed only when the perturber has a nonzero eccentricity, the term "eccentric Kozai-Lidov effect" (or EKL effect) was proposed by Lithwick and Naoz (Astrophys J 742:94, 2011) to specify such behavior. We demonstrate that the EKL effect can be interpreted as a resonance phenomenon. To this end, we write down the equations of motion in terms of "action-angle" variables emerging in the integrable Kozai-Lidov model. It turns out that for some initial values the resonance is degenerate and the usual "pendulum" approximation is insufficient to describe the evolution of the resonance phase. Analysis of the related bifurcations allows us to estimate the typical time between the successive flips for different parts of the phase space.

Wave-function description of conductance mapping for a quantum Hall electron interferometer

NASA Astrophysics Data System (ADS)

Kolasiński, K.; Szafran, B.

2014-04-01

Scanning gate microscopy of quantum point contacts (QPC) in the integer quantum Hall regime is considered in terms of the scattering wave functions with a finite-difference implementation of the quantum transmitting boundary approach. Conductance (G) maps for a clean QPC as well as for a system including an antidot within the QPC constriction are evaluated. The steplike locally flat G maps for clean QPCs turn into circular resonances that are reentrant in an external magnetic field when the antidot is introduced to the constriction. The current circulation around the antidot and the spacing of the resonances at the magnetic field scale react to the probe approaching the QPC. The calculated G maps with a rigid but soft antidot potential reproduce the features detected recently in the electron interferometer [F. Martins et al., Sci. Rep. 3, 1416 (2013), 10.1038/srep01416].

A Martian PFS average spectrum: Comparison with ISO SWS

NASA Astrophysics Data System (ADS)

Formisano, V.; Encrenaz, T.; Fonti, S.; Giuranna, M.; Grassi, D.; Hirsh, H.; Khatuntsev, I.; Ignatiev, N.; Lellouch, E.; Maturilli, A.; Moroz, V.; Orleanski, P.; Piccioni, G.; Rataj, M.; Saggin, B.; Zasova, L.

2005-08-01

The evaluation of the planetary Fourier spectrometer performance at Mars is presented by comparing an average spectrum with the ISO spectrum published by Lellouch et al. [2000. Planet. Space Sci. 48, 1393.]. First, the average conditions of Mars atmosphere are compared, then the mixing ratios of the major gases are evaluated. Major and minor bands of CO 2 are compared, from the point of view of features characteristics and bands depth. The spectral resolution is also compared using several solar lines. The result indicates that PFS radiance is valid to better than 1% in the wavenumber range 1800-4200 cm -1 for the average spectrum considered (1680 measurements). The PFS monochromatic transfer function generates an overshooting on the left-hand side of strong narrow lines (solar or atmospheric). The spectral resolution of PFS is of the order of 1.3 cm -1 or better. A large number of narrow features to be identified are discovered.

SOFIA Science Imagery

NASA Image and Video Library

2017-09-14

SCI2012_0003: SOFIA mid-infrared image of the planetary nebula Minkowski 2-9 (M2-9), also known as the Butterfly Nebula, compared with a visual-wavelength Hubble Space Telescope image at the same scale and orientation. The nebula is composed of two lobes of gas & dust expelled from a dying star with about the mass of our Sun that is seen at the center of the lobes. The HST image shows mostly ionized gas in the lobes whereas the SOFIA image shows mostly solid grains condensing in the gas. The SOFIA data were obtained during SOFIA's Early Science program in 2011 by a Guest Investigator team led by Michael Werner of Caltech/JPL using the FORCAST camera (P.I.Terry Herter, Cornell University). Credit: SOFIA image, RGB = 37, 24, 20 microns; NASA/DLR/USRA/DSI/FORCAST team/M. Werner et al./A. Helton, J. Rho; HST image: NASA/ESA/NSF/AURA/Hubble Heritage Team/STScI/B. Balick, V. Icke, G. Mellema

Near midplane scintillator-based fast ion loss detector on DIII-D.

PubMed

Chen, X; Fisher, R K; Pace, D C; García-Muñoz, M; Chavez, J A; Heidbrink, W W; Van Zeeland, M A

2012-10-01

A new scintillator-based fast-ion loss detector (FILD) installed near the outer midplane of the plasma has been commissioned on DIII-D. This detector successfully measures coherent fast ion losses produced by fast-ion driven instabilities (≤500 kHz). Combined with the first FILD at ∼45° below the outer midplane [R. K. Fisher, et al., Rev. Sci. Instrum. 81, 10D307 (2010)], the two-detector system measures poloidal variation of losses. The phase space sensitivity of the new detector (gyroradius r(L) ∼ [1.5-8] cm and pitch angle α ∼ [35°-85°]) is calibrated using neutral beam first orbit loss measurements. Since fast ion losses are localized poloidally, having two FILDs at different poloidal locations allows for the study of losses over a wider range of plasma shapes and types of loss orbits.

Reports and recommendations from COSPAR Planetary Exploration Committee (PEX) & International Lunar Exploration Working Group (ILEWG)

NASA Astrophysics Data System (ADS)

Ehrenfreund, Pascale; Foing, Bernard

2014-05-01

In response to the growing importance of space exploration, the objectives of the COSPAR Panel on Exploration (PEX) are to provide high quality, independent science input to support the development of a global space exploration program while working to safeguard the scientific assets of solar system bodies. PEX engages with COSPAR Commissions and Panels, science foundations, IAA, IAF, UN bodies, and IISL to support in particular national and international space exploration working groups and the new era of planetary exploration. COSPAR's input, as gathered by PEX, is intended to express the consensus view of the international scientific community and should ultimately provide a series of guidelines to support future space exploration activities and cooperative efforts, leading to outstanding scientific discoveries, opportunities for innovation, strategic partnerships, technology progression, and inspiration for people of all ages and cultures worldwide. We shall focus on the lunar exploration aspects, where the COSPAR PEX is building on previous COSPAR, ILEWG and community conferences. An updated COSPAR PEX report is published and available online (Ehrenfreund P. et al, COSPAR planetary exploration panel report, http://www.gwu.edu/~spi/assets/COSPAR_PEX2012.pdf). We celebrate 20 years after the 1st International Conference on Exploration and Utilisation of the Moon at Beatenberg in June 1994. The International Lunar Exploration Working Group (ILEWG) was established the year after in April 1995 at an EGS meeting in Hamburg, Germany. As established in its charter, this working group reports to COSPAR and is charged with developing an international strategy for the exploration of the Moon (http://sci.esa.int/ilewg/ ). It discusses coordination between missions, and a road map for future international lunar exploration and utilisation. It fosters information exchange or potential and real future lunar robotic and human missions, as well as for new scientific and exploration information about the Moon. We present the GLUC/ICEUM11 declaration (with emphasis on Science and exploration; Technologies and resources, Infrastructures and human aspects; Moon, Space, Society and Young Explorers) (http://sci.esa.int/iceum11). We give a report on ongoing relevant ILEWG community activities. We discuss how lunar missions SMART-1, Kaguya, Chang'E1&2, Chandrayaan-1, LCROSS, LRO, GRAIL, LADEE, Chang'E3 and upcoming missions contribute to lunar exploration objectives & roadmap.

Microvesicles as mediators of intercellular communication in cancer.

PubMed

Antonyak, Marc A; Cerione, Richard A

2014-01-01

The discovery that cancer cells generate large membrane-enclosed packets of epigenetic information, known as microvesicles (MVs), that can be transferred to other cells and influence their behavior (Antonyak et al., Small GTPases 3:219-224, 2012; Cocucci et al., Trends Cell Biol 19:43-51, 2009; Rak, Semin Thromb Hemost 36:888-906, 2010; Skog et al., Nat Cell Biol 10:1470-1476, 2008) has added a unique perspective to the classical paracrine signaling paradigm. This is largely because, in addition to growth factors and cytokines, MVs contain a variety of components that are not usually thought to be released into the extracellular environment by viable cells including plasma membrane-associated proteins, cytosolic- and nuclear-localized proteins, as well as nucleic acids, particularly RNA transcripts and micro-RNAs (Skog et al., Nat Cell Biol 10:1470-1476, 2008; Al-Nedawi et al., Nat Cell Biol 10:619-624, 2008; Antonyak et al., Proc Natl Acad Sci U S A 108:4852-4857, 2011; Balaj et al., Nat Commun 2:180, 2011; Choi et al., J Proteome Res 6:4646-4655, 2007; Del Conde et al., Blood 106:1604-1611, 2005; Gallo et al., PLoS One 7:e30679, 2012; Graner et al., FASEB J 23:1541-1557, 2009; Grange et al., Cancer Res 71:5346-5356, 2011; Hosseini-Beheshti et al., Mol Cell Proteomics 11:863-885, 2012; Martins et al., Curr Opin Oncol 25:66-75, 2013; Noerholm et al., BMC Cancer 12:22, 2012; Zhuang et al., EMBO J 31:3513-3523, 2012). When transferred between cancer cells, MVs have been shown to stimulate signaling events that promote cell growth and survival (Al-Nedawi et al., Nat Cell Biol 10:619-624, 2008). Cancer cell-derived MVs can also be taken up by normal cell types that surround the tumor, an outcome that helps shape the tumor microenvironment, trigger tumor vascularization, and even confer upon normal recipient cells the transformed characteristics of a cancer cell (Antonyak et al., Proc Natl Acad Sci U S A 108:4852-4857, 2011; Martins et al., Curr Opin Oncol 25:66-75, 2013; Al-Nedawi et al., Proc Natl Acad Sci U S A 106:3794-3799, 2009; Ge et al., Cancer Microenviron 5:323-332, 2012). Thus, the production of MVs by cancer cells plays crucial roles in driving the expansion of the primary tumor. However, it is now becoming increasingly clear that MVs are also stable in the circulation of cancer patients, where they can mediate long-range effects and contribute to the formation of the pre-metastatic niche, an essential step in metastasis (Skog et al., Nat Cell Biol 10:1470-1476, 2008; Noerholm et al., BMC Cancer 12:22, 2012; Peinado et al., Nat Med 18:883-891, 2012; Piccin et al., Blood Rev 21:157-171, 2007; van der Vos et al., Cell Mol Neurobiol 31:949-959, 2011). These findings, when taken together with the fact that MVs are being aggressively pursued as diagnostic markers, as well as being considered as potential targets for intervention against cancer (Antonyak et al., Small GTPases 3:219-224, 2012; Hosseini-Beheshti et al., Mol Cell Proteomics 11:863-885, 2012; Martins et al., Curr Opin Oncol 25:66-75, 2013; Ge et al., Cancer Microenviron 5:323-332, 2012; Peinado et al., Nat Med 18:883-891, 2012; Piccin et al., Blood Rev 21:157-171, 2007; Al-Nedawi et al., Cell Cycle 8:2014-2018, 2009; Cocucci and Meldolesi, Curr Biol 21:R940-R941, 2011; D'Souza-Schorey and Clancy, Genes Dev 26:1287-1299, 2012; Shao et al., Nat Med 18:1835-1840, 2012), point to critically important roles for MVs in human cancer progression that can potentially be exploited to develop new targeted approaches for treating this disease.

The validation and preference among different EAM potentials to describe the solid-liquid transition of aluminum

NASA Astrophysics Data System (ADS)

Jiang, Yewei; Luo, Jie; Wu, Yongquan

2017-06-01

Empirical potential is vital to the classic atomic simulation, especially for the study of phase transitions, as well as the solid-interface. In this paper, we attempt to set up a uniform procedure for the validation among different potentials before the formal simulation study of phase transitions of metals. Two main steps are involved: (1) the prediction of the structures of both solid and liquid phases and their mutual transitions, i.e. melting and crystallization; (2) the prediction of vital thermodynamic (the equilibrium melting point at ambient pressure) and dynamic properties (the degrees of superheating and undercooling). We applied this procedure to the testing of seven published embedded-atom potentials (MKBA (Mendelev et al 2008 Philos. Mag. 88 1723), MFMP (Mishin et al 1999 Phys. Rev. B 59 3393), MDSL (Sturgeon and Laird 2000 Phys. Rev. B 62 14720), ZM (Zope and Mishin 2003 Phys. Rev. B 68 024102), LEA (Liu et al 2004 Model. Simul. Mater. Sci. Eng. 12 665), WKG (Winey et al 2009 Model. Simul. Mater. Sci. Eng. 17 055004) and ZJW (Zhou et al 2004 Phys. Rev. B 69 144113)) for the description of the solid-liquid transition of Al. All the predictions of structure, melting point and superheating/undercooling degrees were compared with the experiments or theoretical calculations. Then, two of them, MKBA and MDSL, were proven suitable for the study of the solid-liquid transition of Al while the residuals were unqualified. However, potential MKBA is more accurate to predict the structures of solid and liquid, while MDSL works a little better in the thermodynamic and dynamic predictions of solid-liquid transitions.

Exertional Heat Illness and Hyponatremia: An Epidemiological Prospective

DTIC Science & Technology

2008-01-01

physical fitness Excessive body weight Dehydration >1-h aerobic intense exercise Alcohol Peer pressure/ motivation Medical Febrile illness...Med. Sci. Sports Exerc. 38:1197Y1203, 2006. 23. Savdie, E., H. Prevedoros, A. Irish, et al. Heat stroke following Rugby League football. Med. J. Aust

Exposure Science for Chemical Prioritization and Toxicity Testing

EPA Science Inventory

Currently, a significant research effort is underway to apply new technologies to screen and prioritize chemicals for toxicity testing as well as to improve understanding of toxicity pathways (Dix et al. 2007, Toxicol Sci; NRC, 2007, Toxicity Testing in the 21st Century; Collins ...

Navigating "Thorny" Issues

ERIC Educational Resources Information Center

Hutchinson, Kashema; Gilbert, Aderinsola; Malyukova, Anna

2016-01-01

In their article "Mindfulness and discussing 'thorny' issues in the classroom" Konstantinos Alexakos et al. ("Cult Stud Sci Educ," 2016. doi: 10.1007/s11422-015-9718-0) describe "thorny" issues as "difficult topics to discuss because they are more personal to some perhaps even cause pain and violence." As…

Public Data Set: Radially Scanning Magnetic Probes to Study Local Helicity Injection Dynamics

DOE Office of Scientific and Technical Information (OSTI.GOV)

Richner, Nathan J; Bongard, Michael W; Fonck, Raymond J

This data set contains openly-documented, machine readable digital research data corresponding to figures published in N.J. Richner et al., 'Radially Scanning Magnetic Probes to Study Local Helicity Injection Dynamics,' accepted for publication in Rev. Sci. Instrum (2018).

Correction: Humic-like substances from urban waste as auxiliaries for photo-Fenton treatment: a fluorescence EEM-PARAFAC study.

PubMed

García Ballesteros, S; Costante, M; Vicente, R; Mora, M; Amat, A M; Arques, A; Carlos, L; García Einschlag, F S

2018-06-13

Correction for 'Humic-like substances from urban waste as auxiliaries for photo-Fenton treatment: a fluorescence EEM-PARAFAC study' by S. García Ballesteros et al., Photochem. Photobiol. Sci., 2017, 16, 38-45.

Re-examination of the Possibility of Haze in Pluto's Atmosphere Based on Multi-Wavelength Observations of the Pluto Occultation of P131.1.

NASA Astrophysics Data System (ADS)

Thomas-Osip, J. E.; Elliot, J. L.; Clancy, K. B.

2002-12-01

Multi-wavelength observations of the occultation of P131.1 by Pluto (see Elliot et al., this conference) allow for a re-examination of the possibility of the existence of haze in Pluto's atmosphere. Models of the extinction efficiency of haze particles as a function of wavelength are being used investigate the potential for the existence of haze in the 2002 Pluto atmosphere. The existence of a haze layer in Pluto's atmosphere was postulated to explain the abrupt change in slope seen in the light curve of the 1988 stellar occultation by Pluto (Elliot and Young 1992, AJ, 103, 991). An alternative explanation (Hubbard et al. 1990, Icarus, 84, 1) includes a steep thermal gradient near the surface instead of, or in addition to, a haze layer. Modeling of the growth and sedimentation of photo-chemically produced spherical aerosols (Stansberry et al. 1989, Geophys. Res. Let., 16, 1221) suggested that an appropriate production rate is not sufficient to produce the opacity necessary to account for change in slope found in the 1988 light curve, if it were due solely to spherical particle haze extinction. Recent studies (see for example, Rannou et al. 1995, Icarus, 188, 355 and Thomas-Osip et al. 2002, Icarus, submitted) have shown that it is likely that photochemical hazes on Titan are aggregate in nature. Fractal aggregate particles can have larger extinction efficiencies than equivalent mass spheres of the same material (Rannou et al. 1999, Planet. Space Sci., 47,385). We are, therefore, also re-examining the effect of a haze with an aggregate morphology on modeling of the 1988 occultation observations. This research has been supported in part by NSF Grant AST-0073447 and NASA Grant NAG5-10444.

Comparative study between the reflective optics and lens based system for microwave imaging system on KSTAR

DOE Office of Scientific and Technical Information (OSTI.GOV)

Lee, W.; Yun, G. S.; Nam, Y.

2010-10-15

Recently, two-dimensional microwave imaging diagnostics such as the electron cyclotron emission imaging (ECEI) system and microwave imaging reflectometry (MIR) have been developed to study magnetohydrodynamics instabilities and turbulence in magnetically confined plasmas. These imaging systems utilize large optics to collect passive emission or reflected radiation. The design of this optics can be classified into two different types: reflective or refractive optical systems. For instance, an ECEI/MIR system on the TEXTOR tokamak [Park et al., Rev. Sci. Instrum. 75, 3787 (2004)] employed the reflective optics which consisted of two large mirrors, while the TEXTOR ECEI upgrade [B. Tobias et al., Rev.more » Sci. Instrum. 80, 093502 (2009)] and systems on DIII-D, ASDEX-U, and KSTAR adopted refractive systems. Each system has advantages and disadvantages in the standing wave problem and optical aberrations. In this paper, a comparative study between the two optical systems has been performed in order to design a MIR system for KSTAR.« less

A generalized nonlocal vector calculus

NASA Astrophysics Data System (ADS)

Alali, Bacim; Liu, Kuo; Gunzburger, Max

2015-10-01

A nonlocal vector calculus was introduced in Du et al. (Math Model Meth Appl Sci 23:493-540, 2013) that has proved useful for the analysis of the peridynamics model of nonlocal mechanics and nonlocal diffusion models. A formulation is developed that provides a more general setting for the nonlocal vector calculus that is independent of particular nonlocal models. It is shown that general nonlocal calculus operators are integral operators with specific integral kernels. General nonlocal calculus properties are developed, including nonlocal integration by parts formula and Green's identities. The nonlocal vector calculus introduced in Du et al. (Math Model Meth Appl Sci 23:493-540, 2013) is shown to be recoverable from the general formulation as a special example. This special nonlocal vector calculus is used to reformulate the peridynamics equation of motion in terms of the nonlocal gradient operator and its adjoint. A new example of nonlocal vector calculus operators is introduced, which shows the potential use of the general formulation for general nonlocal models.

The Role of Oxytocin in Social Buffering: What Do Primate Studies Add?

PubMed

Crockford, Catherine; Deschner, Tobias; Wittig, Roman M

2017-09-02

The ability to maintain close social bonds impacts on reproductive success, longevity, stress and health in social mammals, including humans (Silk et al., Curr Biol 20(15):1359-1361, 2010; Crockford et al., Horm Behav 53(1):254-265, 2008; Wittig et al., Horm Behav 54(1):170-177, 2008; Archie et al., Proc R Soc B 281(1793):20141261, 2014; Cameron et al., Proc Natl Acad Sci U S A 106:13850-13853, 2009; Schülke et al., Curr Biol 20:2207-2210, 2010; Silk et al., Science 302:1231-1234, 2003; Holt-Lunstad et al., PLoS Med 7(7):e1000316, 2010). Close social bonds provide an important social support system, at least in part by acting as a buffer against the deleterious effects of chronic exposure to stressors (Young et al., Proc Natl Acad Sci U S A 51:18195-18200, 2014; Heinrichs et al., Biol Psychiatry 54:1389-1398, 2003). There is accumulating evidence that individuals that provide predictable affiliation or support to others (bond partners) may moderate the perception of the stressor as well as of the physiological stress response. The neuropeptide, oxytocin, may mediate social buffering by down-regulating HPA activity and thus reducing the stress response. However, much within this process remains unclear, such as whether oxytocin is always released when exposed to a stressor, whether more oxytocin is released if there is social support, what aspect of stress or social support triggers oxytocin release and whether social support in the absence of a stressor also impacts oxytocin release and HPA activity, during everyday life. We review the literature that addresses each of these questions in an attempt to clarify where future research effort will be helpful. A better understanding of these dynamics is likely to have implications for enhancing social and health gains from human social relationships.

Metabolic activity of subseafloor microbes in the South Pacific Gyre

NASA Astrophysics Data System (ADS)

Morono, Y.; Ito, M.; Terada, T.; Inagaki, F.

2013-12-01

The South Pacific Gyre (SPG) is characterized as the most oligotrophic open ocean environment. The sediment is rich in oxygen but poor in energy-sources such as reduced organic matter, and hence harbors very low numbers of microbial cells in relatively shallow subseafloor sediment (D'Hondt et al., 2009; Kallmeyer et al., 2012). In such an energy-limited sedimentary habitat, a small size of microbial community persists living functions with extraordinary low oxygen-consumption rate (Røy et al., 2012). During IODP Expedition 329, a series of sediment samples were successfully recovered from 7 drill sites (U1365-1371) from the seafloor to basement in the SPG, providing an unprecedented opportunity to study metabolic activity of the aerobic subseafloor microbial communities. We initiated incubation onboard by adding stable isotope-labeled substrates to the freshly collected sediment sample, such as 13C and/or 15N-labeled bicarbonate, glucose, amino acids, acetate, and ammonium under the (micro-) aerobic condition. One of the technological challenges in this study is to harvest microbial cells from very low-biomass sediment samples for the analysis using nano-scale secondary ion mass spectrometry (NanoSIMS). To address the technical issue, we improved existing cell separation technique for the SPG sediment samples with small inorganic zeolitic grains. By monitoring cell recovery rates through an image-based cell enumeration technique (Morono et al., 2009), we found that cell recovery rates in the SPG sediment samples are generally lower than those in other oceanographic settings (i.e., organic-rich ocean margin sediments). To gain higher cell recovery ratio, we applied multiple density gradient layers, resulting in the cell recovery ratio up to around 80-95% (Morono et al., in press). Then, using the newly developed cell separation technique, we successfully sorted enough number of microbial cells in small spots on the membrane (i.e., 103 to 105 cells per spot). NanoSIMS analysis showed incorporation of the supplemented stable isotope-labeled substrates after 1.5 year-incubation. The substrate incorporation rates of individual microbial cell ranged in average from 1/10 to 1/2 of those values previously observed in an organic-rich ocean margin sediment (Morono et al., 2011). References S. D'Hondt et al., Subseafloor sedimentary life in the South Pacific Gyre. Proc Natl Acad Sci USA 106, 11651 (2009) J. Kallmeyeret al., Global distribution of microbial abundance and biomass in subseafloor sediment. Proc Natl Acad Sci USA 109, 16213 (2012) H. Røy et al., Aerobic microbial respiration in 86-million-year-old deep-sea red clay. Science 336, 922 (2012) Y. Morono et al. Discriminative detection and enumeration of microbial life in marine subsurface sediments. ISME J 3, 503 (2009) Y. Morono et al., An Improved Cell Separation Technique for Marine Subsurface Sediments: Applications for High-throughput Analysis Using Flow Cytometry and Cell Sorting. Environ Microbiol, (2013) Y. Morono et al., Carbon and nitrogen assimilation in deep subseafloor microbial cells. Proc Natl Acad Sci USA 108, 18295 (2011)

A Physical Model of Cosmogenic Nuclide Production in Stony and Iron Meteoroids on the Basis of Simulation Experiments

NASA Astrophysics Data System (ADS)

Leya, I.; Lange, H.-J.; Michel, R.; Meltzow, B.; Herpers, U.; Busemann, H.; Wieler, R.; Dittrich-Hannen, B.; Suter, M.; Kubik, P. W.

1995-09-01

By extending and improving earlier model calculations [1-4] of cosmogenic nuclide production by GCR particles in extraterrestrial matter, we can now present a physical model without free parameters for a consistent description of GCR production rates in stony and iron meteoroids. The model takes explicitely into account p and n-induced reactions. GCR 4He particles are considered only approximately. It is based on depth-size and bulk-chemistry-dependent spectra of primary and secondary protons and of secondary neutrons calculated by HET and MORSE codes within the HERMES code system [5] and on the cross sections of the underlying reactions. Comprehensive and reliable sets of proton cross sections from thresholds up to 2.6 GeV exist now for many cosmogenic nuclides (see [6] for a review). For n-induced reactions the situation is not so good. Only a few data at low energies and practically no data at higher energies exist. GCR production of cosmogenic nuclides in stony meteoroids is already dominated by neutron-induced reactions for most meteoroid radii. In iron meteoroids neutrons are even more important because of the high mass numbers of the bulk and of consequently higher multiplicities for production of secondary neutrons. In order to overcome this problem, the necessary excitation functions of neutron-induced reactions were determined from experimental thick-target production rates by least-squares unfolding procedures using the code STAYS'L [7]. The data were produced in laboratory experiments under completely controlled conditions [8-11]. The unfolding procedure starts from guess functions (from threshold up to 900 MeV) based on all available experimental neutron cross sections and on theoretical ones calculated by the AREL [12] code which is a relativistic version of the hybrid model of pre-equilibrium reactions [13]. With the new neutron cross sections it is possible to describe simultanously all data from the simulation experiments with an accuracy of better than 10 % and to calculate consistent cosmogenic nuclide production rates in stony and iron meteoroids. The new model calculations are so far valid for 10Be, 26Al, 36Cl, 41Ca, 53Mn as well as He, Ne and Ar isotopes. The new theoretical production rates are compared with measured depth profiles in stony and iron meteorites and will be discussed with respect to primary GCR spectra and preatmospheric radii and exposure histories of stony and iron meteoroids. Acknowledgement: This work was partially supported by the Deutsche Forschungsgemeinschaft and the Swiss National Science Foundation. References: [1] Michel R. et al. (1991) Meteoritics, 26, 221-242. [2] Michel R. et al. (1995) Planet. Space Sci., in press. [3] Bhandari N. et al. (1993) GCA, 57, 2361-2375. [4] Herpers U. et al. (1995) Planet. Space Sci., in press. [5] Cloth P. et al. (1988) JUEL-2203. [6] Michel R. (1994) in Nuclear Data for Science and Technology (J. K. Dickens, ed.), 337-343, Am. Nucl. Soc., La Grange Park. [7] Perrey F. G. (1977) Code STAYS'L, NEA Data Bank, OECD Paris. [8] Michel R. et al. (1986) Nucl. Instr. Meth. Phys. Res., B16, 61-82. [9] Michel R. et al. (1989) Nucl. Instr. Meth. Phys. Res., B42, 76-100. [10] Michel R. et al. (1993) J. Radioanal. Nucl. Chem., 169, 13-25. [11] Michel R. et al. (1994) in Nuclear Data for Science and Technology (J. K. Dickens, ed.), 377-379, Am. Nucl. Soc., La Grange Park. [12] Blann M. (1994) Code AREL, personal communication to R. Michel. [13] Blann M. (1972) Phys. Rev. Lett., 27, 337-340.

Modeling Mercury

NASA Astrophysics Data System (ADS)

Burger, M. H.; Killen, R. M.; M, N.; Sarantos, M.; Crider, D. H.; Vervak, R. J.

2009-04-01

Mercury has a tenuous exosphere created by the combined effects of solar radiation and micrometeoroid bombardment on the surface and the interaction of the solar wind with Mercury's magnetic field and surface. Observations of this exosphere provide essential data necessary for understanding the composition and evolution of Mercury's surface, as well as the interaction between Mercury's magnetosphere with the solar wind. The sodium component of the exosphere has been well observed from the ground (see review by Killen et al., 2007). These observations have revealed a highly variable and inhomogeneous exosphere with emission often peaking in the polar regions. Radiation acceleration drives exospheric escape producing a sodium tail pointing away from the sun which has been detected up to 1400 Mercury radii from the planet (Potter et al. 2002; Baumgardner et al. 2008). Calcium has also been observed in Mercury's exosphere showing a distribution distinct from sodium, although also variable (Killen et al. 2005). During the first two encounters with Mercury by MESSENGER, observations of the exosphere were made by the UltraViolet and Visible Spectrometer (UVVS) channel of the Mercury Atmospheric and Surface Composition Spectrometer (MASCS). Sodium and calcium emission were detected during both flybys, and magnesium was detected for the first time in Mercury's exosphere during the second flyby. The spatial distributions of these species showed significant, unexpected differences which suggest differences in the mechanisms responsible for releasing them from the surface. We present a Monte-Carlo model of sodium, magnesium, and calcium in Mercury's exosphere. The important source mechanisms for ejecting these species from the surface are sputtering by solar wind ions, photon-stimulated desorption, and micrometeoroid impact vaporization. Thermal desorption on the dayside does not supply enough energy to significantly populate the exosphere, although it does play a role in redistributing volatiles over the surface. In addition, atomic calcium can be produced from the dissociation of Ca-bearing molecules, such as CaO, which can be formed in impact vapors. The primary loss processes are the escape of neutrals ejected with sufficient energy and photoionization. The former process is supplemented by radiation pressure which accelerates neutrals anti-sunward such that escaping neutrals form a tail pointing away from the sun. Because Mercury's heliocentric distance and radial velocity vary during its orbit, both loss processes are functions of Mercury's true anomaly. We also consider the spatial distribution of the surface source. Impact vaporization is roughly isotropic over the surface, although there may be a leading/trailing asymmetry in the impact rate due to Mercury's orbital motion. Sputtering is confined to regions where the solar wind can impact the surface, which is shielded somewhat by the internal magnetic field. The surface regions vulnerable depend on the solar wind conditions. References: Baumgardner et al., GRL, 35, L03201, 2008. Killen, R.M. et al., Space Sci. Rev. 132, 433-509, 2007. Killen, R.M. et al., Icarus, 173, 300-311, 2005. Potter et al., Meteoritics & Planetary Sci., 37, 1165, 2002.

Electromagnetic compatibility test report for the tethered satellite data acquisition and control assembly

NASA Astrophysics Data System (ADS)

Hoskins, Douglas; Snead, Robert

1988-05-01

This report details the results of an electromagnetic compatibility test on the SCI Systems Data Acquisition and Control Assembly (DACA). This assembly is an electronic processor which controls the central communication link from the Tethered Satellite System (TSS) to the Space Transportation System Orbiter Space Shuttle.

Infrared Rydberg Transitions in B Stars.

NASA Astrophysics Data System (ADS)

Sigut, Thomas Allan Aaron

1995-01-01

The infrared solar spectrum exhibits emission lines near 12 μm from the Mg scI high-l Rydberg transitions 6g - 7h and 6h - 7i. Chang et al. (1991) demonstrated that the emission arises from small deviations in the populations of these Rydberg levels from their thermodynamic equilibrium values. In this thesis, the possible operation of this emission mechanism is investigated in the B stars by performing non-LTE radiative transfer calculations for the high-l Rydberg transitions of Mg scII and O scI. Highly realistic atomic models are employed, complete in energy levels and radiative transitions far into the Rydberg regime. For Mg scII, the collisional excitation rates are improved by computing collision strengths in a 10 state close-coupling approximation using the R-matrix method. The collisional excitation rates derived from these collisions strengths include the full effects of autoionizing resonances and have an expected accuracy of +/-10% for transitions between levels lying low in energy in the close-coupling expansion. For Mg scII, wide-ranging infrared emission is found, spanning the entire range of B spectral types. The emission is caused by the same mechanism operative in the Rydberg levels of Mg scI in the sun. Small divergences between the Rydberg departure coefficients produce rising monochromatic source functions and emission. Flux profiles of the Mg scII high-l ( Delta n = +1) transitions from n = 4 and 5 show an emission peak superposed on wider absorption trough, similar in form to the solar Mg scI lines, while for higher n, the profiles are in full emission. The strongest emission is predicted for transitions from n = 5, 6, and 7 and strongly increases for lower surface gravities where the rates of thermalizing collisions are lower. The emission strengths reach maxima of Flambda /Fc ~ 1.15 and Wlambda ~ -0.1 A. Transitions from higher n exhibit progressively lower continuum contrasts due to the steep rise with wavelength of the continuous opacity in the infrared and increased Stark broadening. The largest source of potential uncertainty affecting the emission strengths is the uncertain scale of the collisional excitation rates between the Rydberg levels. However, reasonable variations of these rates does not eliminate the emission. Although small divergences occur between the Rydberg departure coefficients of O scI, wide-ranging infrared emission is not predicted. Only small self-reversals in the cores of the high-l transitions from n = 4 and 5 are seen and then only at the lowest surface gravities. The failure of O scI to produce significant emission, or more precisely, significant Rydberg population divergences, can be attributed to the lack of strong ultraviolet photoionization rates from its lower energy levels, the increased collisional coupling between its more closely spaced Rydberg levels, and the longer wavelengths of its Rydberg transitions. Considerable uncertainty exists in the prediction of the absolute infrared line strengths of O scI due to uncertainty in the exact treatment or radiative transfer in the resonance line and in the magnitude of the collisional excitation rates among the Rydberg levels. However, these uncertainties do not alter the basic conclusion of no significant emission from the high-l Rydberg transitions of O scI in B stars.

Complement and Antibody-Mediated Enhancement of Erythrocyte Invasion by Plasmodium Falciparum

DTIC Science & Technology

2016-04-01

Waki et al., 1995; Yoneto et al., 2001). However, the doses of antibody in those studies were much higher, usually given in milligram amounts and...erythrocyte receptor for Plasmodium falciparum PfRh4 invasion ligand. Proc. Natl. Acad. Sci. U. S. A. 107, 17327–17332. Waki , S., Uehara, S., Kanbe, K...infections. J. Immunol. 126, 1826–1828. Wold Health Organization, 2013. World Malaria Report 2013 (Geneva). Yoneto, T., Waki , S., Takai, T., Tagawa, Y

Erratum: Lakes et al (2017).

PubMed

2018-05-01

In the article by Lakes KD, Abdullah MM, Youssef J, et al. Assessing parent perceptions of physical activity in families of toddlers with neurodevelopmental disorders: The Parent Perceptions of Physical Activity Scale (PPPAS), Pediatr Exerc Sci. 2017; 29: 396-407, https://doi.org/10.1123/pes.2016-0213 , an author's name was incorrectly listed. Shlomit Aizik should have been listed as Shlomit Radom-Aizik. The online version of this article has been corrected. We apologize for this error.

Introducing the potential of antimicrobial materials for human and robotic spaceflight activities

NASA Astrophysics Data System (ADS)

Hahn, Claudia; Reitz, Guenther; Moeller, Ralf; Rettberg, Petra; Hans, Michael; Muecklich, Frank

One major goal of space research is to discover past or present life on foreign planets such as Mars (Horneck et al., 2010). To detect extraterrestrial life on other planets it is important to prevent microbial contamination imported from the Earth, also known as forward contamination. Until now missions to Mars are solely progressed by robots like the Mars Science Laboratory mission with the Curiosity lander. The assembly of spacecraft components is performed in special bioburden controlled clean rooms. Nevertheless, the microbial diversity in these clean rooms is enormous (Vaishampayan et al., 2013). The propagation of microorganisms and in particular the spread of environmental and human-associated species can be facilitated through numerous exposure routes (e.g., air, personal contact, water, excretions, etc.). Besides robotic missions, on-board the International Space Station (ISS) and in (future) space vehicles for long-term journeys to special targets of astrobiological interests in the solar system, astronauts will have the unique opportunity for scientific exploration. The manned exploration of new environments (e.g. asteroids, Mars) require long-term residence in confined stations and habitats (e.g. space stations, spacecraft, vehicles). During these missions, the health of the crew members has to be protected, and the integrity of the materials and facilities should be carefully monitored (van Houdt et al., 2012). A major concern is the microbiological burden in enclosed environments, where human inhabitants are continuously exposed to potential harmful microorganisms over a long-duration, which may affect the health and performance of the human subjects (Horneck et al., 2010) in addition to potential risks by biofilm formation and biocorrosion of materials. In both scenarios, the application of antimicrobial surfaces is an encouraging approach to reduce microorganisms in a straightforward way. Antimicrobial agents and materials are characterized by their relative short reaction time, long efficiency and functionality, broad application to reduce (micro-)biological contamination, high inactivation rates, sustainability, and avoidance of microbial resistance. Methods like contact killing measurement are one of the reliable ways to examine the effect of metal surfaces on the inactivation of microorganisms. We conducted contact killing experiments, in which we exposed human-associated microorganisms like Escherichia coli and Staphylococcus sp. on copper and stainless steel to detect and evaluate the potential incorporation of those materials in future spacecraft components. In contrast to an exposure on stainless steel microorganisms exposed on copper died within a few hours and therefore do not have the ability to proliferate, build protecting biofilms or even survive. The application of different surfaces and antimicrobial substances such as copper and silver, as well as testing other model organisms are still under examination. The results of our experiments are also very promising to other research areas, e.g., clinical application. Here, we would like to present our first data and ideas on the utilization of antimicrobial metal-based surfaces for human and robotic spaceflight activities as a beneficial method to reduce microbial contamination. \\underline{References} Horneck G et al. (2010) Space microbiology. Microbiol. Mol. Biol. Rev. 74:121-156. Vaishampayan P et al. (2013) New perspectives on viable microbial communities in low-biomass cleanroom environments. ISME J. 7:312-324. van Houdt R et al. (2012) Microbial contamination monitoring and control during human space missions. Planet. Space Sci. 60:115-120.

Holocene geological records of flood regime in French Alps

NASA Astrophysics Data System (ADS)

Arnaud, Fabien; Wilhelm, Bruno; Giguet-Covex, Charline; Jenny, Jean-Philippe; Fouinat, Laurent; Sabatier, Pierre; Debret, Maxime; Révillon, Sidonie; Chapron, Emmanuel; Revel, Marie

2014-05-01

In this paper we present a review of a ca. 10-years research effort (1-9) aiming at reconstructing floods dynamics in in French Alps through the Holocene, based on lake sediment records. We will particularly discuss how such geological records can be considered as representative of past climate. This implies a wise interpretation of data in order to really understand "what does the core really says". Namely, we showed that different lake systems record different types of flood events. Low altitude lakes, fed by large-scale catchment areas are more sensitive to regional heavy rainfall events (2-5), whereas high altitude small lakes record local extreme rainfall events (6). Moreover, human societies' development must be taken into account as it is susceptible to modulate the climate-geological record relationship (7). Altogether our data permit the establishment of a Holocene-long perspective upon both regional heavy rainfall and torrential activities in high elevation sites. We hence show that both types of events frequency co-evolve in Northern as well as Southern French Alps where Holocene colder spells generally present higher flood frequencies (6-9). On the other hand, intensities of torrential events present a North-South opposite pattern: during warm spells (e.g. the Medieval Warm Period or nowadays), northern Alps are subject to rare but extremely intense heavy rainfall events, whereas in the southern Alps torrential floods are both rare and weak. During cold spells (e.g. the Little Ice Age), the inverse pattern is observed: torrential floods are more frequent everywhere and above-average intensity in Southern Alps. This point is particularly important for risk management in mountain areas in a context of global warming. Our results point out how complex can be the response of regional system to global climate changes. We are hence far from completely understanding this complexity which is moreover imperfectly simulated by climate models. As geological records represent the only way to reconstruct long-term trends in flood regimes, more efforts must still be pursued to get a more complete image of this complexity and further improve climate models. 1. Chapron et al. The Holocene 12, 177-185 (2002) 2. Arnaud et al. Quat. Sci. Rev. 51, 81-92 (2012) 3. Debret et al. Quat. Sci. Rev. 29, 2185-2200 (2010) 4. Arnaud et al. The Holocene 15, 420-428 (2005) 5. Revel-Rolland et al. Chem. Geol. 224, 183-200 (2005) 6. Wilhelm et al. Clim. Change 113, 563-581 (2012) 7. Giguet-Covex et al. Quat. Res. 77, 12-22 (2012) 8. Wilhelm et al. Quat. Res. 78, 1-12 (2012) 9. Wilhelm et al. J. Quat. Sci. 28, 189-199 (2013)

Public Data Set: Control and Automation of the Pegasus Multi-point Thomson Scattering System

DOE Data Explorer

Bodner, Grant M. [University of Wisconsin-Madison] (ORCID:0000000324979172); Bongard, Michael W. [University of Wisconsin-Madison] (ORCID:0000000231609746); Fonck, Raymond J. [University of Wisconsin-Madison] (ORCID:0000000294386762); Reusch, Joshua A. [University of Wisconsin-Madison] (ORCID:0000000284249422); Rodriguez Sanchez, Cuauhtemoc [University of Wisconsin-Madison] (ORCID:0000000334712586); Schlossberg, David J. [University of Wisconsin-Madison] (ORCID:0000000287139448)

2016-08-12

This public data set contains openly-documented, machine readable digital research data corresponding to figures published in G.M. Bodner et al., 'Control and Automation of the Pegasus Multi-point Thomson Scattering System,' Rev. Sci. Instrum. 87, 11E523 (2016).

One-Year Observations of Jupiter by the Jovian Infrared Auroral Mapper on Juno

NASA Astrophysics Data System (ADS)

Adriani, A.; Mura, A.; Bolton, S. J.; Connerney, J. E. P.; Levin, S.; Becker, H. N.; Bagenal, F.; Hansen, C. J.; Orton, G.; Gladstone, R.; Kurth, W. S.; Mauk, B.; Valek, P. W.

2017-12-01

The Jovian InfraRed Auroral Mapper (JIRAM) [1] on board the Juno [2,3] spacecraft, is equipped with an infrared camera and a spectrometer working in the spectral range 2-5 μm. JIRAM was built to study the infrared aurora of Jupiter as well as to map the planet's atmosphere in the 5 µm spectral region. The spectroscopic observations are used for studying clouds and measuring the abundance of some chemical species that have importance in the atmosphere's chemistry, microphysics and dynamics like water, ammonia and phosphine. During 2017 the instrument will operate during all 7 of Juno's Jupiter flybys. JIRAM has performed several observations of the polar regions of the planet addressing the aurora and the atmosphere. Unprecedented views of the aurora and the polar atmospheric structures have been obtained. We present a survey of the most significant observations that the instrument has performed during the current year. [1] Adriani A. et al., JIRAM, the Jovian Infrared Auroral Mapper. Space Sci. Rew., DOI 10.1007/s11214-014-0094-y, 2014. [2] Bolton S.J. et al., Jupiter's interior and deep atmosphere: The initial pole-to-pole passes with the Juno spacecraft. Science DOI: 10.1126/science.aal2108, 2017. [3] Connerney J. E.P. et al., Jupiter's magnetosphere and aurorae observed by the Juno spacecraft during its first polar orbits. Science, DOI: 10.1126/science.aam5928, 2017.

Studies of giant magnetoresistance and interfacial structure in Cu/Co and Co/Re multilayers

NASA Astrophysics Data System (ADS)

Setty, Arun; Fernando, G.; Cooper, B. R.

2003-03-01

A study of giant magnetoresistance (GMR) in the Cu/Co [1]and Co/Re multilayer [2,3] systems is presented. The role of interface structure in such systems is significant, and is being investigated using an ab-initio based approach [4]. The role of intermixing [5], impurities and growth textures have been considered. Structural relaxation is taken into account using Hellman-Feynman and symmetry-based approaches. We find lattice spacings in agreement with experiment, energetically establish the favored growth textures and find results motivating the existence of the observed wavy interface in the Cu/Co system [6]. The transport properties of these multilayer systems will be studied using a theoretical model [7] incorporating material parameters obtained from the multiscale modeling approach we envisage. [1] S.S.P. Parkin, Z.G. Li, and D. J. Smith, Appl. Phys. Lett., 58, 2710-2712 (1991). [2] T. Charlton et al, Phys. Rev. B 63, 094404 (2001) [3] T. Charlton et al, Phys. Rev. B 59, 11897-11908 (1999) [4] C. Villagonzalo, A.K. Setty and B.R. Cooper, submitted to Phys. Rev. [5] J. Fassbender, R. Allenspach, and U. Durig. Surf. Sci., 383, L742-L748, (1997). [6] D.J. Larson et al, Appl. Phys. Lett., 73:1125-1127, (1998). [7] J. C. Slonczewski, Phys. Rev. B 39, 6995 (1989).

Hydrated Minerals in Circumpolar Terrains: Geographic Distribution, Mineralogical Composition and Possible Origins

NASA Astrophysics Data System (ADS)

Langevin, Y.; Poulet, F.; Fishbaugh, K. E.; Roach, L.; Vincendon, M.; Gondet, B.; Bibring, J.; Murchie, S.

2007-12-01

The nearly global mapping provided at a scale of a few km by the OMEGA Vis/NIR imaging spectrometer on board Mars Express revealed that hydrated minerals on Mars are mostly observed in ancient terrains (Bibring et al., 2005). These discoveries led to the conclusion that surface water on Mars was mainly present early in the history of the planet, and that Mars has remained cold and dry during the last 3 billion years (Bibring et al., 2006). The observation by OMEGA of a very strong calcium sulfate signature (most likely dominated by gypsum) within the boundaries of the Olympia Planitia Dune field (Langevin et al., 2005) is a major puzzle as this geological feature is at most a few 100 m.y. old. An independent analysis of the OMEGA data (Horgan et al. 2007) confirmed the results of Langevin et al. (2005), in particular the identification of gypsum as the dominant mineralogical hydrated species in the dune field. The extended region richest in gypsum (~ 60 km x 200 km) remained unresolved at a resolution of 1 km/pixel (Langevin et al., 2006). With its 20 m resolution, CRISM, the Vis/NIR imaging spectrometer on board MRO, secured the relationship between the gypsum signature and the dune field as well as its absence over the "basal unit" (only a few pixels wide in OMEGA data) which is exposed between the dune field and the ice (Roach et al., 2007). CRISM showed that the gypsum signatures were highest over dune crests and weakest over exposed bedrock. Mineralogical modeling of the CRISM and OMEGA spectra shows that Gypsum represents at least 60% of the dune material in the eastern part of the Olympia field and decreases towards the western part. This lower limit has been raised since then by accounting for aerosol contributions which reduce the strength of absorption bands. The low albedo (< 20%) requires significant intimate and/or intra- mixture of dark material. The low thermal inertia (Herkenhoff and Vasavada, 1999) is difficult to reconcile with morphologic evidence for induration (Schatz et al., 2006). Weaker occurrences of the 1.93 µm OH stretch band have been observed in other northern and southern circumpolar locations. Sulfates and hydrated oxides provide much better matches for these signatures than phyllosilicates. The formation of large amounts of hydrated sulfates in the relatively young northern circumpolar terrains requires a source of sulfur (already present in soils? volcanic activity?) as well as water, which most likely is provided by outflows from the nearby polar cap (Fishbaugh et al., 2007). This process for generating hydrated minerals is distinct from that which was active during the first few hundred million years of the history of the planet. Bibring et al., Science 307, p. 1576-1581 (2005); Bibring et al., Science 312, p. 400-404 (2006); Feldman et al., Lunar Planet. Sci. 38 #2311 (2007); Fishbaugh et al., J. Geophys. Res. 112, E07002 (2007); Herkenhoff and Vasavada, J. Geophys. Res. 104, 16484. Horgan et al., 7th Int. Conf. on Mars #3241 (2007); Langevin et al., Science 307, p. 1581-1583 ; Langevin et al., Lunar Planet. Sci. 36 #1652 (2005) ; Roach et al., Lunar Planet. Sci. 38 #1970 (2007) ; Schatz et al., J. Geophys. Res. 111, E04006 (2006).

Proceedings of oceans 87. The ocean - an international workplace

DOE Office of Scientific and Technical Information (OSTI.GOV)

Not Available

1987-01-01

This book includes proceedings containing 347 papers. Some of the topics are: ICE -Cold ocean and ice research; ICE-1-Icebergs; ICE-2-Sea ice and structures; IE-3-Cold ocean instrumentation; ICE-4-Ocean and ice; INS-Oceanographic instrumentation; INS-1-Acoustic Doppler Current profilers; ENG-1-New solutions to old problems; ENG-2-energy from the ocean; ENG-3-Cables and connectors; POL-Policy, education and technology transfer; POL-1-International issues; POL-2-Ocean space utilization; POL-3-Economics, planning and management; SCI-6-fish stock assessment; ACI-7-Coastal currents and sediment; SCI-9-Satellite navigation; SCI-10-Deep sea minerals and methods of recovery; ODS-Fifth working symposium on oceanographic data system; ODS-1-Data base management; UND-Underwater work systems; UND-1-Diving for science.

KENNEDY SPACE CENTER, FLA. - At Vandenberg Air Force Base, Calif., the Pegasus launch vehicle is moved toward its hangar. The Pegasus will carry the SciSat-1 spacecraft in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

NASA Image and Video Library

2003-06-27

KENNEDY SPACE CENTER, FLA. - At Vandenberg Air Force Base, Calif., the Pegasus launch vehicle is moved toward its hangar. The Pegasus will carry the SciSat-1 spacecraft in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

KENNEDY SPACE CENTER, FLA. - The Pegasus launch vehicle is moved back to its hangar at Vandenberg Air Force Base, Calif. The Pegasus will carry the SciSat-1 spacecraft in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

NASA Image and Video Library

2003-06-27

KENNEDY SPACE CENTER, FLA. - The Pegasus launch vehicle is moved back to its hangar at Vandenberg Air Force Base, Calif. The Pegasus will carry the SciSat-1 spacecraft in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

KENNEDY SPACE CENTER, FLA. - At Vandenberg Air Force Base, Calif., the Pegasus launch vehicle is moved into its hangar. The Pegasus will carry the SciSat-1 spacecraft in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

NASA Image and Video Library

2003-06-27

KENNEDY SPACE CENTER, FLA. - At Vandenberg Air Force Base, Calif., the Pegasus launch vehicle is moved into its hangar. The Pegasus will carry the SciSat-1 spacecraft in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

Differential Adaptations of the Musculoskeletal System after Spinal Cord Contusion and Transection in Rats.

PubMed

Lin, Ching-Yi; Androjna, Charlie; Rozic, Richard; Nguyen, Bichtram; Parsons, Brett; Midura, Ronald J; Lee, Yu-Shang

2018-04-05

Spinal cord injury (SCI) causes impaired neuronal function with associated deficits in the musculoskeletal system, which can lead to permanent disability. Here, the impact of SCI on in vivo musculoskeletal adaptation was determined by studying deficits in locomotor function and analyzing changes that occur in the muscle and bone compartments within the rat hindlimb after contusion or transection SCI. Analyses of locomotor patterns, as assessed via the Basso, Beattie, and Bresnahan (BBB) rating scale, revealed that transection animals showed significant deficits, while the contusion group had moderate deficits, compared with naïve groups. Muscle myofiber cross-sectional areas (CSA) of both the soleus and tibialis anterior muscles were significantly decreased three months after contusion SCI. Such decreases in CSA were even more dramatic in the transection SCI group, suggesting a dependence on muscle activity, which is further validated by the correlation analyses between BBB score and myofiber CSA. Bone compartment analyses, however, revealed that transection animals showed the most significant deficits, while contusion animals showed no significant differences in the trabecular bone content within the proximal tibia compartment. In general, values of bone volume per total bone volume (BV/TV) were similar across the SCI groups. Significant decreases were observed, however, in the transection animals for bone mineral content, bone mineral density, and three-dimensional trabecular structure parameters (trabecular number, thickness, and spacing) compared with the naïve and contusion groups. Together, these findings suggest an altered musculoskeletal system can be correlated directly to motor dysfunctions seen after SCI.

The Virtual Earth-Solar Observatory of the SCiESMEX

NASA Astrophysics Data System (ADS)

De la Luz, V.; Gonzalez-Esparza, A.; Cifuentes-Nava, G.

2015-12-01

The Mexican Space Weather Service (SCiESMEX, http://www.sciesmex.unam.mx) started operations in October 2014. The project includes the Virtual Earth-Solar Observatory (VESO, http://www.veso.unam.mx). The VESO is a improved project wich objetive is integrate the space weather instrumentation network from the National Autonomous University of Mexico (UNAM). The network includes the Mexican Array Radiotelescope (MEXART), the Callisto receptor (MEXART), a Neutron Telescope, a Cosmic Ray Telescope. the Schumann Antenna, the National Magnetic Service, and the mexican GPS network (TlalocNet). The VESO facility is located at the Geophysics Institute campus Michoacan (UNAM). We offer the service of data store, real-time data, and quasi real-time data. The hardware of VESO includes a High Performance Computer (HPC) dedicated specially to big data storage.

Richard Ahrenkiel | NREL

Science.gov Websites

Kuciauskas, J Tynan, "Dual-sensor technique for characterization of carrier lifetime decay transients in semiconductors", Journal of Applied Physics 116 (21), 214510 (2014) J. Moseley, M.M. Al-Jassim, H.R For Contactless Measurement of Carrier Lifetime", J. Vac. Sci. Technol. B 31, 04D113 R. K

Distributed Scaffolding: Synergy in Technology-Enhanced Learning Environments

ERIC Educational Resources Information Center

Ustunel, Hale H.; Tokel, Saniye Tugba

2018-01-01

When technology is employed challenges increase in learning environments. Kim et al. ("Sci Educ" 91(6):1010-1030, 2007) presented a pedagogical framework that provides a valid technology-enhanced learning environment. The purpose of the present design-based study was to investigate the micro context dimension of this framework and to…

Characterization and Modeling of Insect Swarms Using tools from Fluid Dynamics

DTIC Science & Technology

2016-09-01

Scientific Reports, (01 2013): 1073 . doi: 10.1038/srep01073 James G. Puckett, Douglas H. Kelley, Nicholas T. Ouellette. Searching for effective...dynamics of laboratory insect swarms,” Sci. Rep. 3, 1073 (2013). [Ouellette et al. 2006] N. T. Ouellette, H. Xu, and E. Bodenschatz, “A quantitative

Enhanced gluten properties in soft kernel durum wheat

USDA-ARS?s Scientific Manuscript database

Soft kernel durum wheat is a relatively recent development (Morris et al. 2011 Crop Sci. 51:114). The soft kernel trait exerts profound effects on kernel texture, flour milling including break flour yield, milling energy, and starch damage, and dough water absorption (DWA). With the caveat of reduce...

Apoptosis and Tumor Progressionin Prostate Cancer

DTIC Science & Technology

2005-02-01

control. Proc Natl Acad Sci USA 94: 10057- 10062 . 5. Colombel M, Symmans F, et al. (1993): Detection of the apoptosis-suppressing oncoprotein bcl-2 in...hours prior to treatment. After treatment, cells were washed with phosphate buffered saline ( PBS ) and fixed in 500 [tL 0.2% glutaraldehyde in water for

The Exosphere of Ceres Generated by Photolysis and Radiolysis

NASA Astrophysics Data System (ADS)

Tseng, W. L.; Ip, W. H.; Kuan, Y. J.

2016-12-01

Ceres is the largest object (with a diameter of 950 km) among the main-belt asteroids. The OH cloud, the photodissociated products of H2O, was suggested by the IUE (International Ultraviolet Explorer) observations to be present around Ceres (A'Hearn and Feldman, 1992). Recently, Kuppers et al. (2014) reported a direct detection of water vapor by Herschel that > 1026 molecules s-1was produced from localized sources on Ceres' surface. Most excitingly, the Dawn images showed that a haze layer consisting of water-ice particles and dust was found above the Occator crater (Nathues et al., 2015). The haze was also shown to have a diurnal change of brightness, indicating a comet-like sublimation activity. In addition, subsurface outgassing (e.g., cryovolcanism and/or the plume activity similar to that found in Enceladus) is another possible source mechanism, which is not fully understood yet. Following the Ceres' exospheric model of Tu et al. (2014), here we focus on O2, O3 and H2O2 molecules, which are the primary products of radiolytic and photolytic decomposition of water ice, and possibly the CO2 and SO2 molecules produced from the impurities. We will compute the source rates from various production mechanisms and simulate the cloud morphologies. Then we will compare with the available data (e.g., the atomic oxygen emission observed by HST from Roth et al., 2016) and seek for any evidence in the ground-based millimeter/submillimeter observations. Understanding the chemical composition of Ceres and its evolved exosphere, in analogy to comets and the icy satellites, would reveal the secret of the origin and evolution of the solar system. 1. A'Hearn, M.F., Feldman, P.D., (1992) Water vaporization on Ceres. Icarus 98, 389-407. 2. Küppers, M., et al., (2014) Localized sources of water vapour on the dwarf planet (1) Ceres. Nature 505, 525-527. 3. Nathues, A., et al. (2015), Sublimation in bright spots on (1) Ceres, Nature, 528(7581), 237-240. 4. Tu, L., W.-H. Ip, and Y.-C. Wang (2014), A sublimation-driven exospheric model of Ceres, Planet. Space Sci., 104, 157-162. 5. Roth, L., et al. (2016), Constraints on an exosphere at Ceres from Hubble Space Telescope observations, Geophys. Res. Lett., 43, 2465-2472.

Determine the Role of Canonical Wnt Signaling in Ovarian Tumorigenesis

DTIC Science & Technology

2012-10-01

Acad Sci U S A, 1999. 96(4): p. 1603-8. 11. Kuilman, T., et al., The essence of senescence. Genes Dev, 2010. 24(22): p. 2463- 79. 12. Bernardi, R...Tu,1 Katherine M. Aird,1 Benjamin G. Bitler,1 Jasmine P. Nicodemus,1 Neil Beeharry,2 Bing Xia,3 Tim J. Yen,2 and Rugang Zhang1,2,* 1Women’s Cancer...Bitler, Jasmine P. Nicodemus, Hua Li, et al. Senescence Wnt5a Suppresses Epithelial Ovarian Cancer by Promoting Cellular Updated Version

Comment on "Timing and nature of the Xinlin-Xiguitu Ocean: constraints from ophiolitic gabbros in the northern Great Xing'an Range, eastern Central Asian Orogenic Belt" by Feng et al. (2016)

NASA Astrophysics Data System (ADS)

Ni, Dong-Hong

2017-09-01

We disagree the transitional supra-subduction zone model of Feng et al. (Int J Earth Sci (Geol Rundsch) 105:491-505, 2016) for the tectonic setting of Jifeng ophiolite suite in NE China. Existence of the komatiite in the Jifeng ophiolite indicates an oceanic plateau environment for this ophiolite suite within the so-called Xinlin-Xiguitu ocean.

Interface-induced localization in AlSb/InAs heterostructures

NASA Astrophysics Data System (ADS)

Shaw, M. J.; Briddon, P. R.; Jaros, M.

1995-12-01

The existence of localized states at perfect InSb-like interfaces in AlSb/InAs superlattices is predicted from ab initio pseudopotential calculations. Localized states are predicted in both the valence and conduction bands, the former being identifiable with the interface states proposed by Kroemer, Nguyen, and Brar [J. Vac. Sci. Technol. 10, 1769 (1990)]. The existence of these interface localized states is invoked to explain the reported experimental dependence of the band gap upon interface types in such superlattices.

Reconstructing latent dynamical noise for better forecasting observables

NASA Astrophysics Data System (ADS)

Hirata, Yoshito

2018-03-01

I propose a method for reconstructing multi-dimensional dynamical noise inspired by the embedding theorem of Muldoon et al. [Dyn. Stab. Syst. 13, 175 (1998)] by regarding multiple predictions as different observables. Then, applying the embedding theorem by Stark et al. [J. Nonlinear Sci. 13, 519 (2003)] for a forced system, I produce time series forecast by supplying the reconstructed past dynamical noise as auxiliary information. I demonstrate the proposed method on toy models driven by auto-regressive models or independent Gaussian noise.

Molecular Profiles for Lung Cancer Pathogenesis and Detection in US Veterans

DTIC Science & Technology

2011-10-01

expression data was analyzed using the BRB-ArrayTools v .4.1.0 developed by Dr. Richard Simon and the BRB-ArrayTools Development Team and then normalized...14. Spira A, Beane J, Shah V , et al. Effects of cigarette smoke on the human airway epithelial cell transcriptome. Proc Natl Acad Sci U S A 2004;101...10143-10148 15. Spira A, Beane JE, Shah V , et al. Airway epithelial gene expression in the diagnostic evaluation of smokers with suspect lung cancer

Molecular Profiles for Lung Cancer Pathogenesis and Detection in US Veterans

DTIC Science & Technology

2011-10-01

data was analyzed using the BRB-ArrayTools v .4.1.0 developed by Dr. Richard Simon and the BRB-ArrayTools Development Team and then normalized and log...Spira A, Beane J, Shah V , et al. Effects of cigarette smoke on the human airway epithelial cell transcriptome. Proc Natl Acad Sci U S A 2004;101:10143...10148 15. Spira A, Beane JE, Shah V , et al. Airway epithelial gene expression in the diagnostic evaluation of smokers with suspect lung cancer. Nat

Methods Development for the Isolation and Culture of Primary Corneal Endothelial Cells

DTIC Science & Technology

2017-02-01

1989 Yue et al. described methods that reached a 59% success rate in supporting human CEC growth using corneal tissue obtained from donors over 20...delayed-onset mustard gas keratitis: report of 48 patients and review of literature. Ophthalmology 2005; 112(4): 617-25. 6. Kadar T, Dachir S, Cohen L...toxicity following corneal exposure to sulfur mustard vapor. Invest Ophthalmol Vis Sci 2013; 54(10): 6735-44. 9. Kadar T, Cohen M, Cohen L, et al

Ambient seismic noise applications for Titan

NASA Astrophysics Data System (ADS)

Jackson, J. M.; Zhan, Z.; Clayton, R. W.; Helmberger, D. V.; Tsai, V. C.

2010-12-01

Titan is Saturn’s largest moon and is host to a myriad of surface, crustal, and perhaps interior dynamic processes (e.g., Lunine & Lorenz 2009; Sotin et al. 2009). Although recent gravity data put constraints on the nature of Titan’s deep interior (Iess et al. 2010), details regarding the layering and crustal structure remain poorly constrained. For example, the crustal thickness derived from modeling of the gravity data suggests a value ~100 km, but with a large uncertainty. There may exist a subsurface ocean or reservoirs of liquid that actively connects with Titan’s hyrdrocarbon-bearing lakes and atmosphere. Cross-correlation of ambient seismic noise is an emerging method to study crustal structures (e.g., Shapiro et al. 2005). Recent results show that under certain conditions, such as post-critical reflections, the Moho-reflected shear wave (SmS) can be clearly identified with ambient seismic noise [Zhan et al. 2010]. Titan may represent a plausible planetary body to apply the methods of ambient seismic noise, thereby providing a unique opportunity to better understand the interior of an icy body in our solar system. We will explore the use of ambient seismic noise on Titan and assess its application to determine interior structures, such as signals expected for different crust-(ocean)-mantle boundary depths. References: Iess, L. et al. (2010), Science 327: 1367-1369 Lunine, J.I. and Lorenz, R.D. (2009), Ann. Rev. Earth Planet. Sci. 37: 299-320. Shapiro et al. (2005), Science 307: 1615-1618. Sotin et al. (2009), in Titan from Cassini-Huygens: 61-73. R.H. Brown, J.-P. Lebreton, J. Hunter Waite, Eds. Zhan, Z. et al. (2010), Geophys. J. Int. doi: 10.1111/j/1365-246X.2010.04625.x Acknowledgments: Parts of this work grew out of discussions during a mini study at the Keck Institute for Space Studies, which is funded by the W. M. Keck Foundation.

Oxygen isotope heterogeneity of the mantle beneath the Canary Islands: a discussion of the paper of Gurenko et al.

NASA Astrophysics Data System (ADS)

Day, James M. D.; Macpherson, Colin G.; Lowry, David; Pearson, D. Graham

2012-07-01

Gurenko et al. (Contrib Mineral Petrol 162:349-363, 2011) report laser-assisted fluorination (LF) and secondary ionization mass spectrometry (SIMS) 18O/16O datasets for olivine grains from the Canary Islands of Gran Canaria, Tenerife, La Gomera, La Palma and El Hierro. As with prior studies of oxygen isotopes in Canary Island lavas (e.g. Thirlwall et al. Chem Geol 135:233-262, 1997; Day et al. Geology 37:555-558, 2009, Geochim Cosmochim Acta 74:6565-6589, 2010), these authors find variations in δ18Ool (~4.6-6.0 ‰) beyond that measured for mantle peridotite olivine (Mattey et al. Earth Planet Sci Lett 128:231-241, 1994) and interpret this variation to reflect contributions from pyroxenite-peridotite mantle sources. Furthermore, Gurenko et al. (Contrib Mineral Petrol 162:349-363, 2011) speculate that δ18Ool values for La Palma olivine grains measured by LF (Day et al. Geology 37:555-558, 2009, Geochim Cosmochim Acta 74:6565-6589, 2010) may be biased to low values due to the presence of altered silicate, possibly serpentine. The range in δ18Ool values for Canary Island lavas are of importance for constraining their origin. Gurenko et al. (Contrib Mineral Petrol 162:349-363, 2011) took a subset (39 SIMS analyses from 13 grains from a single El Hierro lava; EH4) of a more extensive dataset (321 SIMS analyses from 110 grains from 16 Canary Island lavas) to suggest that δ18Ool is weakly correlated ( R 2 = 0.291) with the parameter used by Gurenko et al. (Earth Planet Sci Lett 277:514-524, 2009) to describe the estimated weight fraction of pyroxenite-derived melt ( Xpx). With this relationship, end-member δ18O values for HIMU-peridotite (δ18O = 5.3 ± 0.3 ‰) and depleted pyroxenite (δ18O = 5.9 ± 0.3 ‰) were defined. Although the model proposed by Gurenko et al. (Contrib Mineral Petrol 162:349-363, 2011) implicates similar pyroxenite-peridotite mantle sources to those proposed by Day et al. (Geology 37:555-558, 2009, Geochim Cosmochim Acta 74:6565-6589, 2010) and Day and Hilton (Earth Planet Sci Lett 305:226-234, 2011), there are significant differences in the predicted δ18O values of end member components in the two models. In particular, Day et al. (Geochim Cosmochim Acta 74:6565-6589, 2010) proposed a mantle source for La Palma lavas with low-δ18O (<5 ‰), rather than higher-δ18O (c.f. the HIMU-peridotite composition of Gurenko et al. in Contrib Mineral Petrol 162:349-363, 2011). Here we question the approach of using weakly correlated variations in δ18Ool and the Xpx parameter to define mantle source oxygen isotope compositions, and provide examples of why this approach appears flawed. We also provide reasons why the LF datasets previously published for Canary Island lavas remain robust and discuss why LF and SIMS data may provide complementary information on oxygen isotope variations in ocean island basalts (OIB), despite unresolved small-scale uncertainties associated with both techniques.

Introduction to EGU session "Lunar Science and Exploration Towards Moon Village"

NASA Astrophysics Data System (ADS)

Foing, Bernard

2017-04-01

The EGU PS2.2 session "Lunar Science and Exploration" Towards Moon Village" will address: - Recent lunar results: geochemistry, geophysics in the context of open planetary science and exploration - Synthesis of results from SMART-1, Kaguya, Chang'e 1, 2 and 3, Chandrayaan-1, LCROSS, LADEE, Lunar Reconnaissance Orbiter and, Artemis and GRAIL - Goals and Status of missions under preparation: orbiters, Luna-Glob, Google Lunar X Prize, Luna Resurs polar lander, SLIM, Chandrayaan2, Chang'E 4 & 5, Lunar Resource Prospector, Future landers, Lunar sample return missions - Precursor missions, instruments and investigations for landers, rovers, sample return, and human cis-lunar activities and human lunar surface sorties - Preparation for International Lunar Decade: databases, instruments, missions, terrestrial field campaigns, support studies - ILEWG and Global Exploration roadmaps towards a global robotic/human Moon village - Strategic Knowledge Gaps, and key science Goals relevant to Lunar Global Exploration Lunar science and exploration are developing further with new and exciting missions being developed by China, the US, Japan, India, Russia, Korea and Europe, and with new stakeholders. The Moon Village is an open concept proposed by ESA DG with the goal of a sustainable human and robotic presence on the lunar surface as an ensemble where multiple users can carry out multiple activities. Multiple goals of the Moon Village include planetary science, life sciences, astronomy, fundamental research, resources utilisation, human spaceflight, peaceful cooperation, economical development, inspiration, training and capacity building. ESA director general has revitalized and enhanced the original concept of MoonVillage discussed in the last decade. Space exploration builds on international collaboration. COSPAR and its ILEWG International Lunar Exploration Working Group (created in 1994) have fostered collaboration between lunar missions [4-8]. A flotilla of lunar orbiters has flown in the last international lunar decade (SMART-1, Kaguya, Chang'Eal1 &2, Chandrayaan-1, LCROSS, LRO, GRAIL, LADEE). Chinese Chang'E 3 lander and Yutu rover, and upcoming 2017 other landers from 2017 (GLXP, Chang'E 4 & 5, SLIM, Luna , LRP) will constitute a Robotic Village on the Moon. A number of MoonVillage talks and/or interactive jam sessions have been conducted at International workshops and symposia 2016. Moon Village Workshops were held at ESA centres: they were held with senior experts as well as Young ESA professionals to discuss general topics and specific issues ( habitat design, technology, science and precursor missions; public and stakeholder engagement) . Many workshops were complemented with ILEWG EuroMoonMars simulation campaigns. Moon Village Workshops or Jam sessions were also conducted at international symposia or in collaboration with specific universities or institutes. The PS2.2 session will include invited and contributed talks as well as a panel discussion and interactive posters with short oral introduction. Acknowledgements We thank Prof J. Woerner (ESA DG) for energizing the concept of MoonVillage. We thank co-conveners of MoonVillage Workshops and ILEWG EuroMoonMars field campaigns in 2016 (including C. Jonglez, V.Guinet, M.Monnerie, A. Kleinschneider, A. Kapoglou, A. Kolodziejczyk, M. Harasymczuk, I. Schlacht, C. Heinicke, D. Esser, M.Grulich, T. Siruguet, H.Vos, M.Mirino, D.Sokolsky, J.Blamont) and participants to these events. We thank A.Cowley, C. Haigneré, P. Messina, G. Ortega, S.Cristoforetti, ESA colleagues involved in MoonVillage related activities. We thank colleagues from ILEWG, Young Lunar Explorers, the International Lunar Decade Group, the Moon Village Association and Moon Village Support Groups and "MoonVillagers" at large. [1] Jan Wörner, Driving #MoonVillage http://www.iafastro.org/events/iac/iac-2015/plenaryprogramme/the-moon-a-continent-and-a-gateway-for-ourfuture/ (IAC 2015, Jerusalem); [2]http://www.iafastro.org/events/iac/iac2016/globalnetworking-forum/making-the-moon-village-and-marsjourney-accessible-and-affordable-for-all/ (IAC 2016) ; [3] B. Foing et al , Highlights from Moon Village Workshop, held at ESTEC in December 2015, http://www.hou.usra.edu/meetings/lpsc2016/pdf/2719.pdf, http://www.hou.usra.edu/meetings/lpsc2016/pdf/2798.pdf [4] P. Ehrenfreund et al. "Toward a Global Space Exploration Program: A Stepping Stone Approach" (Advances in Space Research, 49, n°1, January 2012), prepared by COSPAR Panel on Exploration (PEX) [5] http://www.lpi.usra.edu/leag/GER_2011.pdf; [6] http://sci.esa.int/ilewg/47170-gluc-iceum11- beijing-2010lunar-declaration/; [7] http://www.lpi.usra.edu/meetings/leagilewg2008/ [8] http://sci.esa.int/ilewg/41506-iceum9-sorrento- 2007-lunar-declaration/ [9] National Research Council (2007), The Scientific Context for Exploration of the Moon [10] P. Ehrenfreund , B.H. Foing, A. Cellino Editors, The Moon and Near Earth Objects), Advances in Space Research, Volume 37, Issue 1, pp 1-192, 2006 [11] http://sci.esa.int/ilewg/38863-iceum8-beijing- 2006declaration/ [12] W. Huntress, D. Stetson, R. Farquhar, J. Zimmerman, B. Clark, W. O'Neil, R. Bourke& B. Foing,'The next steps in exploring deep space - A cosmic study by the IAA', Acta Astronautica, Vol 58, Issues 6-7, 2006, p302-377 [13]http://sci.esa.int/ilewg/38178-iceum7-toronto-2005-declaration/ [14] H. Balsiger et al. Eds, International Lunar Workshop, 1994 May 31-June 3, Beatenberg, Switzerland. Proceedings. Ed. European Space Agency, 1994. ESA-SP-1170 [15] R.M. Bonnet et al, 'Mission to the Moon, Europe's Priorities for Scientific Exploration and Utilisation of the Moon', European Space Agency, ESA SP-1150, June 1992 [16] http://www.iafastro.org/events/iaf-spring-meetings/spring-meetings-2016/ [17] https://www.spacesymposium.org/ [18] http://www.egu2016.eu/ http://meetingorganizer.copernicus.org/EGU2016/session/20378 [19] https://els2016.arc.nasa.gov/ [20] https://nesf2016.arc.nasa.gov/ [21] https://www.cospar-assembly.org/abstractcd/COSPAR-16/ [22] https://www.iac2016.org/, [23] http://www.hou.usra.edu/meetings/leag2016/presentations/ [24] http://newworlds2016.space/ [25] http://www.stx.ox.ac.uk/happ/events/history-moon [26] https://www.cranfield.ac.uk/events/events-2016/manufacturing-2075#

Development of Modeling Methods and Tools for Predicting Coupled Reactive Transport Processes in Porous Media at Multiple Scales

DOE Office of Scientific and Technical Information (OSTI.GOV)

Clement, T. Prabhakar; Barnett, Mark O.; Zheng, Chunmiao

DE-FG02-06ER64213: Development of Modeling Methods and Tools for Predicting Coupled Reactive Transport Processes in Porous Media at Multiple Scales Investigators: T. Prabhakar Clement (PD/PI) and Mark O. Barnett (Auburn), Chunmiao Zheng (Univ. of Alabama), and Norman L. Jones (BYU). The objective of this project was to develop scalable modeling approaches for predicting the reactive transport of metal contaminants. We studied two contaminants, a radioactive cation [U(VI)] and a metal(loid) oxyanion system [As(III/V)], and investigated their interactions with two types of subsurface materials, iron and manganese oxyhydroxides. We also developed modeling methods for describing the experimental results. Overall, the project supportedmore » 25 researchers at three universities. Produced 15 journal articles, 3 book chapters, 6 PhD dissertations and 6 MS theses. Three key journal articles are: 1) Jeppu et al., A scalable surface complexation modeling framework for predicting arsenate adsorption on goethite-coated sands, Environ. Eng. Sci., 27(2): 147-158, 2010. 2) Loganathan et al., Scaling of adsorption reactions: U(VI) experiments and modeling, Applied Geochemistry, 24 (11), 2051-2060, 2009. 3) Phillippi, et al., Theoretical solid/solution ratio effects on adsorption and transport: uranium (VI) and carbonate, Soil Sci. Soci. of America, 71:329-335, 2007« less

Characterization of emergent leakage neutrons from multiple layers of hydrogen/water in the lunar regolith by Monte Carlo simulation

NASA Astrophysics Data System (ADS)

SU, J.; Sagdeev, R.; Usikov, D.; Chin, G.; Boyer, L.; Livengood, T. A.; McClanahan, T. P.; Murray, J.; Starr, R. D.

2013-12-01

Introduction: The leakage flux of lunar neutrons produced by precipitation of galactic cosmic ray (GCR) particles in the upper layer of the lunar regolith and measured by orbital instruments such as the Lunar Exploration Neutron Detector (LEND) is investigated by Monte Carlo simulation. Previous Monte Carlo (MC) simulations have been used to investigate neutron production and leakage from the lunar surface to assess the elemental composition of lunar soil [1-6] and its effect on the leakage neutron flux. We investigate effects on the emergent flux that depend on the physical distribution of hydrogen within the regolith. We use the software package GEANT4 [7] to calculate neutron production from spallation by GCR particles [8,9] in the lunar soil. Multiple layers of differing hydrogen/water at different depths in the lunar regolith model are introduced to examine enhancement or suppression of leakage neutron flux. We find that the majority of leakage thermal and epithermal neutrons are produced in 25 cm to 75 cm deep from the lunar surface. Neutrons produced in the shallow top layer retain more of their original energy due to fewer scattering interactions and escape from the lunar surface mostly as fast neutrons. This provides a diagnostic tool in interpreting leakage neutron flux enhancement or suppression due to hydrogen concentration distribution in lunar regolith. We also find that the emitting angular distribution of thermal and epithermal leakage neutrons can be described by cos3/2(theta) where the fast neutrons emitting angular distribution is cos(theta). The energy sensitivity and angular response of the LEND detectors SETN and CSETN are investigated using the leakage neutron spectrum from GEANT4 simulations. A simplified LRO model is used to benchmark MCNPX[10] and GEANT4 on CSETN absolute count rate corresponding to neutron flux from bombardment of 120MV solar potential GCR particles on FAN lunar soil. We are able to interpret the count rates of SETN and CSETN from the leakage neutron spectrum, emission angle, detector energy sensitivity and angular response. Reference: [1] W. C. Feldman, et al., Science 4 September 1998: Vol. 281 no. 5382 pp. 1496-1500. [2] Gasnault, O., et al., (2000) J. Geophys. Res., 105(E2), 4263-4271. [3] Little, R. C., et al. (2003), J. Geophys. Res., 108(E5), 5046. [4] McKinney et al., (2006), J. Geophys. Res., 111, E06004. [5] Lawrence et al., (2006), J. Geophys. Res., 111, E08001. [6] Looper et al, (2013), Space Weather, VOL. 11, 142-152. [7] J. Allison, et al, (2006) IEEE TRANS. ON NUCL SCI, VOL. 53, NO. 1. [8] J. Masarik and R. Reedy (1996), J. Geophys. Res., 101, 18,891-18,912. [9] P. O'Neil (2010) IEEE Trans. Nucl. Sci., 57(6), 3148-3153. [10] D. Pelowitz, (2005), Rep. LA-CP-05-0369, LANL, Los Alamos, NM.

A hierarchically distributed architecture for fault isolation expert systems on the space station

NASA Technical Reports Server (NTRS)

Miksell, Steve; Coffer, Sue

1987-01-01

The Space Station Axiomatic Fault Isolating Expert Systems (SAFTIES) system deals with the hierarchical distribution of control and knowledge among independent expert systems doing fault isolation and scheduling of Space Station subsystems. On its lower level, fault isolation is performed on individual subsystems. These fault isolation expert systems contain knowledge about the performance requirements of their particular subsystem and corrective procedures which may be involved in repsonse to certain performance errors. They can control the functions of equipment in their system and coordinate system task schedules. On a higher level, the Executive contains knowledge of all resources, task schedules for all systems, and the relative priority of all resources and tasks. The executive can override any subsystem task schedule in order to resolve use conflicts or resolve errors that require resources from multiple subsystems. Interprocessor communication is implemented using the SAFTIES Communications Interface (SCI). The SCI is an application layer protocol which supports the SAFTIES distributed multi-level architecture.

Melting depths associated with Jack Hills zircons crystallization as revealed by in situ trace element measurements

NASA Astrophysics Data System (ADS)

Profeta, L.; Ducea, M. N.; Gehrels, G. E.

2016-12-01

The Jack Hills zircons hosted within the Narryer Gneiss Complex, Yilgarn craton have ages from 4.4 Ga up to Mesoarchean. These zircons crystallized from low temperature granitoid magmas (Harrison, 2009). Here, we use trace element measurements obtained simultaneously with U-Pb ages using LA-ICP-MS on 276 Jack Hills zircons in order to estimate the depth of melting. La/Yb are converted to whole rock equivalent values using newly determined REE -whole rock partition coefficients (Chapman et al., 2016). La/Yb are subsequently transformed into depth estimates using the correlation between whole rock La/Yb and crustal thickness put forward in Profeta et al. (2015) for modern arcs. Our data pertains to 4.2 to 3.2 Ga zircons, which are supplemented with previously published data on 4.4.-4.3 Ga zircons (Peck et al. 2001). Depth estimates are averaged over 100 Ma bins, revealing a remarkably constant trend throughout the investigated period with values around 50 ± 10 km. We interpret that these depths may not be the result of a thick continental crust, as is the case for modern arcs, but rather the existence of different melting conditions during the Hadean and Paleoarchean due to elevated thermal regimes within the mantle. The high La/Yb whole rock ratios (with computed values greater than 10) coupled with elevated mantle temperatures point towards granitoid generation from partial melting of hydrated basalts (e.g. Martin et al., 2014). [1] Harrison, T.M., Annu. Rev. Earth Planet. Sci. 37, 479-505 (2009). [2] Chapman, J. B. et al., Chem. Geol. 439, 59-70 (2016). doi: 10.1016/j.chemgeo.2016.06.014. [3] Profeta, L. et al., Sci. Rep. 5, 17786 (2015). doi: 10.1038/srep17786 [4] Peck, W. et al., Cosmochim. Acta 65, 4215-4229 (2001). doi: 10.1016/S0016-7037(01)00711-6 [5] Martin, H. et al. Lithos 198, 1-13 (2014). doi: 10.1016/j.lithos.2014.02.017

Water Vapor in Titan’s Stratosphere from Cassini CIRS Far-infrared Spectra

NASA Astrophysics Data System (ADS)

Cottini, Valeria; Nixon, C. A.; Jennings, D. E.; Anderson, C. M.; Gorius, N.; Bjoraker, G. L.; Coustenis, A.; Teanby, N. A.; Achterberg, R. K.; Bézard, B.; de Kok, R.; Lellouch, E.; Irwin, P. G. J.; Flasar, F. M.; Bampasidis, G.

2012-10-01

We will report the measurement of water vapor in Titan’s stratosphere (Cottini et al. 2012), using the Cassini Composite Infrared Spectrometer (CIRS, Flasar et al. 2004). CIRS senses water emissions in the far infrared spectral region near 50 microns, which we have modeled using a radiative transfer code (NEMESIS, Irwin et al. 2008). From the analysis of nadir spectra we have derived a mixing ratio of 0.14 ± 0.05 ppb at an altitude of 97 km, which corresponds to an integrated (from 0 to 600 km) surface normalized column abundance of 3.7±1.3 × 1014 molecules/cm2. In the latitude range 80°S to 30°N we see no evidence for latitudinal variations in these abundances within the error bars. Using limb observations, we obtained mixing ratios of 0.13 ± 0.04 ppb at an altitude of 115 km and 0.45 ± 0.15 ppb at an altitude of 230 km, confirming that the water abundance has a positive vertical gradient as predicted by previous photochemical models. We have also fitted our data using scaling factors of 0.1-0.6 to these photochemical model profiles, indicating that the models over-predict the water abundance in Titan’s lower stratosphere. Valeria Cottini is supported by the NASA Postdoctoral Program. References Cottini V. et al., 2012. Detection of water vapor in Titan’s atmosphere from Cassini/CIRS infrared spectra. Icarus, 220, 2, 855-862 Flasar, F.M., and 44 colleagues, 2004. Exploring the Saturn system in the thermal infrared: The Composite Infrared Spectrometer. Space Sci. Rev., 115, 169-297 Irwin, P.G.J., et al., 2008. The NEMESIS planetary atmosphere radiative transfer and retrieval tool. J. Quant. Spectrosc. Radiat. Trans., 109, 1136-1150.

Mars Organic Matter Revealed by the Detection of Organo-chlorinated Molecules from Pyro-GCMS Analyses of Yellowknife Bay Mudstone

NASA Astrophysics Data System (ADS)

Szopa, C.; Freissinet, C.; Glavin, D. P.; Buch, A.; Coll, P. J.; Cabane, M.; Millan, M.; Belmahadi, I.; Navarro-Gonzalez, R.; Steele, A.; Summons, R. E.; Eigenbrode, J. L.; Mahaffy, P. R.

2015-12-01

Mudstones collected on the Yellowknife Bay site in Gale crater by the Curiosity rover, were analyzed with the Sample Analysis at Mars (SAM) chemical laboratory with the aim (among others) to detect and identify organic molecules in the Martian reglith [1]. The pyrolysis (to 900°C)-gas chromatography-mass spectrometry (Pyro-GCMS) analytical mode was systematically used to reach that goal. It revealed the existence of complex interactions between compounds present in the soil sample (e.g. oxychlorines [2]) and internal components of the SAM experiment (e.g. derivatization reactant) resulting in signals complex to interpret [3]. By comparing these results with those obtained for the other Mars samples analysed with SAM, and by carefully identifying, from laboratory work, the possible SAM internal contributions to the organic molecules detected [4], chlorobenzene has already been identified as mainly originating from organics present in the mudstone [5]. Since this discovery, we did additional studies of the chromatograms that reveal the presence of dichlorobenzene originating from an organic source endogenous to the sample. Even if the exact original source of these organic molecules cannot be strictly identified, the detection of several chlorinated aromatic molecules suggests the presence of a significant amount of aromatized materials which are in an oxidized state involving oxygen in the mudstone. We present here the corresponding results and the implication it can have on the origin of these organic materials References: [1] Mahaffy, P. et al. (2012) Space Sci Rev, 170, 401-478. [2] Glavin, D. et al. (2013), JGR. [3] Ming D. et al. (2013), Science 32, 64, [4] Miller K. et al. (In press), JGR, [5] Freissinet et al., (2015), JGR Pla. 120, 495.

Solid-state experiments at high pressure and strain rates

NASA Astrophysics Data System (ADS)

Kalantar, D. H.

1999-11-01

We are developing experiments on intense laser facilities to study shock compressed metal foils in the solid state. At high pressure, Rayleigh-Taylor induced perturbation growth can be reduced by the strength of the material. [1] We use this to characterize the strength of the metal foils accelerated at high pressure in the solid state. In our experiments, Al and Cu foils are compressed and accelerated with staged shocks using a temporally shaped x-ray drive that is generated in a Nova laser hohlraum target. [2] The peak pressures exceed 1 Mbar (100 GPa), and strain rates are very high, 10^7-10^9 s-1. The instability growth is observed by x-ray radiography. To probe the state of the material under compression and to demonstrate that it remains solid, we are using the dynamic Bragg diffraction technique. [3] This technique has been demonstrated on the Nova laser [4] using Si crystals shocked to 200-500 kbar. Additionally, we have observed diffraction from Cu crystals that are shocked to 100-200 kbar by direct laser irradiation on the Trident and OMEGA lasers. Compressions of up to a 10in the crystal lattice spacing have been observed. We will present the results of our work to develop these high pressure solid-state hydrodynamics experiments. 1. J. F. Barnes et al, J. Appl. Phys. 45, 727 (1974); A. I. Lebedev et al , Proc. 4th IWPCTM, 29 March-1 April, 1993, p. 81. 2. D. H. Kalantar et al., to appear in Int. J. of Impact Eng. (1999). 3. R. R. Whitlock and J. S. Wark, Phys. Rev. B 52, 8 (1995). 4. D. H. Kalantar et al, Rev. Sci. Instrum. 70, 629 (1999).

Does atomic polarizability play a role in hydrogen radio recombination spectra from Galactic H II regions?

NASA Astrophysics Data System (ADS)

Hey, J. D.

2013-09-01

Since highly excited atoms, which contribute to the radio recombination spectra from Galactic H II regions, possess large polarizabilities, their lifetimes are influenced by ion (proton)-induced dipole collisions. It is shown that, while these ion-radiator collisional processes, if acting alone, would effectively limit the upper principal quantum number attainable for given plasma parameters, their influence is small relative to that of electron impacts within the framework of line broadening theory. The present work suggests that ion-permanent dipole interactions (Hey et al 2004 J. Phys. B: At. Mol. Opt. Phys. 37 2543) would also be of minor importance in limiting the occupation of highly excited states. On the other hand, the ion-induced dipole collisions are essential for ensuring equipartition of energy between atomic and electron kinetic distributions (Hey et al 1999 J. Phys. B: At. Mol. Opt. Phys. 32 3555; 2005 J. Phys. B: At. Mol. Opt. Phys. 38 3517), without which Voigt profile analysis to extract impact broadening widths would not be possible. Electron densities deduced from electron impact broadening of individual lines (Griem 1967 Astrophys. J. 148 547; Watson 2006 J. Phys. B: At. Mol. Opt. Phys. 39 1889) may be used to check the significance of the constraints arising from the present analysis. The spectra of Bell et al (2000 Publ. Astron. Soc. Pac. 112 1236; 2011 Astrophys. Space Sci. 333 377; 2011 Astrophys. Space Sci. 335 451) for Orion A and W51 in the vicinity of 6.0 and 17.6 GHz are examined in this context, and also in terms of a possible role of the background ion microfield in reducing the near-elastic contributions to the electron impact broadening below the predictions of theory (Hey 2012 J. Phys. B: At. Mol. Opt. Phys. 45 065701). These spectra are analysed, subject to the constraint that calculated relative intensities of lines, arising from upper states in collisional-radiative equilibrium, should be consistent with those obtained from Voigt profile analysis. It is shown that the experimental technique yields an excellent temperature diagnostic for the H II regions. On the other hand, strong evidence is not obtained, from those spectra which satisfy the above constraint on intensity, to indicate that the electron impact broadening theory requires substantial correction. The main grounds for attempting a revision of theory to allow for the influence of the ion microfield during the scattering processes on the upper and lower states of each line thus still appear to have a stronger theoretical (Hey 2007 J. Phys. B: At. Mol. Opt. Phys. 40 4077) than experimental basis.

Taurine reduces inflammatory responses after spinal cord injury.

PubMed

Nakajima, Yasuhiro; Osuka, Koji; Seki, Yukio; Gupta, Ramesh C; Hara, Masahito; Takayasu, Masakazu; Wakabayashi, Toshihiko

2010-02-01

Taurine has multiple functions in the central nervous system (CNS), serving as an osmoregulator, antioxidant, inhibitory neuromodulator, and regulator of intracellular Ca(2+) flux. Since the role of taurine in traumatic spinal cord injury (SCI) is not fully understood, the present study was conducted with C57 black/6 mice (18-20 g) who underwent severe SCI at the Th-8 level using a weight compression device. Taurine was injected intraperitoneally at doses of 25, 80, 250, and 800 mg/kg within 30 min after SCI. Controls were injected with saline. The contusional cord segments were removed 6 h after SCI, and concentrations of interleukin-6 (IL-6) and myeloperoxidase (MPO) were measured using ELISA kits. Phosphorylation of STAT3, which is activated by IL-6, and expression of inducible cyclooxygenase-2 (COX-2) were also compared between the taurine treatment group (250 mg/kg) and the control group by Western blot analysis. Morphological changes were evaluated with H&E-stained sections. Taurine significantly decreased IL-6 and MPO levels in a dose-dependent manner, significantly reducing the phosphorylation of STAT3 and expression of COX-2 after SCI compared to controls. A reduced accumulation of neutrophils, especially in the subarachnoid spaces, and secondary degenerative changes in gray matter were also noted, and motor disturbances were significantly attenuated with taurine treatment (250 mg/kg). These findings indicate that taurine has anti-inflammatory effects against SCI, and may play a neuroprotective role against secondary damage, and thus it may have therapeutic potential.

An adaptable XML based approach for scientific data management and integration

NASA Astrophysics Data System (ADS)

Wang, Fusheng; Thiel, Florian; Furrer, Daniel; Vergara-Niedermayr, Cristobal; Qin, Chen; Hackenberg, Georg; Bourgue, Pierre-Emmanuel; Kaltschmidt, David; Wang, Mo

2008-03-01

Increased complexity of scientific research poses new challenges to scientific data management. Meanwhile, scientific collaboration is becoming increasing important, which relies on integrating and sharing data from distributed institutions. We develop SciPort, a Web-based platform on supporting scientific data management and integration based on a central server based distributed architecture, where researchers can easily collect, publish, and share their complex scientific data across multi-institutions. SciPort provides an XML based general approach to model complex scientific data by representing them as XML documents. The documents capture not only hierarchical structured data, but also images and raw data through references. In addition, SciPort provides an XML based hierarchical organization of the overall data space to make it convenient for quick browsing. To provide generalization, schemas and hierarchies are customizable with XML-based definitions, thus it is possible to quickly adapt the system to different applications. While each institution can manage documents on a Local SciPort Server independently, selected documents can be published to a Central Server to form a global view of shared data across all sites. By storing documents in a native XML database, SciPort provides high schema extensibility and supports comprehensive queries through XQuery. By providing a unified and effective means for data modeling, data access and customization with XML, SciPort provides a flexible and powerful platform for sharing scientific data for scientific research communities, and has been successfully used in both biomedical research and clinical trials.

An Adaptable XML Based Approach for Scientific Data Management and Integration.

PubMed

Wang, Fusheng; Thiel, Florian; Furrer, Daniel; Vergara-Niedermayr, Cristobal; Qin, Chen; Hackenberg, Georg; Bourgue, Pierre-Emmanuel; Kaltschmidt, David; Wang, Mo

2008-02-20

Increased complexity of scientific research poses new challenges to scientific data management. Meanwhile, scientific collaboration is becoming increasing important, which relies on integrating and sharing data from distributed institutions. We develop SciPort, a Web-based platform on supporting scientific data management and integration based on a central server based distributed architecture, where researchers can easily collect, publish, and share their complex scientific data across multi-institutions. SciPort provides an XML based general approach to model complex scientific data by representing them as XML documents. The documents capture not only hierarchical structured data, but also images and raw data through references. In addition, SciPort provides an XML based hierarchical organization of the overall data space to make it convenient for quick browsing. To provide generalization, schemas and hierarchies are customizable with XML-based definitions, thus it is possible to quickly adapt the system to different applications. While each institution can manage documents on a Local SciPort Server independently, selected documents can be published to a Central Server to form a global view of shared data across all sites. By storing documents in a native XML database, SciPort provides high schema extensibility and supports comprehensive queries through XQuery. By providing a unified and effective means for data modeling, data access and customization with XML, SciPort provides a flexible and powerful platform for sharing scientific data for scientific research communities, and has been successfully used in both biomedical research and clinical trials.

Orbit-Attitude Changes of Objects in Near Earth Space Induced by Natural Charging

DTIC Science & Technology

2017-05-02

depends upon Earth’s magnetosphere. Typically, magneto-sphere models can be grouped under two classes: statistical and physics -based. The Physics ...models were primarily physics -based due to unavailability of sufficient space-data, but over the last three decades, with the availability of huge...Attitude Determination and Control,” Astrophysics and Space Sci- ence Library, Vol. 73, D. Reidel Publishing Company, London, 1978 [17] Fairfield

Searching for the light-element candidate of the Earth's inner core

NASA Astrophysics Data System (ADS)

Li, Y.; Vocadlo, L.; Brodholt, J. P.; Wood, I. G.

2016-12-01

The mismatch between the seismic observations of the Earth's inner core and observations from mineral physics (Vočadlo, 2007; Vočadlo et al., 2009; Belonoshko et al., 2007; Martorell et al., 2013) questions the basic structure of the core and also makes it more difficult to understand its other complex characteristics. The premelting elastic softening predicted in hcp Fe under inner core conditions gives a match with seismic wave velocities, but clearly the density is too high (Martorell et al., 2013); in addition, the origin of such premelting softening is not clear. Using ab-initio based simulation techniques, we have studied the structures and elastic properties of Fe alloys and compounds with C and Si that are strongly relevant to the inner core. The densities and elastic constants were obtained up to melting under inner core pressures. The premelting elastic softening observed in hcp Fe was also observed in materials like Fe7C3, and was found to be correlated with the partial weakening of the bonding network, but the density of Fe7C3 is too low to match that of the inner core. However, the density and elastic properties from calculations on the Fe-Si-C ternary alloy were found to be very close to the seismic observations of the core, suggesting that it may, finally, be possible to report a core composition which is fully matched with seismology. Belonoshko, A. B., Skorodumova, N. V., Davis, S., Osiptsov, A. N., Rosengren, A., Johansson, B., (2007). Science 316 (5831), 1603-1605. Vočadlo, L., (2007). Earth. Planet. Sci. Lett., 254 (1), 227-232. Vočadlo, L., Brodholt, J., Dobson, D.P., Knight, K., Marshall, W., Price, G.D., Wood, I.G. (2002). Earth. Planet. Sci. Lett., 203 (1) 567-575. Vočadlo, L., Dobson, D. P., Wood, I. G., (2009). Earth. Planet. Sci. Lett., 288 (3), 534-538. Martorell, B., Vočadlo, L., Brodholt, J., Wood, I. G., (2013b). Science 342 (6157), 466-468.

Permeability Changes in Reaction Induced Fracturing

NASA Astrophysics Data System (ADS)

Ulven, Ole Ivar; Malthe-Sørenssen, Anders; Kalia, Rajiv

2013-04-01

The process of fracture formation due to a volume increasing chemical reaction has been studied in a variety of different settings, e.g. weathering of dolerites by Røyne et al.[4], serpentinization and carbonation of peridotite by Rudge et al.[3] and replacement reactions in silica-poor igneous rocks by Jamtveit et al.[1]. It is generally assumed that fracture formation will increase the net permeability of the rock, and thus increase the reactant transport rate and subsequently the total reaction rate, as summarised by Kelemen et al.[2]. Røyne et al.[4] have shown that transport in fractures will have an effect on the fracture pattern formed. Understanding the feedback process between fracture formation and permeability changes is essential in assessing industrial scale CO2 sequestration in ultramafic rock, but little is seemingly known about how large the permeability change will be in reaction-induced fracturing under compression, and it remains an open question how sensitive a fracture pattern is to permeability changes. In this work, we study the permeability of fractures formed under compression, and we use a 2D discrete element model to study the fracture patterns and total reaction rates achieved with different permeabilities. We achieve an improved understanding of the feedback processes in reaction-driven fracturing, thus improving our ability to decide whether industrial scale CO2 sequestration in ultramafic rock is a viable option for long-term handling of CO2. References [1] Jamtveit, B, Putnis, C. V., and Malthe-Sørenssen, A., "Reaction induced fracturing during replacement processes," Contrib. Mineral Petrol. 157, 2009, pp. 127 - 133. [2] Kelemen, P., Matter, J., Streit, E. E., Rudge, J. F., Curry, W. B., and Blusztajn, J., "Rates and Mechanisms of Mineral Carbonation in Peridotite: Natural Processes and Recipes for Enhanced, in situ CO2 Capture and Storage," Annu. Rev. Earth Planet. Sci. 2011. 39:545-76. [3] Rudge, J. F., Kelemen, P. B., and Spiegelman, M., "A simple model of reaction induced cracking applied to serpentinization and carbonation of peridotite," Earth Planet. Sci. Lett. 291, Issues 1-4, 2010, pp. 215 - 227. [4] Røyne, A., Jamtveit, B., and Malthe-Sørenssen, A., "Controls on rock weathering rates by reaction-induced hierarchial fracturing," Earth Planet. Sci. Lett. 275, 2008, pp. 364 - 369.

Metasomatism-induced magnesium isotope fractionation in ultramafic rocks: Evidence from the Franciscan Complex, California

NASA Astrophysics Data System (ADS)

Li, W. Y.; Teng, F. Z.; Xiao, Y.

2016-12-01

To investigate the behaviour of Mg isotopes during metasomatic reactions between peridotites and infiltrating fluids along the slab-mantle interface, we analyzed Mg isotopic compositions of a set of well-characterized samples from the ultramafic blocks in the Franciscan Complex of California [1]. The Group 1 and Group 2 samples that were defined by the initial serpentinization and complete serpentinization of peridotites at temperatures of 450-500 ºC, respectively [1], have δ26Mg values (from -0.26 to -0.14‰) clustered around the mantle value. This suggests that Mg isotope fractionation during serpentinization by slab-derived fluids, if any, is small. By contrast, the Group 3 samples that were defined by the replacement of serpentine by talc [1], are enriched in heavy Mg isotopes (δ26Mg of -0.13 to -0.01‰). This may reflect the loss of light Mg isotopes into fluids during the dehydration reaction that produced talc from serpentine, which is consistent with previous observations that secondary clay minerals preferentially incorporate heavy Mg isotopes during water-rock interactions [2, 3]. The Group 4 samples that were defined by the further replacement of talc by tremolite [1], however, have light Mg isotopic compositions (δ26Mg of -0.50 to -0.41‰). Such a shift towards light Mg isotopic compositions likely results from metasomatism by fluids that derived from isotopically light carbonates, which is supported by the remarkably higher CaO content of Group 4 samples (from 6.9 to 9.2 wt%) than Group 3 ones (from 1.1 to 1.4 wt%). Collectively, significant Mg isotopic variations occur during metasomatism of peridotites in the mantle wedge, which would potentially lead to heterogeneous Mg isotopic compositions in arc lavas [4]. Therefore, Mg isotopes can be used as a powerful tracer of crust-mantle interaction at subduction zones. [1] King et al. (2003) Geol. Soc. Am. Bull. 115, 1097-1109. [2] Teng et al. (2010) Earth Planet. Sci. Lett. 300, 63-71. [3] Wimpenny et al. (2014) Geochim. Cosmochim. Acta 128, 178-194. [4] Teng et al. (2016) Proc. Natl. Acad. Sci. 113, 7082-7087. et al. (2016) Proc. Natl. Acad. Sci. 113, 7082-7087.

Imaging quantum transport using scanning gate microscopy

NASA Astrophysics Data System (ADS)

Hackens, Benoit

2014-03-01

Quantum transport in nanodevices is usually probed thanks to measurements of the electrical resistance or conductance, which lack the spatial resolution necessary to probe electron behaviour inside the devices. In this talk, we will show that scanning gate microscopy (SGM) yields real-space images of quantum transport phenomena inside archetypal mesoscopic devices such as quantum point contacts and quantum rings. We will first discuss the SGM technique, which is based on mapping the electrical conductance of a device as an electrically-biased sharp metallic tip scans in its vicinity. With SGM, we demonstrated low temperature imaging of the electron probability density and interferences in embedded mesoscopic quantum rings [B. Hackens et al., Nat. Phys. 2, 826 (2006)]. At high magnetic field, thanks to the SGM conductance maps, one can decrypt complex transport phenomena such as tunneling between quantum Hall edge state, either direct or through localized states [B. Hackens et al., Nat. Comm. 1, 39 (2010)]. Moreover, the technique also allows to perform local spectroscopy of electron transport through selected localized states [F. Martins et al., New J. of Phys. 15, 013049 (2013); F. Martins et al., Sci. Rep. 3, 1416 (2013)]. Overall, these examples show that scanning gate microscopy is a powerful tool for imaging charge carrier behavior inside devices fabricated from a variety of materials, and opens the way towards a more intimate manipulation of charge and quasiparticle transport. This work was performed in collaboration with F. Martins, S. Faniel, B. Brun, M. Pala, X. Wallart, L. Desplanque, B. Rosenow, T. Ouisse, H. Sellier, S. Huant and V. Bayot.

Spatial Transport of Magnetic Flux Surfaces in Strongly Anisotropic Turbulence

NASA Astrophysics Data System (ADS)

Matthaeus, W. H.; Servidio, S.; Wan, M.; Ruffolo, D. J.; Rappazzo, A. F.; Oughton, S.

2013-12-01

Magnetic flux surfaces afford familiar descriptions of spatial structure, dynamics, and connectivity of magnetic fields, with particular relevance in contexts such as solar coronal flux tubes, magnetic field connectivity in the interplanetary and interstellar medium, as well as in laboratory plasmas and dynamo problems [1-4]. Typical models assume that field-lines are orderly, and flux tubes remain identifiable over macroscopic distances; however, a previous study has shown that flux tubes shred in the presence of fluctuations, typically losing identity after several correlation scales [5]. Here, the structure of magnetic flux surfaces is numerically investigated in a reduced magnetohydrodynamic (RMHD) model of homogeneous turbulence. Short and long-wavelength behavior is studied statistically by propagating magnetic surfaces along the mean field. At small scales magnetic surfaces become complex, experiencing an exponential thinning. At large scales, instead, the magnetic flux undergoes a diffusive behavior. The link between the diffusion of the coarse-grained flux and field-line random walk is established by means of a multiple scale analysis. Both large and small scales limits are controlled by the Kubo number. These results have consequences for understanding and interpreting processes such as magnetic reconnection and field-line diffusion in plasmas [6]. [1] E. N. Parker, Cosmical Magnetic Fields (Oxford Univ. Press, New York, 1979). [2] J. R. Jokipii and E. N. Parker, Phys. Rev. Lett. 21, 44 (1968). [3] R. Bruno et al., Planet. Space Sci. 49, 1201 (2001). [4] M. N. Rosenbluth et al., Nuclear Fusion 6, 297 (1966). [5] W. H. Matthaeus et al., Phys. Rev. Lett. 75, 2136 (1995). [6] S. Servidio et al., submitted (2013).

1H, 15N, and 13C resonance assignments of the third domain from the S. aureus innate immune evasion protein Eap.

PubMed

Herrera, Alvaro I; Ploscariu, Nicoleta T; Geisbrecht, Brian V; Prakash, Om

2018-04-01

Staphylococcus aureus is a widespread and persistent pathogen of humans and livestock. The bacterium expresses a wide variety of virulence proteins, many of which serve to disrupt the host's innate immune system from recognizing and clearing bacteria with optimal efficiency. The extracellular adherence protein (Eap) is a multidomain protein that participates in various protein-protein interactions that inhibit the innate immune response, including both the complement system (Woehl et al in J Immunol 193:6161-6171, 2014) and Neutrophil Serine Proteases (NSPs) (Stapels et al in Proc Natl Acad Sci USA 111:13187-13192, 2014). The third domain of Eap, Eap3, is an ~ 11 kDa protein that was recently shown to bind complement component C4b (Woehl et al in Protein Sci 26:1595-1608, 2017) and therefore play an essential role in inhibiting the classical and lectin pathways of complement (Woehl et al in J Immunol 193:6161-6171, 2014). Since structural characterization of Eap3 is still incomplete, we acquired a series of 2D and 3D NMR spectra of Eap3 in solution. Here we report the backbone and side-chain 1 H, 15 N, and 13 C resonance assignments of Eap3 and its predicted secondary structure via the TALOS-N server. The assignment data have been deposited in the BMRB data bank under accession number 27087.

An effect of couterion in STM imaging process of DNA on Cu(111)

NASA Astrophysics Data System (ADS)

Furukawa, Masashi; Nishimura, Makoto; Tanaka, Hiroyuki; Kawai, Tomoji

2002-03-01

In order to elucidate electrical conduction mechanism of DNA, which is still under debate over the last decade, we have performed local electronic structure measurement of single- and double-stranded DNA molecules adsorbed onto Cu(111) surfaces using scanning tunneling microscope (STM). Bias-voltage-dependent STM images (from -5 V to +5 V) have shown that the molecular corrugation height in STM increases gradually at positive bias voltage region (empty state). Despite the theoretical assumption in which their 1st-LUMO states are localized at π plane of DNA bases, one cannot conclude its origin as the existence of their LUMO states, based on the results of relevant control measurements, DNA base molecules/Cu(111) [1] and NaCl/Cu(111). In fact, we found almost identical bias dependencies in the latter case (NaCl/Cu(111)), indicating that the feature of π* states of DNA bases should be buried in an additional channel that opens up by the onset of its unoccupied overlayer state in the tunneling process [2]. This study implies a potential difficulty in direct comparison of the obtained data with those characterized by XAS, in which π* states is located at ca. -1 eV relative to the Fermi level [3]. [1]M. Furukawa et al., submitted to Surf. Sci. [2] J. Kliewer et al., Surf. Sci. 477 (2001) 250.; A. Carlsson et al., Phys. Rev. B. 56 (1997) 1593. [3] M. Furukawa et al., submitted to Phys. Rev. B.

Metal-silicate partitioning of Co, Ni, V, Cr, Si, and O up to 100 GPa and 5500 K: Implications for core formation

NASA Astrophysics Data System (ADS)

Fischer, R. A.; Campbell, A. J.; Frost, D. J.; Harries, D.; Langenhorst, F.; Miyajima, N.; Pollok, K.; Rubie, D. C.

2013-12-01

During core formation, metal and silicate of accreted bodies equilibrated with the proto-Earth in a series of partitioning reactions, characterized by average (or time-intregrated) partition coefficients that can be calculated assuming a bulk Earth that is chondritic in nonvolatile elements [e.g. 1]. Comparisons to experimentally-measured partition coefficients allow constraints on the time-integrated conditions of core-mantle equilibration [e.g. 2-7], providing valuable input into more complex chemical models of Earth's evolution [8]. Partitioning has been studied extensively in the multi-anvil press [e.g. 3, 7], but very few studies extend to pressures above ~25 GPa [e.g. 2, 5-6]. In this study, we measure the metal-silicate partitioning of Co, Ni, V, Cr, Si, and O at higher pressures and temperatures. Thin foils of Fe-rich alloy doped with trace elements were loaded in a diamond anvil cell between layers of (Mg,Fe)2SiO4. Samples were laser-heated to melt the metal and silicate. After decompression, samples were cut parallel to the compression axis into sections ~100 nm thick with a focused ion beam (FIB). Chemical analyses of all elements except oxygen in the coexisting metal, silicate, and oxide were performed using energy dispersive X-ray spectroscopy (EDXS) in a transmission electron microscope (TEM). Later, samples were further thinned by FIB to ~60 nm and analyzed by electron energy loss spectroscopy (EELS) in a TEM to determine the Fe/O ratio of the metal. Analysis was performed on a suite of six experiments from pressures of 25, 31, 43, 57, 58, and 100 GPa and temperatures above the silicate liquidus, up to 5500 K. Our results are generally consistent with the recent findings of [5-6], although our log(KD) values for cobalt are ~0.1-0.2 log units lower. Some of our experiments contain carbon in the metal which may affect the partitioning of some elements. The metal in the experiment from 100 GPa and 5500 K contains 9 wt% silicon and an estimated 11 wt% oxygen, which is a significantly higher percentage of light elements than the Earth's outer core is thought to contain [e.g. 1]. Using our results, we develop a model for metal/silicate exchange during core formation, the light element composition of the core, and possible chemical reactions at the core-mantle boundary. [1] McDonough, W.F. (2003) Treatise on Geochemistry, Vol. 2, pp 547-568. [2] Bouhifd, M.A. and A.P. Jephcoat (2011) Earth Planet. Sci. Lett. 307, 341-348. [3] Mann, U., D.J. Frost, and D.C. Rubie (2009) Geochim. Cosmochim. Acta 73, 7360-7386. [4] Righter, K. et al. (2010) Earth Planet. Sci. Lett. 291, 1-9. [5] Siebert, J. et al. (2012) Earth Planet. Sci. Lett. 321-322, 189-197. [6] Siebert, J. et al. (2013) Science 339, 1194-1197. [7] Wade, J., and B.J. Wood (2005) Earth Planet. Sci. Lett. 236, 78-95. [8] Rubie, D.C. et al. (2011) Earth Planet. Sci. Lett. 301, 31-42.

Pryce-Hoyle Tensor in a Combined Einstein-Cartan-Brans-Dicke Model

NASA Astrophysics Data System (ADS)

Berman, Marcelo Samuel

2009-03-01

In addition to introducing matter injection through a scalar field determined by Pryce-Hoyle tensor, we also combine it with a BCDE (Brans-Dicke-Einstein-Cartan) theory with lambda-term developed earlier by Berman (Astrophys. Space Sci. 314:79-82, 2008), for inflationary scenario. It involves a variable cosmological constant, which decreases with time, jointly with energy density, cosmic pressure, shear, vorticity, and Hubble’s parameter, while the scale factor, total spin and scalar field increase exponentially. The post-inflationary fluid resembles a perfect one, though total spin grows, but not the angular speed (Berman, in Astrophys. Space Sci. 312:275, 2007). The Pryce-Hoyle tensor, which can measured by the number of injected particles per unit proper volume and time, as well as shear and vorticity, can be neglected in the aftermath of inflation (“no-hair”).

Detection of negative pickup ions at Saturn's moon Dione

NASA Astrophysics Data System (ADS)

Nordheim, T.; Jones, G. H.; Coates, A. J.; Wellbrock, A.; Hand, K. P.; Waite, J. H., Jr.

2015-12-01

Negative ions may be formed in both tenuous and dense planetary atmospheres and have been observed in-situ at Earth, Titan [Coates et al., 2007, 2009; Wellbrock et al., 2013] and Enceladus [Coates et al., 2010] as well as at comet Halley [Chaizy et al., 1991]. In the case of Titan, heavy hydrocarbon and nitrile based ions with masses reaching almost 14,000 amu/q have been observed using the CAPS Electron Spectrometer (ELS) onboard Cassini. These are believed to form even more massive organic aerosols termed tholins which fall to lower altitudes where they make up the distinct haze layers, and eventually rain down onto Titan's surface perhaps forming the organic-rich dunes. Very tenuous atmospheres were predicted at the smaller icy moons of Saturn [Sittler et al., 2004; Saur and Strobel, 2005], and subsequently detected [Teolis et al., 2010; Tokar et al., 2012]. These are produced when charged particles from Saturn's magnetosphere interact with moon surfaces, ejecting neutral species. Some portion of these atmospheric neutrals will in turn become ionized and 'picked up' by Saturn's corotating magnetosphere. These pickup ions will then move in cycloidal trajectories that we may intercept using the Cassini spacecraft, even at considerable distance from the moon itself. In this fashion, negative and positive pickup ions have been used to infer a tenuous CO2-O2 atmosphere at Saturn's moon Rhea [Teolis et al., 2010], and positive pickup ions at Dione [Tokar et al., 2012]. Here we report on the detection of negative pickup ions during a close flyby of Dione by the Cassini CAPS ELS instrument, and the implications that these observations may have for the Dionian atmosphere. Chaizy, P., et al. (1991), Nature, 349(6308), 393-396 Coates, A. J., et al. (2007), Geophys. Res. Lett., 34(22), 6-11 Coates, A. J., et al. (2009), Planet. Space Sci., 57(14-15), 1866-1871 Coates, A. J., et al. (2010), Icarus, 206(2), 618-622 Saur, J., and D. F. Strobel (2005), Astrophys. J. Lett., 620, L115. Sittler, E. C., et al. (2004), J. Geophys. Res., 109(A1) Teolis, B. D., et al. (2010), Science, 330(6012), 1813-5 Tokar, R. L., et al. (2012) Geophys. Res. Lett., 39(3), 1-7 Wellbrock, A., et al.(2013), Geophys. Res. Lett., 40(17), 4481-4485

Public Data Set: A Novel, Cost-Effective, Multi-Point Thomson Scattering System on the Pegasus Toroidal Experiment

DOE Data Explorer

Schlossberg, David J. [University of Wisconsin-Madison] (ORCID:0000000287139448); Bodner, Grant M. [University of Wisconsin-Madison] (ORCID:0000000324979172); Reusch, Joshua A. [University of Wisconsin-Madison] (ORCID:0000000284249422); Bongard, Michael W. [University of Wisconsin-Madison] (ORCID:0000000231609746); Fonck, Raymond J. [University of Wisconsin-Madison] (ORCID:0000000294386762); Rodriguez Sanchez, Cuauhtemoc [University of Wisconsin-Madison] (ORCID:0000000334712586)

2016-09-16

This public data set contains openly-documented, machine readable digital research data corresponding to figures published in D.J. Schlossberg et. al., 'A Novel, Cost-Effective, Multi-Point Thomson Scattering System on the Pegasus Toroidal Experiment,' Rev. Sci. Instrum. 87, 11E403 (2016).

Navigating Tensions between Conceptual and Metaconceptual Goals in the Use of Models

ERIC Educational Resources Information Center

Delgado, Cesar

2015-01-01

Science education involves learning about phenomena at three levels: concrete (facts and generalizations), conceptual (concepts and theories), and metaconceptual (epistemology) (Snir et al. in "J Sci Educ Technol" 2(2):373-388, 1993). Models are key components in science, can help build conceptual understanding, and may also build…

Empirical Approach to Interpreting Card-Sorting Data

ERIC Educational Resources Information Center

Wolf, Steven F.; Dougherty, Daniel P.; Kortemeyer, Gerd

2012-01-01

Since it was first published 30 years ago, the seminal paper of Chi "et al." on expert and novice categorization of introductory problems led to a plethora of follow-up studies within and outside of the area of physics [Cogn. Sci. 5 121 (1981)]. These studies frequently encompass "card-sorting" exercises whereby the…

Molecular Determinants Fundamental to Axon Regeneration after SCI

DTIC Science & Technology

2012-06-01

gray arrow) and a 130kDa N-terminal processed neurocan fragment (black arrow) in chABC treated samples (Asher et. al., 2000). Zebrafish brain tissue...PTPRSREV: GTG TGT GTG CTG ATG AAG GTC GC (EXON 9). 275 bp product expected. We have also designed a forward primer in exon 6 with negative results

Quantification of site-city interaction effects on the response of structure under double resonance condition

NASA Astrophysics Data System (ADS)

Kumar, Neeraj; Narayan, Jay Prakash

2018-01-01

This paper presents the site-city interaction (SCI) effects on the response of closely spaced structures under double resonance condition (F_{02{{D}}}^{{S}} = F_{02{{D}}}^{{B}}), where F_{02{{D}}}^{{S}} and F_{02{{D}}}^{{B}} are fundamental frequencies of 2-D structure and 2-D basin, respectively. This paper also presents the development of empirical relations to predict the F_{02{{D}}}^{{B}} of elliptical and trapezoidal basins for both the polarizations of the S wave. Simulated results revealed that F_{02{{D}}}^{{B}} of a 2-D basin very much depends on its geometry, shape ratio and polarization of the incident S wave. The obtained spectral amplification factor (SAF) at F_{02{{D}}}^{{S}} of a standalone structure in a 2-D basin is greater than that in the 1-D case under double resonance condition. A considerable reduction of the fundamental resonance frequency of structures due to the SCI effects is observed for both the polarizations of the S wave. The SAFs at F_{02{{D}}}^{{S}} of closely spaced structures due to SCI effects is larger in the case of SV than SH waves. A splitting of the fundamental-mode frequency bandwidth along with the drastic decrease of SAF due to the SCI effects is obtained. The findings of this paper raise the question concerning the validity of the predicted response of standalone structure based on soil-structure interaction for the design of structures in a 2-D small basin, in an urban environment.

KENNEDY SPACE CENTER, FLA. - Inside the hangar at Vandenberg Air Force Base, Calif., workers wait for the Pegasus launch vehicle to be moved inside. The Pegasus will carry the SciSat-1 spacecraft in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

NASA Image and Video Library

2003-06-27

KENNEDY SPACE CENTER, FLA. - Inside the hangar at Vandenberg Air Force Base, Calif., workers wait for the Pegasus launch vehicle to be moved inside. The Pegasus will carry the SciSat-1 spacecraft in a 400-mile-high polar orbit to investigate processes that control the distribution of ozone in the upper atmosphere. The scientific mission of SciSat-1 is to measure and understand the chemical processes that control the distribution of ozone in the Earth’s atmosphere, particularly at high altitudes. The data from the satellite will provide Canadian and international scientists with improved measurements relating to global ozone processes and help policymakers assess existing environmental policy and develop protective measures for improving the health of our atmosphere, preventing further ozone depletion. The mission is designed to last two years.

Methane concentrations in water wells unrelated to proximity to existing oil and gas wells in northeastern Pennsylvania.

PubMed

Siegel, Donald I; Azzolina, Nicholas A; Smith, Bert J; Perry, A Elizabeth; Bothun, Rikka L

2015-04-07

Recent studies in northeastern Pennsylvania report higher concentrations of dissolved methane in domestic water wells associated with proximity to nearby gas-producing wells [ Osborn et al. Proc. Natl. Acad. Sci. U. S. A. 2011 , 108 , 8172 ] and [ Jackson et al. Proc. Natl. Acad. Sci. U. S. A. , 2013 , 110 , 11250 ]. We test this possible association by using Chesapeake Energy's baseline data set of over 11,300 dissolved methane analyses from domestic water wells, densely arrayed in Bradford and nearby counties (Pennsylvania), and near 661 pre-existing oil and gas wells. The majority of these, 92%, were unconventional wells, drilled with horizontal legs and hydraulically fractured. Our data set is hundreds of times larger than data sets used in prior studies. In contrast to prior findings, we found no statistically significant relationship between dissolved methane concentrations in groundwater from domestic water wells and proximity to pre-existing oil or gas wells. Previous analyses used small sample sets compared to the population of domestic wells available, which may explain the difference in prior findings compared to ours.

Non-3D domain swapped crystal structure of truncated zebrafish alphaA crystallin

PubMed Central

Laganowsky, A; Eisenberg, D

2010-01-01

In previous work on truncated alpha crystallins (Laganowsky et al., Protein Sci 2010; 19:1031–1043), we determined crystal structures of the alpha crystallin core, a seven beta-stranded immunoglobulin-like domain, with its conserved C-terminal extension. These extensions swap into neighboring cores forming oligomeric assemblies. The extension is palindromic in sequence, binding in either of two directions. Here, we report the crystal structure of a truncated alphaA crystallin (AAC) from zebrafish (Danio rerio) revealing C-terminal extensions in a non three-dimensional (3D) domain swapped, “closed” state. The extension is quasi-palindromic, bound within its own zebrafish core domain, lying in the opposite direction to that of bovine AAC, which is bound within an adjacent core domain (Laganowsky et al., Protein Sci 2010; 19:1031–1043). Our findings establish that the C-terminal extension of alpha crystallin proteins can be either 3D domain swapped or non-3D domain swapped. This duality provides another molecular mechanism for alpha crystallin proteins to maintain the polydispersity that is crucial for eye lens transparency. PMID:20669149

Human mobility in large cities as a proxy for crime.

PubMed

Caminha, Carlos; Furtado, Vasco; Pequeno, Tarcisio H C; Ponte, Caio; Melo, Hygor P M; Oliveira, Erneson A; Andrade, José S

2017-01-01

We investigate at the subscale of the neighborhoods of a highly populated city the incidence of property crimes in terms of both the resident and the floating population. Our results show that a relevant allometric relation could only be observed between property crimes and floating population. More precisely, the evidence of a superlinear behavior indicates that a disproportional number of property crimes occurs in regions where an increased flow of people takes place in the city. For comparison, we also found that the number of crimes of peace disturbance only correlates well, and in a superlinear fashion too, with the resident population. Our study raises the interesting possibility that the superlinearity observed in previous studies [Bettencourt et al., Proc. Natl. Acad. Sci. USA 104, 7301 (2007) and Melo et al., Sci. Rep. 4, 6239 (2014)] for homicides versus population at the city scale could have its origin in the fact that the floating population, and not the resident one, should be taken as the relevant variable determining the intrinsic microdynamical behavior of the system.

Human mobility in large cities as a proxy for crime

PubMed Central

Caminha, Carlos; Furtado, Vasco; Pequeno, Tarcisio H. C.; Ponte, Caio; Melo, Hygor P. M.; Oliveira, Erneson A.; Andrade, José S.

2017-01-01

We investigate at the subscale of the neighborhoods of a highly populated city the incidence of property crimes in terms of both the resident and the floating population. Our results show that a relevant allometric relation could only be observed between property crimes and floating population. More precisely, the evidence of a superlinear behavior indicates that a disproportional number of property crimes occurs in regions where an increased flow of people takes place in the city. For comparison, we also found that the number of crimes of peace disturbance only correlates well, and in a superlinear fashion too, with the resident population. Our study raises the interesting possibility that the superlinearity observed in previous studies [Bettencourt et al., Proc. Natl. Acad. Sci. USA 104, 7301 (2007) and Melo et al., Sci. Rep. 4, 6239 (2014)] for homicides versus population at the city scale could have its origin in the fact that the floating population, and not the resident one, should be taken as the relevant variable determining the intrinsic microdynamical behavior of the system. PMID:28158268

Looking for Martian True Polar Wander in mutually oriented slices of ALH84001

NASA Astrophysics Data System (ADS)

Buz, J.; Murphy, T. G.; Kirschvink, J. L.

2016-12-01

True polar wander (TPW) on Mars has been hypothesized based on a variety of observations including geoid instability [1], locations of apparent polar deposits [2], and locations of magnetic anomalies [3, 4]. A proposed driving force for TPW is redistribution of mass on the surface of the planet such as by extensive volcanism events [5]. The majority of TPW modeling research has been using orbital datasets and modeling. However, laboratory analyses of Martian samples should also be conducted to test for Martian TPW. The Martian meteorite, ALH84001, is a prime sample for observing Martian TPW because of its preservation of thermal remanent magnetization from Mars [6]. Previous work on the sample has demonstrated that the interior of the meteorite was not heated above 40 C during transport from Mars to Earth and that there is a heterogeneous magnetization within the meteorite [7]. Within the meteorite are a series of fracture-filling carbonate blebs which contain magnetite and pyrrhotite with original remanence. These carbonates are presumed to have precipitated onto the meteorite [8]. We have divided a fracture-containing portion of the meteorite into three sets of sequential, mutually oriented slices. Using an ultra-high resolution scanning SQuID magnetometer we are able to visualize the magnetization within each slice. We are able to model each magnetic scan as a series of discrete dipoles using a modification from Lima and Weiss [9]. Our results demonstrate that within one of our slice sequences the dipoles lie along a great circle path. Dipoles lying along an arc in a stereographic projection can be interpreted as resulting from TPW if there is a significant amount of time from start to end of magnetization. Our ongoing work includes continued analysis and scanning of our slices as well as statistical tests for confirming if the dipoles lie along an arc. [1] Sprenke, KF et al. 2005 Icarus 174(2) 486-9 [2] Perron, JT et al. 2007 Nature 447(7146) 840-3 [3] Kobayashi, D & Sprenke, KF 2010 Icarus 210(1) 37-42 [4] Boutin, D & Arkani-Hamed, J 2006 Icarus 181(1) 13-25 [5] Kite, ES et al. 2009 Earth Planet Sci Lett 280(1-4) 254-67 [6] Weiss, B et al. 2000 Science 290(5492) 791-5 [7] Weiss, BP et al. 2002 Earth Planet Sci Lett 201(3-4) 449-63 [8] Halevy, I et al. 2011 Proc Natl Acad Sci 108(41) 16895-9 [9] Lima, EA & Weiss, BP 2009 J Geophys Res 114(B6)

SciSpark's SRDD : A Scientific Resilient Distributed Dataset for Multidimensional Data

NASA Astrophysics Data System (ADS)

Palamuttam, R. S.; Wilson, B. D.; Mogrovejo, R. M.; Whitehall, K. D.; Mattmann, C. A.; McGibbney, L. J.; Ramirez, P.

2015-12-01

Remote sensing data and climate model output are multi-dimensional arrays of massive sizes locked away in heterogeneous file formats (HDF5/4, NetCDF 3/4) and metadata models (HDF-EOS, CF) making it difficult to perform multi-stage, iterative science processing since each stage requires writing and reading data to and from disk. We have developed SciSpark, a robust Big Data framework, that extends ApacheTM Spark for scaling scientific computations. Apache Spark improves the map-reduce implementation in ApacheTM Hadoop for parallel computing on a cluster, by emphasizing in-memory computation, "spilling" to disk only as needed, and relying on lazy evaluation. Central to Spark is the Resilient Distributed Dataset (RDD), an in-memory distributed data structure that extends the functional paradigm provided by the Scala programming language. However, RDDs are ideal for tabular or unstructured data, and not for highly dimensional data. The SciSpark project introduces the Scientific Resilient Distributed Dataset (sRDD), a distributed-computing array structure which supports iterative scientific algorithms for multidimensional data. SciSpark processes data stored in NetCDF and HDF files by partitioning them across time or space and distributing the partitions among a cluster of compute nodes. We show usability and extensibility of SciSpark by implementing distributed algorithms for geospatial operations on large collections of multi-dimensional grids. In particular we address the problem of scaling an automated method for finding Mesoscale Convective Complexes. SciSpark provides a tensor interface to support the pluggability of different matrix libraries. We evaluate performance of the various matrix libraries in distributed pipelines, such as Nd4jTM and BreezeTM. We detail the architecture and design of SciSpark, our efforts to integrate climate science algorithms, parallel ingest and partitioning (sharding) of A-Train satellite observations from model grids. These solutions are encompassed in SciSpark, an open-source software framework for distributed computing on scientific data.

Investigating Hydroxyl at Asteroid 951 Gaspra

NASA Astrophysics Data System (ADS)

Granahan, James C.

2015-11-01

Recent investigations [Granahan, 2011; 2014] of Galileo Near Infrared Mapping Spectrometer (NIMS) observations of asteroid 951 Gaspra have detected an infrared absorption feature near 2.8 micrometers. These were detected in NIMS data acquired by the Galileo spacecraft on October 29, 1991 at wavelengths ranging from 0.7 - 5.2 micrometers [Carlson et al., 1992]. This abstract presents a summary of the investigation to identify the material creating the 2.8 micrometer spectral absorption feature. The current best match for the observed 951 Gaspra feature is the phyllosilicate bound hydroxyl signature present in a thermally desiccated QUE 99038 carbonaceous chondrite as measured by Takir et al. [2013].The 951 Gaspra absorption feature has been compared to a variety of hydroxyl bearing signatures. Many phyllosilicates, hydroxyl bearing minerals, have absorption minima at different positions (2.7 or 2.85 micrometers). It also differs from similar absorptions in a potential R chondrite analog, LAP 04840. The spectra LAP 04840 has a 2.7 micrometer feature due to biotite and a 2.9 micrometer feature due to adsorbed water [Klima et al., 2007]. 2.8 micrometer absorption minima have been found for adsorbed hydroxyl on the Moon [McCord et al., 2011] and various carbonaceous chondrites [Calvin and King, 1997; Takir et al., 2013]. The best match, with a minimum Euclidean distance difference to the 951 Gaspra feature, is found in the spectrum of QUE 99038 [Takir et al., 2013]. This spectrum is the product of an infrared measurement of a sample that had its adsorbed water baked off and removed in a vacuum chamber. The remaining hydroxyl in the sample belongs to a mixture of phyllosilicates dominated by the presence of cronstedtite.References: Calvin, W. M., and T. V. King (1997), Met. Planet. Sci., 32, 693-702. Carlson, R. W., et al. (1992), Bull. American Astro. Soc., 24, 932. Granahan, J. C. (2011), Icarus, 213, 265-272. Granahan, J. C. (2014), 45th LPSC, #1092. Klima, R., C. et al. (2007), 38th LPSC, #1710. McCord, T. B., et al. (2011), JGR, 116, E00G05. Takir, D., et al. (2013), Met. Planet. Sci., 48, 1618-1637.

Evaluating the flux of extraterrestrial osmium at the onset of Younger Dryas in the GRIP ice core

NASA Astrophysics Data System (ADS)

Seo, J. H.; Han, C.; Hong, S.; Steffensen, J. P.; Sharma, M.

2016-12-01

The Younger Dryas (YD: 12.9-11.6 ka) was an abrupt cooling event during the last deglaciation. The mechanism behind the cooling is suggested to be a temporary slowdown of North Atlantic thermohaline circulation due to catastrophic release of meltwater from proglacial Lake Agassiz during the retreat of the Laurentide Ice Sheet [1]. An alternative hypothesis states that the cooling was directly/indirectly triggered by one or more cosmic airbursts/impacts [2]. While several papers have documented evidence for a YD extraterrestrial impact including microspherules, nanodiamonds, magnetic grains, and glass-like carbon [4-7], this hypothesis remains controversial [8-10]. In a recent study by Petaev et al. [11], an unusually high Pt/Ir ratio of 1200 was discovered in the GISP-2 ice core at the onset of YD, indicating a large Pt enriched iron meteorite impact. Such a high Pt/Ir in extraterrestrial materials has not been documented [12]. Thus, Petaev et al. [11] acknowledge that the interpretation of the Pt anomaly is based on circumstantial evidence. The distinct Os isotopic composition (187Os/188Os ratio) of the terrestrial (=1.26) and extraterrestrial (= 0.13) sources should allow us to evaluate if there was a meteorite impact at the YD boundary. These analyses are technically challenging owing to rather low concentration of Os in ice-melts ( 1x10-15g/g). Here, we will present Os isotope data from the GRIP ice core spanning the time period through YD to shed light on the meteorite/comet impact hypothesis. [1] Broecker et al. (1989) Nature 341, 318-321; [2] Firestone et al. (2007) PNAS. 104, 16016-16021; [3] Bunch et al. (2012) PNAS. 109, 1903-1912; [4] LeCompte et al. (2012) PNAS. 109, 2960-2969; [5] Wittke et al. (2013) PNAS 110, 2088-2097; [6] Wu et al. (2013) PNAS. 110, 3557-3566; [7] Kennett et al. (2015) PNAS 112, E4344-E4353; [8] Pinter et al. (2011) Earth Sci. Rev., 106, 247-264; [9] Holliday et al. (2014) J. Quat. Sci. 29, 515-530; [10] Meltzer et al. (2014) PNAS. 111, 2162-2171; [11] Petaev et al. (2013) PNAS. 110, 12917-12920; [12] Wasson et al. (2007) GCA. 71:760-781

Exploring Jupiter's icy moons with old techniques and big facilities - new insights on sulfuric acid hydrates

NASA Astrophysics Data System (ADS)

Maynard-Casely, H. E.; Avdeev, M.; Brand, H.; Wallwork, K.

2013-12-01

Sulfuric acid hydrates have been proposed to be abundant on the surface of Europa [1], and hence would be important planetary forming materials for this moon and its companions Ganymede and Callisto. Understanding of the surface features and subsurface of these moons could be advanced by firmer knowledge of the icy materials that comprise them [2], insight into which can be drawn from firmer knowledge of physical properties and phase behaviour of the candidate materials. We wish to present results from a study that started with the question ';What form of sulfuric acid hydrate would form on the surface of Europa'. The intrinsic hydrogen-domination of planetary ices, makes studying these materials with laboratory powder diffraction very challenging. Insights into their crystalline phase behavior and the extraction of a number of thermal and mechanical properties is often only accessible with high-flux synchrotron x-ray diffraction and utilization of the large scattering cross section with neutron diffraction. We have used the Powder Diffraction beamline at Australian synchrotron [4] and the Echidna (High-resolution neutron powder diffraction) instrument of the Australian Nuclear Science and Technology Organization, [5] to obtain an number of new insights into the crystalline phases formed from sulfruic acid and water mixtures. These instruments have enabled the discovery a new water-rich sulfuric acid hydrate form [6], improved structural characterisation of existing forms [7] and a charting the phase diagram of this fundamental binary system [8]. This has revealed exciting potential for understanding more about the surface of Europa from space, perhaps even providing a window into its past. [1] Carlson, R.W., R.E. Johnson, and M.S. Anderson, Science, 1999. 286(5437): p. 97-99. [2] Fortes, A.D. and M. Choukroun. Space Sci Rev, 2010. 153(1-4): p. 185-218. [3] Blake, D., et al., Space Sci Rev,, 2012. 170(1-4): p. 341-399. [4] Wallwork, K.S., Kennedy B. J. and Wang, D., AIP Conf Proc, 2007. 879: p. 879-882. [5] Liss, K.D., et al., Phys B-Cond Mat, 2006. 385-86: p. 1010-1012. [6] Maynard-Casely, H.E., K.S. Wallwork, and M. Avdeev, (In review). [7] Maynard-Casely, H.E., H.E.A. Brand, and K.S. Wallwork, J.of App.Cryst, 2012. 45: p.1198-1207. [8] Maynard-Casely, H.E., K.S. Wallwork, and H.E.A. Brand, (In Preparation). Stages of the crystal structure determination of sulfruic acid octahydrate a) the oxygen and sulfur postions were determined from the synchrotron x-ray data b) Once neutron diffraction data was collected Fourier difference methods were used to locate hydrogen positions to determine c) the full structure of sulfuric acid octahydrate.

Atomic model of anti-phase boundaries in a face-centred icosahedral Zn Mg Dy quasicrystal

NASA Astrophysics Data System (ADS)

Wang, Jianbo; Yang, Wenge; Wang, Renhui

2003-03-01

An atomic model in the physical space for an anti-phase boundary (APB) in the ordered face-centred icosahedral Zn-Mg-Dy quasicrystal phase is presented, based on a six-dimensional model suggested by Ishimasa and Shimizu (2000 Mater. Sci. Eng. A 294-296 232, Ishimasa 2001 private communication). The physical space atomic positions of the defected structure were used for the calculation of the corresponding exit-plane wavefunction and high-resolution transmission electron microscopy images. The analysis of the defect by inverse Fourier transformation reveals that when superstructure reflection spots are used for back-transformation, then at the APB, bright lattice fringes are found to turn into dark ones, and vice versa. When fundamental reflections are used, the APB is not visible. This phenomenon is the same as the corresponding experimental study recently published by Heggen et al(2001a Phys. Rev. B 64 014202). Based on this atomic model it is found that the APB perpendicular to a fivefold axis A5 (APB-A5) is a non-conservative boundary, while the APB perpendicular to a pseudo-twofold axis A2P (APB-A2P) is a conservative one. This fact is consistent with the experimental observation (Heggen et al2002 J. Alloys Compounds 342 330) that the frequency of occurrence of APB-A5 is 90% in the heat-treated samples compared with that in the deformed samples (45%), while the frequency of occurrence of APB-A2P is 34% in the deformed samples compared with that in the heat-treated samples.

Three-dimensional thermal structure of the South Polar Vortex of Venus

NASA Astrophysics Data System (ADS)

Hueso, Ricardo; Garate-Lopez, Itziar; Garcia-Muñoz, Antonio; Sánchez-Lavega, Agustín

2014-11-01

We have analyzed thermal infrared images provided by the VIRTIS-M instrument aboard Venus Express (VEX) to obtain high resolution thermal maps of the Venus south polar region between 55 and 85 km altitudes. The maps investigate three different dynamical configurations of the polar vortex including its classical dipolar shape, a regularly oval shape and a transition shape between the different configurations of the vortex. We apply the atmospheric model described by García Muñoz et al. (2013) and a variant of the retrieval algorithm detailed in Grassi et al. (2008) to obtain maps of temperature over the Venus south polar region in the quoted altitude range. These maps are discussed in terms of cloud motions and relative vorticity distribution obtained previously (Garate-Lopez et al. 2013). Temperature maps retrieved at 55 - 63 km show the same structures that are observed in the ~5 µm radiance images. This altitude range coincides with the optimal expected values of the cloud top altitude at polar latitudes and magnitudes derived from the analysis of ~5 µm images are measured at this altitude range. We also study the imprint of the vortex on the thermal field above the cloud level which extends up to 80 km. From the temperature maps, we also study the vertical stability of different atmospheric layers. The cold collar is clearly the most statically stable structure at polar latitudes, while the vortex and subpolar latitudes show lower stability values. Furthermore, the hot filaments present within the vortex at 55-63 km exhibit lower values of static stability than their immediate surroundings.ReferencesGarate-Lopez et al. Nat. Geosci. 6, 254-257 (2013).García Muñoz et al. Planet. Space Sci. 81, 65-73 (2013).Grassi, D. et al. J. Geophys. Res. 113, 1-12 (2008).AcknowledgementsWe thank ESA for supporting Venus Express, ASI, CNES and the other national space agencies supporting VIRTIS on VEX and their principal investigators G. Piccioni and P. Drossart. This work was supported by projects AYA2012-36666 with FEDER support, PRICI-S2009/ESP-1496, Grupos Gobierno Vasco IT-765-13 and by UPV/EHU through program UFI11/55. IGL and AGM acknowledge ESA/RSSD for hospitality and access to ‘The Grid’ computing resources.

SciServer: An Online Collaborative Environment for Big Data in Research and Education

NASA Astrophysics Data System (ADS)

Raddick, Jordan; Souter, Barbara; Lemson, Gerard; Taghizadeh-Popp, Manuchehr

2017-01-01

For the past year, SciServer Compute (http://compute.sciserver.org) has offered access to big data resources running within server-side Docker containers. Compute has allowed thousands of researchers to bring advanced analysis to big datasets like the Sloan Digital Sky Survey and others, while keeping the analysis close to the data for better performance and easier read/write access. SciServer Compute is just one part of the SciServer system being developed at Johns Hopkins University, which provides an easy-to-use collaborative research environment for astronomy and many other sciences.SciServer enables these collaborative research strategies using Jupyter notebooks, in which users can write their own Python and R scripts and execute them on the same server as the data. We have written special-purpose libraries for querying, reading, and writing data. Intermediate results can be stored in large scratch space (hundreds of TBs) and analyzed directly from within Python or R with state-of-the-art visualization and machine learning libraries. Users can store science-ready results in their permanent allocation on SciDrive, a Dropbox-like system for sharing and publishing files.SciServer Compute’s virtual research environment has grown with the addition of task management and access control functions, allowing collaborators to share both data and analysis scripts securely across the world. These features also open up new possibilities for education, allowing instructors to share datasets with students and students to write analysis scripts to share with their instructors. We are leveraging these features into a new system called “SciServer Courseware,” which will allow instructors to share assignments with their students, allowing students to engage with big data in new ways.SciServer has also expanded to include more datasets beyond the Sloan Digital Sky Survey. A part of that growth has been the addition of the SkyQuery component, which allows for simple, fast cross-matching between very large astronomical datasets.Demos, documentation, and more information about all these resources can be found at www.sciserver.org.

Optimal Transport, Convection, Magnetic Relaxation and Generalized Boussinesq Equations

NASA Astrophysics Data System (ADS)

Brenier, Yann

2009-10-01

We establish a connection between optimal transport theory (see Villani in Topics in optimal transportation. Graduate studies in mathematics, vol. 58, AMS, Providence, 2003, for instance) and classical convection theory for geophysical flows (Pedlosky, in Geophysical fluid dynamics, Springer, New York, 1979). Our starting point is the model designed few years ago by Angenent, Haker, and Tannenbaum (SIAM J. Math. Anal. 35:61-97, 2003) to solve some optimal transport problems. This model can be seen as a generalization of the Darcy-Boussinesq equations, which is a degenerate version of the Navier-Stokes-Boussinesq (NSB) equations. In a unified framework, we relate different variants of the NSB equations (in particular what we call the generalized hydrostatic-Boussinesq equations) to various models involving optimal transport (and the related Monge-Ampère equation, Brenier in Commun. Pure Appl. Math. 64:375-417, 1991; Caffarelli in Commun. Pure Appl. Math. 45:1141-1151, 1992). This includes the 2D semi-geostrophic equations (Hoskins in Annual review of fluid mechanics, vol. 14, pp. 131-151, Palo Alto, 1982; Cullen et al. in SIAM J. Appl. Math. 51:20-31, 1991, Arch. Ration. Mech. Anal. 185:341-363, 2007; Benamou and Brenier in SIAM J. Appl. Math. 58:1450-1461, 1998; Loeper in SIAM J. Math. Anal. 38:795-823, 2006) and some fully nonlinear versions of the so-called high-field limit of the Vlasov-Poisson system (Nieto et al. in Arch. Ration. Mech. Anal. 158:29-59, 2001) and of the Keller-Segel for Chemotaxis (Keller and Segel in J. Theor. Biol. 30:225-234, 1971; Jäger and Luckhaus in Trans. Am. Math. Soc. 329:819-824, 1992; Chalub et al. in Mon. Math. 142:123-141, 2004). Mathematically speaking, we establish some existence theorems for local smooth, global smooth or global weak solutions of the different models. We also justify that the inertia terms can be rigorously neglected under appropriate scaling assumptions in the generalized Navier-Stokes-Boussinesq equations. Finally, we show how a “stringy” generalization of the AHT model can be related to the magnetic relaxation model studied by Arnold and Moffatt to obtain stationary solutions of the Euler equations with prescribed topology (see Arnold and Khesin in Topological methods in hydrodynamics. Applied mathematical sciences, vol. 125, Springer, Berlin, 1998; Moffatt in J. Fluid Mech. 159:359-378, 1985, Topological aspects of the dynamics of fluids and plasmas. NATO adv. sci. inst. ser. E, appl. sci., vol. 218, Kluwer, Dordrecht, 1992; Schonbek in Theory of the Navier-Stokes equations, Ser. adv. math. appl. sci., vol. 47, pp. 179-184, World Sci., Singapore, 1998; Vladimirov et al. in J. Fluid Mech. 390:127-150, 1999; Nishiyama in Bull. Inst. Math. Acad. Sin. (N.S.) 2:139-154, 2007).

Corrigendum to “Widespread occurrence of (per)chlorate in the Solar System” [Earth Planet. Sci. Lett. 430 (2015) 470–476

USGS Publications Warehouse

Jackson, W. Andrew; Davila, Alfonso F.; Sears, Derek W. G.; Coates, John D.; McKay, Christopher P.; Brundrett, Maeghan; Estrada, Nubia; Böhlke, John Karl

2016-01-01

The authors regret that two sets of data (Atacama (Rao et al., 2010) and Mars Meteorite Range (Kounaves et al., 2014)) in Fig. 2 of our article were plotted in the wrong units. The correction does not change the relationship between ClO3−">ClO3− and ClO4−">ClO4−; it only shifts the magnitude of the concentrations. The conclusions of the article are not affected. The corrected Fig. 2 appears below.

Hyla gratiosa (barking treefrog) intestinal hernia

USGS Publications Warehouse

Mitchell, J.C.; Green, D.E.

2003-01-01

Deformities and malformations in anurans occur in a variety of manifestations (Meteyer 2000. Field Guide to Malformations of Frogs and Toads with Radiographic Interpretations. Biol. Sci. Rep., USGS/BRD/BSR-2000-0005, 18 pp.). Most of those described in the literature are visible externally (e.g., ectromelia, brachydactyly, polydactyly, brachygnathia, kyphosis) (Ouellet et al. 1997. J. Wildlife Dis. 33:95-104). Internal malformations are less well known and seldom reported (Reeder et al. 1998. Environ. Health Persp. 106:261-266). Here we describe an unusual condition heretofore unreported for a hylid frog.

Nanotwins in Nanocrystalline Mg-Al Alloys: An Insight from High-Resolution TEM and Molecular Dynamics Simulation

DTIC Science & Technology

2013-09-25

Mathaudhu, C.Y.A. Tsao and E.J. Lavernia, Mater. Sci. Eng. A528 (2011) p. 2180. [21] S . Plimpton , J. Comput. Phys. 117 (1995) p. 1. [22] X.-Y. Liu, J.B...grained Mg are identi ? ed and supported with atomistic The views, opinions and/or findings contained in this report are those of the author( s ) and should...MONITORING AGENCY NAME( S ) AND ADDRESS (ES) U.S. Army Research Office P.O. Box 12211 Research Triangle Park, NC 27709-2211 nanocrystalline Mg – Al alloys

Interface Properties of Wide Bandgap Semiconductor Structures

DTIC Science & Technology

1994-06-01

resistive than silicides and their chemistry with 126I I Si-based materials more complex. However, in a series of studies, M. 0. Aboelfotoh et al. have...clarification of these issues. CuGe contacts on Ge:GaN and Mg:GaN. To date, the properties of Cu3Ge films have been documented by Aboelfotoh et al., but the...Martin, V. Malhotra, and J. E. Mahan, J. Vac. Sci. Technol. B 3, 836 (1985). 25. L. Krusin-Elbaum and M. 0. Aboelfotoh , Appl. Phys. Lett. 58(12), 1341

Molecular Profiles for Lung Cancer Pathogenesis and Detection in US Veterans

DTIC Science & Technology

2011-10-01

raw image files that were subsequently converted to probe set data. Raw expression data was analyzed using the BRB-ArrayTools v .4.1.0 developed by Dr...epithelium of cigarette smokers. Am J Respir Cell Mol Biol 2003;29:331-343 14. Spira A, Beane J, Shah V , et al. Effects of cigarette smoke on the...human airway epithelial cell transcriptome. Proc Natl Acad Sci U S A 2004;101:10143-10148 15. Spira A, Beane JE, Shah V , et al. Airway epithelial gene

Phase Equilibria of Stored Chemical Energy Reactants.

DTIC Science & Technology

1984-07-25

aluminate-lithium ferrate system. Detection of a Li1 Al4/7Fe 3/704 compound: C. R. Acad. Sci., Ser. C, V. 273, No. 15, p. 888-90. McNicol, B. D. and Pott...thermodynamic properties of lithium ferrate (LiO.5Fe2 .504) and lithium aluminate (LiO 5Al 2 504) from 5 to 545 K: J. Chem. Thermodyn., V. 7, No. 7, p. 693- 2...1977, Study of low-temperature hydrothermal crystallization in lithium oxide-silicon dioxide-water, potassium oxide-silicon dioxide-water, and

Mo isotope record of shales points to deep ocean oxygenation in the early Paleoproterozoic

NASA Astrophysics Data System (ADS)

Asael, Dan; Scott, Clint; Rouxel, Olivier; Poulton, Simon; Lyons, Timothy; Javaux, Emmanuelle; Bekker, Andrey

2014-05-01

Two steps in Earth's surface oxidation lie at either end of the Proterozoic Eon. The first step, known as the Great Oxidation Event (GOE), occurred at ca. 2.32 Ga (1), when atmospheric oxygen first exceeded 0.001% of present atmospheric levels (2). The second step, occurred at ca. 0.58 Ga, resulting in the pervasive oxygenation of the deep oceans, a feature that persisted through most of the Phanerozoic (3). The conventional model envisions two progressive and unidirectional increases in free oxygen. However, recent studies have challenged this simplistic view of the GOE (4, 5). A dramatic increase and decline in Earth oxidation state between 2.3 and 2.0 Ga is now well supported (6-9) and raises the question of how well-oxygenated the Earth surface was in the immediate aftermath of the GOE. In order to constrain the response of the deep oceans to the GOE, we present a study of Mo isotope composition and Mo concentration from three key early Paleoproterozoic black shale units with ages ranging from 2.32 to 2.06 Ga. Our results suggest high and unstable surface oxygen levels at 2.32 Ga, leading to an abrupt increase in Mo supply to the still globally anoxic ocean, and producing extreme seawater Mo isotopic enrichments in these black shales. We thus infer a period of significant Mo isotopic Rayleigh effects and non-steady state behaviour of the Mo oceanic system at the beginning of the GOE. Between 2.2-2.1 Ga, we observe smaller Mo isotopic variations and estimate the δ98Mo of seawater to be 1.42 ± 0.27 ‰W conclude that oxygen levels must have stabilized at a relatively high level and that the deep oceans were oxygenated for the first time in Earth's history. By ca. 2.06 Ga, immediately after the Lomagundi Event, the Mo isotopic composition decreased dramatically to δ98MoSW = 0.80 ± 0.21 o reflecting the end of deep ocean oxygenation and the return of largely anoxic deep oceans. References: [1] A. Bekker et al., 2004, Nature 427, 117-20. [2] A. Pavlov and J. Kasting, 2002, Astrobiology 2, 27-41. [3] C. Scott et al., 2008, Nature 452, 456-9. [4] C. Goldblatt et al., 2006, Nature 443, 683-6. [5] L. Kump et al., 2011, Science 334, 1694-6. [6] A. Bekker and D. Holland, 2012, Earth Planet. Sci. Lett. 317-318, 295-304. [7] N. Planavsky et al., 2012, Proc. Natl. Acad. Sci. U. S. A. 109, 18300-5. [8] C. Partin et al., 2013, Chem. Geol. 362, 82-90. [9] C. Scott et al., 2014, Earth Planet. Sci. Lett. 389, 95-104.

The Noble Gas Abundances in the Coma of Comet 67P/Churyumov-Gerasimenko from Rosetta/ROSINA

NASA Astrophysics Data System (ADS)

Rubin, M.; Altwegg, K.; Balsiger, H. R.; Berthelier, J. J.; Briois, C.; Combi, M. R.; De Keyser, J.; Fiethe, B.; Fuselier, S. A.; Gasc, S.; Gombosi, T. I.; Hansen, K. C.; Jäckel, A.; Kopp, E.; Korth, A.; Mall, U.; Marty, B.; Mousis, O.; Owen, T.; Reme, H.; Schuhmann, M.; Schroeder, I. R. H. G.; Semon, T.; Tzou, C. Y.; Waite, J. H., Jr.; Wurz, P.

2017-12-01

The Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA), the mass spectrometer suite on board the European Space Agency's Rosetta mission, was dedicated to the measurement of the volatiles in the coma of comet 67P/Churyumov-Gerasimenko (67P) [1]. Among many other species, ROSINA DFMS, the Double Focusing Mass Spectrometer, detected and quantified the three noble gases argon, krypton, and xenon including their major isotopes [2,3]. Noble gases provide important clues to the physical and chemical conditions during and possibly even before and after the comet's formation in the early solar system. Furthermore, measurements of the isotope ratios provide constraints on the amount of cometary material brought to Earth and its early atmosphere. In this presentation, we will report on the measured coma densities and derived nucleus bulk abundances of these three noble gases and investigate correlations with other volatiles. Furthermore, we will discuss the measured isotope ratios and the implications of these results. AcknowledgementsUoB was funded by the State of Bern, the Swiss National Science Foundation and by the European Space Agency PRODEX Programme. Work at MPS was funded by the Max-Planck Gesellschaft and BMWI (contract 50QP1302), at Southwest Research institute by Jet Propulsion Laboratory (subcontract #1496541 and JPL subcontract to JWH NAS703001TONMO710889), at the University of Michigan by NASA (contract JPL-1266313). This work has been supported through the A*MIDEX project from the French National Research Agency (ANR) (n° ANR-11-IDEX- 0001-02) and by CNES grants at IRAP, LATMOS, LPC2E, LAM, CRPG, by the European Research Council (grant no. 267255 to B. Marty) and at BIRA-IASB by the Belgian Science Policy Office via PRODEX/ROSINA PEA C4000107705. References[1] Balsiger, H., et al., Rosina - Rosetta orbiter spectrometer for ion and neutral analysis. Space Science Reviews. 128, 745-801, 2007. [2] Balsiger, H., et al., Detection of argon in the coma of comet 67P/Churyumov-Gerasimenko. Sci Adv. 1, e1500377, 2015. [3] Marty B., et al., Xenon isotopes in 67P/Churyumov-Gerasimenko show that comets contributed to Earth's atmosphere, Science, 356, 1069 - 1072, 2017.

Evidence for frozen hydrocarbons on Titan

NASA Astrophysics Data System (ADS)

Soderblom, Jason M.; Barnes, Jason W.; Brown, Robert H.; Chevrier, Vincent; Farnsworth, Kendra; Soderblom, Laurence A.

2016-10-01

Cassini Visual and Infrared Mapping Spectrometer (VIMS) and Imaging Science Subsystem (ISS) have twice, now, observed widespread darkening of Titan's surface that has been interpreted as evidence of rainfall (Turtle et al., 2009, GRL 36; Turtle et al., 2011, Science 331) followed by an increase in albedo, well beyond the pre-darkened albedo (Barnes et al., 2013, Planet. Sci. 2; Soderblom et al., 2014, DPS). Based on the timescale and magnitude of the albedo changes, and the correlations between the timescale and temperature (inferred from latitude), we favor a thermodynamically controlled process to explain the brightening. Herein, we present a detailed comparison of the IR spectra of the bright materials of these two events. We also discuss the implications on the interpretation of these data from recent laboratory work investigating the freezing of ethane at Titan-like conditions (Farnsworth et al., 2016, LPSC 47).

How the science and engineering of spaceflight contribute to understanding the plasticity of spinal cord injury

NASA Technical Reports Server (NTRS)

Edgerton, V. R.; Roy, R. R.; Hodgson, J. A.; Day, M. K.; Weiss, J.; Harkema, S. J.; Dobkin, B.; Garfinkel, A.; Konigsberg, E.; Koslovskaya, I.

2000-01-01

Space programs support experimental investigations related to the unique environment of space and to the technological developments from many disciplines of both science and engineering that contribute to space studies. Furthermore, interactions between scientists, engineers and administrators, that are necessary for the success of any science mission in space, promote interdiscipline communication, understanding and interests which extend well beyond a specific mission. NASA-catalyzed collaborations have benefited the spinal cord rehabilitation program at UCLA in fundamental science and in the application of expertise and technologies originally developed for the space program. Examples of these benefits include: (1) better understanding of the role of load in maintaining healthy muscle and motor function, resulting in a spinal cord injury (SCI) rehabilitation program based on muscle/limb loading; (2) investigation of a potentially novel growth factor affected by spaceflight which may help regulate muscle mass; (3) development of implantable sensors, electronics and software to monitor and analyze long-term muscle activity in unrestrained subjects; (4) development of hardware to assist therapies applied to SCI patients; and (5) development of computer models to simulate stepping which will be used to investigate the effects of neurological deficits (muscle weakness or inappropriate activation) and to evaluate therapies to correct these deficiencies.

Configuration of Pluto's Volatile Ices

NASA Astrophysics Data System (ADS)

Grundy, William M.; Binzel, R. P.; Cook, J. C.; Cruikshank, D. P.; Dalle Ore, C. M.; Earle, A. M.; Ennico, K.; Jennings, D. E.; Howett, C. J. A.; Linscott, I. R.; Lunsford, A. W.; Olkin, C. B.; Parker, A. H.; Parker, J. Wm; Protopapa, S.; Reuter, D. C.; Singer, K. N.; Spencer, J. R.; Stern, S. A.; Tsang, C. C. C.; Verbiscer, A. J.; Weaver, H. A.; Young, L. A.; Berry, K.; Buie, M. W.; Stansberry, J. A.

2015-11-01

We report on near-infrared remote sensing by New Horizons' Ralph instrument (Reuter et al. 2008, Space Sci. Rev. 140, 129-154) of Pluto's N2, CO, and CH4 ices. These especially volatile ices are mobile even at Pluto's cryogenic surface temperatures. Sunlight reflected from these ices becomes imprinted with their characteristic spectral absorption bands. The detailed appearance of these absorption features depends on many aspects of local composition, thermodynamic state, and texture. Multiple-scattering radiative transfer models are used to retrieve quantitative information about these properties and to map how they vary across Pluto's surface. Using parameter maps derived from New Horizons observations, we investigate the striking regional differences in the abundances and scattering properties of Pluto's volatile ices. Comparing these spatial patterns with the underlying geology provides valuable constraints on processes actively modifying the planet's surface, over a variety of spatial scales ranging from global latitudinal patterns to more regional and local processes within and around the feature informally known as Sputnik Planum. This work was supported by the NASA New Horizons Project.

The MicrOmega Investigation Onboard Hayabusa2

NASA Astrophysics Data System (ADS)

Bibring, J.-P.; Hamm, V.; Langevin, Y.; Pilorget, C.; Arondel, A.; Bouzit, M.; Chaigneau, M.; Crane, B.; Darié, A.; Evesque, C.; Hansotte, J.; Gardien, V.; Gonnod, L.; Leclech, J.-C.; Meslier, L.; Redon, T.; Tamiatto, C.; Tosti, S.; Thoores, N.

2017-07-01

MicrOmega is a near-IR hyperspectral microscope designed to characterize in situ the texture and composition of the surface materials of the Hayabusa2 target asteroid. MicrOmega is implemented within the MASCOT lander (Ho et al. in Space Sci. Rev., 2016, this issue, doi:10.1007/s11214-016-0251-6). The spectral range (0.99-3.65 μm) and the spectral sampling (20 cm^{-1}) of MicrOmega have been chosen to allow the identification of most potential constituent minerals, ices and organics, within each 25 μm pixel of the 3.2× 3.2 mm2 FOV. Such an unprecedented characterization will (1) enable the identification of most major and minor phases, including the potential organic phases, and ascribe their mineralogical context, as a critical set of clues to decipher the origin and evolution of this primitive body, and (2) provide the ground truth for the orbital measurements as well as a reference for the analyses later performed on returned samples.

Exploring the limits of case-to-capsule ratio, pulse length, and picket energy for symmetric hohlraum drive on the National Ignition Facility Laser

NASA Astrophysics Data System (ADS)

Callahan, D. A.; Hurricane, O. A.; Ralph, J. E.; Thomas, C. A.; Baker, K. L.; Benedetti, L. R.; Berzak Hopkins, L. F.; Casey, D. T.; Chapman, T.; Czajka, C. E.; Dewald, E. L.; Divol, L.; Döppner, T.; Hinkel, D. E.; Hohenberger, M.; Jarrott, L. C.; Khan, S. F.; Kritcher, A. L.; Landen, O. L.; LePape, S.; MacLaren, S. A.; Masse, L. P.; Meezan, N. B.; Pak, A. E.; Salmonson, J. D.; Woods, D. T.; Izumi, N.; Ma, T.; Mariscal, D. A.; Nagel, S. R.; Kline, J. L.; Kyrala, G. A.; Loomis, E. N.; Yi, S. A.; Zylstra, A. B.; Batha, S. H.

2018-05-01

We present a data-based model for low mode asymmetry in low gas-fill hohlraum experiments on the National Ignition Facility {NIF [Moses et al., Fusion Sci. Technol. 69, 1 (2016)]} laser. This model is based on the hypothesis that the asymmetry in these low fill hohlraums is dominated by the hydrodynamics of the expanding, low density, high-Z (gold or uranium) "bubble," which occurs where the intense outer cone laser beams hit the high-Z hohlraum wall. We developed a simple model which states that the implosion symmetry becomes more oblate as the high-Z bubble size becomes large compared to the hohlraum radius or the capsule size becomes large compared to the hohlraum radius. This simple model captures the trends that we see in data that span much of the parameter space of interest for NIF ignition experiments. We are now using this model as a constraint on new designs for experiments on the NIF.

Detailed characterization of the LLNL imaging proton spectrometer

DOE Office of Scientific and Technical Information (OSTI.GOV)

Rasmus, A. M., E-mail: rasmus@lanl.gov, E-mail: arasmus@umich.edu; University of Michigan, Ann Arbor, Michigan 48109; Hazi, A. U.

2016-11-15

Ultra-intense short pulse lasers incident on solid targets (e.g., thin Au foils) produce well collimated, broad-spectrum proton beams. These proton beams can be used to characterize magnetic fields, electric fields, and density gradients in high energy-density systems. The LLNL-Imaging Proton Spectrometer (L-IPS) was designed and built [H. Chen et al., Rev. Sci. Instrum. 81, 10D314 (2010)] for use with such laser produced proton beams. The L-IPS has an energy range of 50 keV-40 MeV with a resolving power (E/dE) of about 275 at 1 MeV and 21 at 20 MeV, as well as a single spatial imaging axis. In ordermore » to better characterize the dispersion and imaging capability of this diagnostic, a 3D finite element analysis solver is used to calculate the magnetic field of the L-IPS. Particle trajectories are then obtained via numerical integration to determine the dispersion relation of the L-IPS in both energy and angular space.« less

Complication of Spice Use in a Deployed Combat Setting - Seizure While on Duty

DTIC Science & Technology

2012-01-01

Eiserloh I, et al. Spice: A never ending story? Forensic Sci Int. 2009;191:58–63. 2. Johnson LA, Johnson RL, Alfonzo C. Spice. A Legal marijuana equiv... marijuana . Ann Pharmacother. 2011;45:414–417. 5. Gordon E, Devinsky O. Alcohol and marijuana : Effects on epilepsy and use by patients with epilepsy

Experimental Study of Turbulent Mixing and Selectivity of Competing Reactions

DTIC Science & Technology

1988-07-01

polymerization reactors ( Van der Molen et al., 1982). MIixing is also recognized as a key factor affecting overall performance of a combustor--both in terms...Eng. Sci., 28, 413 (1973). Van der Molen , T. J., A. Koenen, H. H. J. Oosterwijk, and H. Th. Van der Bend. "Effect of Process Conditions on Light-Off

Exploring the Repeated Name Penalty and the Overt Pronoun Penalty in Spanish

ERIC Educational Resources Information Center

Gelormini-Lezama, Carlos

2018-01-01

Anaphoric expressions such as repeated names, overt pronouns, and null pronouns serve a major role in the creation and maintenance of discourse coherence. The felicitous use of an anaphoric expression is highly dependent on the discourse salience of the entity introduced by the antecedent. Gordon et al. ("Cogn Sci" 17:311-347, 1993)…

An Observational Study of a Prefrontal Convective Rainband Using Tamex Single-and Dual-Doppler Data

DTIC Science & Technology

1991-01-01

integration from the surface. Other Doppler studies, e.g., Chong and Testud (1983), Lin et al. 37 (1986), etc, also showed similiar results. 4.3 Variational...Atmos. Sci., 39, 258- 279. Chong, M., and J. Testud , 1983: Three-Dimensional Wind Field Analysis from Dual-Doppler Radar Data. Part III: The Boundary

Elementary Preservice Teachers' Science Vocabulary: Knowledge and Application

ERIC Educational Resources Information Center

Carrier, Sarah J.

2013-01-01

Science vocabulary knowledge plays a role in understanding science concepts, and science knowledge is measured in part by correct use of science vocabulary (Lee et al. in "J Res Sci Teach" 32(8):797-816, 1995). Elementary school students have growing vocabularies and many are learning English as a secondary language or depend on schools to learn…

The Development of a Self-Regulation in a Collaborative Context Scale

ERIC Educational Resources Information Center

Law, Victor; Ge, Xun; Eseryel, Deniz

2016-01-01

Self-regulation has been shown as a critical factor in learning in a regular classroom environment (e.g. Wolters and Pintrich in "Instr Sci" 26(1):27-47, 1998. doi: 10.1023/A:1003035929216). However, little research has been conducted to understand self-regulation in the context of collaboration (Dinsmore et al. in "Educ Psychol…

Anti and Androgenic Activities in MDA-KB2 Cells: A Comparison of Performance in 96 Well Versus HTS Assays

EPA Science Inventory

We developed the MDA-kb2 cell line to screen androgen agonists/antagonists (Wilson et al., ToxSci 66:69, 2002). MDA-kb2 has been used to quantify anti- and androgenic activities of chemicals, mixtures, combustion by-products, oil dispersants and waste, source and drinking water s...

Expanding the Conversation: Further Explorations into Indigenous Environmental Science Education Theory, Research, and Practice

ERIC Educational Resources Information Center

Lowan, Greg

2012-01-01

Indigenous environmental science education is a diverse, dynamic, and rapidly expanding field of research, theory, and practice. This article highlights, challenges, and expands upon key areas of discussion presented by Mack et al. (Cult Stud Sci Educ 7, "2012") as part of the forum on their article "Effective Practices for Creating…

Linking spinal cord injury rehabilitation between the World Wars: The R. Tait McKenzie legacy.

PubMed

Ditunno, John F

2017-11-01

Spinal cord injury (SCI) medicine emerged after World War II due to mass casualties, which required specialized treatment centers. This approach to categorical care, however, was first developed during World War I, led by pioneers R. Tait McKenzie and George Deaver, who demonstrated that soldiers disabled by paralysis could return to society through fitness/mobility, recreational and vocational training. McKenzie, a Canadian and the first professor of physical therapy in the US, influenced Deaver and military physicians in Britain, Canada, and the U.S. with his achievements and publications. Although early mortality from SCI was high, advances in the treatment of skin and bladder complications coupled with rehabilitation developed through lessons learned in World War I, resulted in major changes in survival and quality of life for veterans of World War II in England, US, and Canada. Harry Botterell and Al Jousse, founders of Lyndhurst Lodge, the first SCI center in Canada, adopted Deaver's principles and techniques of rehabilitation and Donald Munro's approach to medical complications. The consequences of failing to organize continuity of care in World War I were recognized both by consumers and physicians. Together with John Counsell, a World War II veteran, they formed the Canadian Paraplegic Association, which "revolutionized" the care of veterans with SCI, as well as civilians, women, and children.

Effect of Heat Treatment on Chemical Segregation in CMSX-4 Nickel-Base Superalloy

NASA Astrophysics Data System (ADS)

Szczotok, A.; Chmiela, B.

2014-08-01

Superalloys display a strong tendency toward chemical segregation during solidification. Therefore, it is of great importance to develop appropriate techniques for the melting and casting of superalloys. Elements partitioning between the γ and γ' phases in single crystal superalloys have been investigated by several authors using electron probe microanalysis (Hemmersmeier and Feller-Kniepmeier Mater Sci Eng A 248:87-97, 1998; Kearsey et al. Intermetallics 12:903-910, 2004; Kearsey et al. Superalloys 2004, pp 801-810, 2004; D'Souza et al. Mater Sci Eng A 490:258-265, 2008). We examined the effect of the particular stages of standard heat treatment (solution treatment and ageing) applied to CMSX-4 single crystal superalloy on chemical segregation that occurs between dendrites and interdendritic areas. Dendritic structures were observed using a scanning electron microscope. Analyses of the chemical composition were performed using energy dispersive x-ray spectroscopy. The obtained qualitative and quantitative results for the concentrations of elements enabled us to confirm the dendritic segregation in as-cast CMSX-4 superalloy. The concentrations of some refractory elements (tungsten, rhenium) were much greater in dendrites than in interdendritic areas. However, these differences in chemical composition gradually decreased during heat treatment. The results obtained in this study warrant further examination of the diffusion processes of elements during heat treatment of the investigated superalloy, and of the kinetics of diffusion.

Preclinical Pharmacokinetics and Pharmacodynamic Target of SCY-078, a First-in-Class Orally Active Antifungal Glucan Synthesis Inhibitor, in Murine Models of Disseminated Candidiasis.

PubMed

Wring, Stephen A; Randolph, Ryan; Park, SeongHee; Abruzzo, George; Chen, Qing; Flattery, Amy; Garrett, Graig; Peel, Michael; Outcalt, Russell; Powell, Kendall; Trucksis, Michelle; Angulo, David; Borroto-Esoda, Katyna

2017-04-01

SCY-078 (MK-3118) is a novel, semisynthetic derivative of enfumafungin and represents the first compound of the triterpene class of antifungals. SCY-078 exhibits potent inhibition of β-(1,3)-d-glucan synthesis, an essential cell wall component of many pathogenic fungi, including Candida spp. and Aspergillus spp. SCY-078 is currently in phase 2 clinical development for the treatment of invasive fungal diseases. In vitro disposition studies to assess solubility, intestinal permeability, and metabolic stability were predictive of good oral bioavailability. Preclinical pharmacokinetic studies were consistent with once-daily administration to humans. After intravenous delivery, plasma clearance in rodents and dogs was low, representing <15% and <25% of hepatic blood flow, respectively. The terminal elimination-phase half-life was 5.5 to 8.7 h in rodents, and it was ∼9.3 h in dogs. The volume of distribution at steady-state was high (4.7 to 5.3 liters/kg), a finding suggestive of extensive tissue distribution. Exposure of SCY-078 in kidney tissue, a target organ for invasive fungal disease such as candidiasis, exceeded plasma by 20- to 25-fold for the area under the concentration-time curve from 0 h to infinity (AUC 0-∞ ) and C max SCY-078 achieved efficacy endpoints following oral delivery across multiple murine models of disseminated candidiasis. The pharmacokinetic/pharmacodynamic indices C max /MIC and AUC/MIC correlated with outcome. Target therapeutic exposure, expressed as the plasma AUC 0-24 , was comparable across models, with an upper value of 11.2 μg·h/ml (15.4 μM·h); the corresponding mean value for free drug AUC/MIC was ∼0.75. Overall, these results demonstrate that SCY-078 has the oral and intravenous (i.v.) pharmacokinetic properties and potency in murine infection models of disseminated candidiasis to support further investigation as a novel i.v. and oral treatment for invasive fungal diseases. Copyright © 2017 Wring et al.

The 176Lu-176Hf System as a Tool to Date Meteorites and Trace Early Silicate Differentiation - Requirements and Pitfalls

NASA Astrophysics Data System (ADS)

Bast, R.; Scherer, E. E.; Sprung, P.; Mezger, K.; Bischoff, A.

2016-12-01

The long-lived 176Lu-176Hf system is a potentially precise and robust chronometer, but when applied to meteorites, several "isochrons" exhibit excessive scatter and yield dates up to 300 Myr older than the Solar System [1-3]. Samples from different parent bodies produce similar patterns of scatter, whereas different pieces of the same meteorite yield contradictory results [e.g., 4-5]. These observations are difficult to explain by early Solar System irradiation [6-7] or diffusion [8-11] events. Instead, we infer that terrestrial contamination and weathering are more plausible disturbance mechanisms. Similar effects can, however, also be induced during sample handling [12-13]. Precise and accurate Lu-Hf chronology requires fresh, unaltered samples, and contamination must be removed without disturbing the target minerals. We have investigated various fractions of ALM-A, a trachyandesite from the Almahata Sitta meteorite fall. Impure mineral separates and bulk fractions contain terrestrial contamination as evidenced by excess 176Hf, whereas the purest, handpicked grains and selectively digested phosphate minerals yield a 13-point isochron with an age of 4569 ±24 Ma (MSWD = 1.3) using λ176Lu = 1.867 × 10-11 yr-1 [14-16]. The initial 176Hf/177Hf of 0.279796 ±0.000011 agrees well with other estimates of the initial 176Hf/177Hf of the Solar System [17-18] and supports the assumption of initial isotopic homogeneity among rocky planetary bodies with respect to Hf. [1] Blichert-Toft et al. (2002) EPSL 202, 167-181. [2] Bizzarro et al. (2003) Nature 421, 931-933. [3] Bizzarro et al. (2012) G³ 13, 10.1029/2011GC004003. [4] Bast et al. (under review) GCA. [5] Sanborn et al. (2015) GCA 171, 80-99. [6] Albarède et al. (2006) GCA 70, 1261-1270. [7] Thrane et al. (2010) Astrophys J 717, 861-867. [8] Debaille et al. (2011) LPI Contrib, 1639, 9066. [9] Debaille et al. (2013) Min Mag, 77, 957. [10] Debaille et al. (2014) Meteorit Planet Sci, 49, A5238. [11] Bloch et al. (2016) Goldschmidt, A250. [12] Amelin et al. (2016) Goldschmidt, A57. [13] Scherer & Bast (2016) this meeting. [14] Scherer et al. (2001) Science 293, 683-687. [15] Scherer et al. (2003) Meteorit Planet Sci, 38, A136. [16] Söderlund et al. (2004) EPSL 219, 311-324. [17] Bouvier et al. (2008) EPSL 273, 48-57. [18] Iizuka et al. (2015) PNAS 112, 5331-5336.

Mercury's spin-orbit model and signature of C/MR2

NASA Astrophysics Data System (ADS)

Rambaux, N.; Bois, E.

2003-04-01

The upcoming missions, MESSENGER (Solomon etal 2001, Planet. Space Sci 49) and Bepi Colombo (Milani etal 2001, Planet. Space Sci 49) with onboard instrumentation capable of measuring the rotational parameters stimulate the objective to reach an accurate theory of the rotational motion of Mercury. Our work deals with the physical and dynamical causes that induce librations around an equilibrium state defined by the 3:2 spin-orbit resonance of Mercury. In order to integrate the spin-orbit motion of Mercury, we have used our gravitational model of the solar System including the Moon's spin-orbit motion. This model, called SONYR (acronym of Spin-Orbit N-bodY Relativistic model), was previously built by Bois, Journet and Vokrouhlicky in accordance with the requirements of the Lunar Laser Ranging observational accuracy (see for instance a review by Bois 2000, C. R. Acad. Sci. Série IV, or Bois and Vokrouhlický 1995). Using the model, the present study is devoted to the main perturbations acting on the spin-orbit motion of Mercury such as the planetary interactions (and their hierarchy) and the dynamical figure of the planet. The effect of the torque of Venus is 105 times smaller in magnitude than the one due to the Sun. Moreover, the complete rotation of Mercury exhibits two proper frequencies, namely 15.825 and 1089 years, and one secular variation of 271043 years which is due to the nodal precession between the equatorial plane of Mercury and its orbital plane. It is the second synchronism of Mercury mentioned by Beletski in 1986. We have made into evidence that the 3:2 resonance of Mercury is preserved by this second synchronism, which can be understood as a spin-orbit secular resonance. We have shown that the secular resonance variable ψ - Ω librates with a frequency of 1089 years. Our model integration starts with an initial obliquity of 1.65 arcminute (re-evaluate from the Cassini state) and gives an amplitude of libration in longitude of the order of 20 arcseconds, which is in agreement with Balogh and Giamperi (2002, Rep. Prog. Phys. 65). Besides, we have computed in the Hermean librations the impact of the variation of the greatest principal moment of inertia, cm2. The maximal signature on the obliquity is then 1.4 mas (milliarsecond) on the 176 day period, and the one on the libration in longitude is 0.4 mas on the 87.9 day period, resulting from an increase of the cm2 value of 1%. These values have to be understood as upper bounds of such signatures. These two effects permit to contribute to precise the relationship between the cm2 coefficient and the internal structure of Mercury. References : Balog, A., and Giamperi, G., 2002, Rep. Prog. Phys. 65, 529-560. Beletski, V, 1986, "Essais sur le Mouvement des Corps Cosmiques", Mir (ed), Moscou. Bois, E., 2000, C. R. Acad. Sci. Paris, t. 1, Série IV, 809-823. Bois, E., and Vokrouhlický, D., 1995, Astronomy and Astrophysics 300, 559-567. Milani, A., Vokrouhlicky, D., and Bonanno, C., 2001, Planet. Space Sci 49, 1579. Solomon, etal, 2001, Planet. Space Sci 49, 1445.

Gravity Waves in the Atmospheres of Mars and Venus

NASA Astrophysics Data System (ADS)

Tellmann, Silvia; Paetzold, Martin; Häusler, Bernd; Bird, Michael K.; Tyler, G. Leonard; Hinson, David P.; Imamura, Takeshi

2016-10-01

Gravity waves are ubiquitous in all stably stratified planetary atmospheres and play a major role in the redistribution of energy and momentum. Gravity waves can be excited by many different mechanisms, e.g. by airflow over orographic obstacles or by convection in an adjacent layer.Gravity waves on Mars were observed in the lower atmosphere [1,2] but are also expected to play a major role in the cooling of the thermosphere [3] and the polar warming [4]. They might be excited by convection in the daytime boundary layer or by strong winter jets in combination with the pronounced topographic diversity on Mars.On Venus, gravity waves play an important role in the mesosphere above the cloud layer [5] and probably below. Convection in the cloud layer is one of the most important source mechanisms but certain correlations with topography were observed by different experiments [6,7,8].Temperature height profiles from the radio science experiments on Mars Express (MaRS) [9] and Venus Express (VeRa) [10] have the exceptionally high vertical resolution necessary to study small-scale vertical gravity waves, their global distribution, and possible source mechanisms.Atmospheric instabilities, which are clearly identified in the data, can be investigated to gain further insight into possible atmospheric processes contributing to the excitation of gravity waves.[1] Creasey, J. E., et al.,(2006), Geophys. Res. Lett., 33, L01803, doi:10.1029/2005GL024037.[2]Tellmann, S., et al.(2013), J. Geophys. Res. Planets, 118, 306-320, doi:10.1002/jgre.20058.[3]Medvedev, A. S., et al.(2015), J. Geophys. Res. Planets, 120, 913-927. doi:10.1002/2015JE004802.[4] Barnes, J. R. (1990), J. Geophys. Res., 95, B2, 1401-1421.[5] Tellmann, S., et al. (2012), Icarus, 221, 471 - 480.[6] Blamont, J.E. et al., (1986) 231, 1422-1425.[7] Bertaux J.-L., et al. (2016), J. Geophys. Res., Planets, in press.[8] Piccialli, A., et al. (2014), Icarus, 227, 94 - 111.[9] Pätzold, M., et al. (2016), Planet. Space Sci., 127, 44 - 90.[10] Häusler, B. et al., (2006). 1315-1335.

Differences in the Community Built Environment Influence Poor Perceived Health among Persons with Spinal Cord Injury

PubMed Central

Botticello, Amanda L.; Rohrbach, Tanya; Cobbold, Nicolette

2015-01-01

Objectives To assess the association between characteristics of the built environment and differences in perceived health among persons with spinal cord injury (SCI) using objective measures of the local community derived from Geographic Information Systems (GIS) data. Design Secondary analysis of cross-sectional survey data. Setting Community. Participants 503 persons with chronic SCI enrolled in the Spinal Cord Injury Model Systems (SCIMS) database. All cases were residents of New Jersey, completed an interview during the years 2000–2012, had a complete residential address, and were community living at the time of follow-up. Intervention Not applicable. Main Outcome Measure Perceived health. Results Bivariate tests indicated that persons with SCI residing in communities with more (versus less) mixed land use and small (versus large) amounts of open space were more likely to report poor perceived health. No associations were found between perceived health and differences in the residential or destination density of the community. Adjusting for variation in demographic, impairment, quality of life, and community socioeconomic characteristics accounted for the gap in the odds of reporting poor health between persons living in areas with large versus small amounts of open space (OR 0.54; 95% CI 0.28–1.02). However, even after accounting for individual background differences, persons living in communities characterized by more heterogeneous land use were twice as likely to report poor health compared to persons living in less mixed areas (OR 2.14; 95% CI 1.12–4.08). Conclusions Differences in the built characteristics of communities may be important to the long-term health and well-being of persons with SCI who may have greater exposure to the features of their local area due to limited mobility. The results of this study suggest living in a community with more heterogeneous land use was not beneficial to the perceived health of persons with chronic SCI living in New Jersey. Further investigation is needed to assess if the relationships observed in this analysis are influenced by differences in infrastructure and resources across communities. Further research is also needed to investigate the role built environment plays in the long-term health and well-being of persons with SCI in other geographic locales. PMID:25998221

Differences in the Community Built Environment Influence Poor Perceived Health Among Persons With Spinal Cord Injury.

PubMed

Botticello, Amanda L; Rohrbach, Tanya; Cobbold, Nicolette

2015-09-01

To assess the association between characteristics of the built environment and differences in perceived health among persons with spinal cord injury (SCI) using objective measures of the local community derived from Geographic Information Systems data. Secondary analysis of cross-sectional survey data. Community. Persons with chronic SCI enrolled in the Spinal Cord Injury Model Systems database (N=503). All cases were residents of New Jersey, completed an interview during the years 2000 through 2012, had a complete residential address, and were community living at the time of follow-up. Not applicable. Perceived health. Bivariate tests indicated that persons with SCI residing in communities with more (vs less) mixed land use and small (vs large) amounts of open space were more likely to report poor perceived health. No associations were found between perceived health and differences in the residential or destination density of the community. Adjusting for variation in demographic, impairment, quality of life, and community socioeconomic characteristics accounted for the gap in the odds of reporting poor health between persons living in areas with large versus small amounts of open space (odds ratio [OR], 0.54; 95% confidence interval [CI], 0.28-1.02). However, even after accounting for individual background differences, persons living in communities characterized by more heterogeneous land use were twice as likely to report poor health compared with persons living in less mixed areas (OR, 2.14; 95% CI, 1.12-4.08). Differences in the built characteristics of communities may be important to the long-term health and well-being of persons with SCI who may have greater exposure to the features of their local area because of limited mobility. The results of this study suggest living in a community with more heterogeneous land use was not beneficial to the perceived health of persons with chronic SCI living in New Jersey. Further investigation is needed to assess if the relationships observed in this analysis are influenced by differences in infrastructure and resources across communities. Further research is also needed to investigate the role built environment plays in the long-term health and well-being of persons with SCI in other geographic locales. Copyright © 2015 American Congress of Rehabilitation Medicine. Published by Elsevier Inc. All rights reserved.

Aerosol volatility in a boreal forest environment

NASA Astrophysics Data System (ADS)

Häkkinen, S. A. K.; ńijälä, M.; Lehtipalo, K.; Junninen, H.; Virkkula, A.; Worsnop, D. R.; Kulmala, M.; Petäjä, T.; Riipinen, I.

2012-04-01

Climate and health effects of atmospheric aerosols are determined by their properties such as their chemical composition. Aerosol chemical composition can be studied indirectly by measuring volatility of aerosol particles. The volatility of submicron aerosol particles (20-500 nm) was studied in a boreal forest site at SMEAR II (Station for Measuring Ecosystem-Atmosphere Relations II) station (Vesala et al., 1998) in Hyytiälä, Finland, during 01/2008-05/2010. The instrument used for the measurements was VDMPS (Volatility Differential Mobility Particle Sizer), which consists of two separate instruments: DMPS (Differential Mobility Particle Sizer, Aalto et al., 2001) and TD (Thermodenuder, Wehner et al., 2002). Aerosol evaporation was examined by heating the aerosol and comparing the total aerosol mass before and after heating. In the VDMPS system ambient aerosol sample was heated up to temperatures ranging from 80 °C to 280 °C. The higher the heating temperature was the more aerosol material was evaporated. There was a non-volatile residual present in aerosol particles when heated up to 280 °C. This residual explained (20±8)% of the total aerosol mass. Aerosol non-volatile mass fraction was highest during winter and smallest during summer months. The role of black carbon in the observed non-volatile residual was determined. Black carbon explained 40 to 90% of the non-volatile mass. Especially during colder seasons noticeable amount of non-volatile material, something else than black carbon, was observed. According to Kalberer et al. (2004) some atmospheric organic species can form polymers that have high evaporation temperatures. Also low-volatile organic salts may contribute to the non-volatile aerosol (Smith et al., 2010). Aerosol mass composition measured directly with AMS (Aerosol Mass Spectrometer, Jayne et al., 2000) was analyzed in order to examine the properties of the non-volatile material (other than black carbon). The AMS measurements were performed during spring and autumn 2008. Results from the aerosol mass spectrometry indicate that the non-volatile residual consists of nitrate and organic compounds, especially during autumn. These compounds may be low-volatile organic nitrates or salts. During winter and spring the non-volatile core (black carbon removed) correlated markedly with carbon monoxide, which is a tracer of anthropogenic emissions. Due to this, the non-volatile residual may also contain other pollutants in addition to black carbon. Thus, it seems that the amount of different compounds in submicron aerosol particles varies with season and as a result the chemical composition of the non-volatile residual changes within a year. This work was supported by University of Helsinki three-year research grant No 490082 and Maj and Tor Nessling Foundation grant No 2010143. Aalto et al., (2001). Physical characterization of aerosol particles during nucleation events. Tellus B, 53, 344-358. Jayne, et al., (2000). Development of an aerosol mass spectrometer for size and composition analysis of submicron particles. Aerosol Sci. Technol., 33(1-2), 49-70. Kalberer et al., (2004). Identification of Polymers as Major Components of Atmospheric Organic Aerosols. Science, 303, 1659-1662. Smith et al., (2010). Observations of aminium salts in atmospheric nanoparticles and possible climatic implications. P. Natl. Acad. Sci., 107(15). Vesala et al., (1998). Long-term field measurements of atmosphere-surface interactions in boreal forest combining forest ecology, micrometeorology, aerosol physics and atmospheric chemistry. Trends Heat, Mass Mom. Trans., 4, 17-35. Wehner et al., (2002). Design and calibration of a thermodenuder with an improved heating unit to measure the size-dependent volatile fraction of aerosol particles. J. Aerosol Sci., 33, 1087-1093.

Shock Prevention

NASA Technical Reports Server (NTRS)

1978-01-01

The electrician pictured is installing a General Electric Ground Fault Interrupter (GFI), a device which provides protection against electrical shock in the home or in industrial facilities. Shocks due to defective wiring in home appliances or other electrical equipment can cause severe burns, even death. As a result, the National Electrical Code now requires GFIs in all new homes constructed. This particular type of GFI employs a sensing element which derives from technology acquired in space projects by SCI Systems, Inc., Huntsville, Alabama, producer of sensors for GE and other manufacturers of GFI equipment. The sensor is based on the company's experience in developing miniaturized circuitry for space telemetry and other spacecraft electrical systems; this experience enabled SCI to package interruptor circuitry in the extremely limited space available and to produce sensory devices at practicable cost. The tiny sensor measures the strength of the electrical current and detects current differentials that indicate a fault in the functioning of an electrical system. The sensing element then triggers a signal to a disconnect mechanism in the GFI, which cuts off the current in the faulty circuit.

An Impact Origin for Surface Minerals on Ceres

NASA Astrophysics Data System (ADS)

Zolotov, M. Y.

2013-12-01

The dwarf planet Ceres is the largest body in the main asteroid belt with a hydrated dark rocky surface and an uncertain internal structure [1,2]. Spectra of Ceres in the near- and mid-infrared ranges show that surface materials may not contain abundant serpentine, saponite, sulfates, olivine, pyroxenes, and organic matter [2,3], which are common in carbonaceous chondrites. However, brucite, Mg carbonates, cronstedtite, and magnetite could be abundant and indicate aqueous processes [2,3]. The formation of abundant brucite, carbonates, and cronstedtite requires open-system low-temperature conditions characterized by elevated water/rock ratios and low fugacities of hydrogen and carbon dioxide. The observed mineralogy is more consistent with a near-surface origin than with a formation within Ceres or on planetesimals. The instability of aqueous solutions at the surface of Ceres implies mineral deposition during transient events of fluidal activity. But a warming of near-surface rocks by thermal processes in the interior requires dehydration of rocks, which is not consistent with the low density of Ceres. The lack of low-solubility sulfates in surface materials does not indicate percolation of interior fluids. Carbonate-bearing fluids may not percolate to the cold surface, especially if Ceres had undergone water-rock differentiation [1,4]. The lack of serpentine in surface materials does not indicate a formation of brucite through aqueous alteration of olivine-rich rocks. Though, the observed minerals could form in impact collisions of ice-rich targets and/or impactors. OH-bearing phases may condense from water-rich impact plumes [5]. Brucite and Mg carbonates could form through hydrolysis and carbonation of condensed MgO formed through evaporation of silicates. Apparently abundant carbonates may indicate an ample oxidation of organics. Ferric iron in magnetite and cronstedtite agrees with water-rich and oxidizing impact settings [5]. Turbulent and disequilibrium environments in impact plumes and surges could have led to deposition of minerals which typically do not form together (e.g., brucite and cronstedtite). Aqueous minerals could have formed in impact clouds, crater outflows, transient ice-covered crater lakes, and related hydrothermal systems. The observed clay-sized and spatially homogeneous surface materials [2] could be gravitationally sorted deposits of impact clouds and surges. The surface materials could have formed through impacts on an icy shell of a differentiated Ceres during the Late Heavy Bombardment (LHB) in the inner solar system, which affected may other asteroids [6]. However, mineral-forming processes during collisions of an undifferentiated and hydrated Ceres with water-rich bodies during LHB remain a possibility. A detection of fluidized crater outflows together with topography and composition of surface materials with Dawn will test this hypothesis. Refs: [1] McCord, T.B. et al. (2011) Space Sci. Rev. 163, 63-76. [2] Rivkin, A.S. et al. (2011) Space Sci. Rev. 101, 1-22. [3] Milliken, R.E., and Rivkin, A.S. (2009) Nature Geoscience 2, 258-261. [4] Castillo-Rogez, J.C., and McCord, T.B. (2010) Icarus 205, 443-459. [5] Gerasimov, M.V. et al. (2002) Deep-Sea Res. II 49, 995-1009. [6] Marchi, S. et al. (2013) Nature Geoscience, 6, 303-307.

Bank Terminals

NASA Technical Reports Server (NTRS)

1978-01-01

In the photo, employees of the UAB Bank, Knoxville, Tennessee, are using Teller Transaction Terminals manufactured by SCI Systems, Inc., Huntsville, Alabama, an electronics firm which has worked on a number of space projects under contract with NASA. The terminals are part of an advanced, computerized financial transaction system that offers high efficiency in bank operations. The key to the system's efficiency is a "multiplexing" technique developed for NASA's Space Shuttle. Multiplexing is simultaneous transmission of large amounts of data over a single transmission link at very high rates of speed. In the banking application, a small multiplex "data bus" interconnects all the terminals and a central computer which stores information on clients' accounts. The data bus replaces the maze-of wiring that would be needed to connect each terminal separately and it affords greater speed in recording transactions. The SCI system offers banks real-time data management through constant updating of the central computer. For example, a check is immediately cancelled at the teller's terminal and the computer is simultaneously advised of the transaction; under other methods, the check would be cancelled and the transaction recorded at the close of business. Teller checkout at the end of the day, conventionally a time-consuming matter of processing paper, can be accomplished in minutes by calling up a summary of the day's transactions. SCI manufactures other types of terminals for use in the system, such as an administrative terminal that provides an immediate printout of a client's account, and another for printing and recording savings account deposits and withdrawals. SCI systems have been installed in several banks in Tennessee, Arizona, and Oregon and additional installations are scheduled this year.

Understanding helicon plasmas

DOE Office of Scientific and Technical Information (OSTI.GOV)

Tarey, R. D.; Sahu, B. B.; Ganguli, A.

2012-07-15

This paper presents a comprehensive overview of work on the helicon plasmas and also discusses various aspects of RF power deposition in such plasmas. Some of the work presented here is a review of earlier work on theoretical [A. Ganguli et al., Phys. Plasmas 14, 113503 (2007)] and experimental [A. Ganguli et al., Plasma Sources Sci. Technol. 20(1), 015021 (2011)] investigations on helicon plasmas in a conducting cylindrical waveguide for m = -1 mode. This work also presents an approach to investigate the mechanisms by which the helicon and associated Trivelpiece-Gould (TG) waves are responsible for RF power deposition inmore » Helicon discharges. Experiment design adopts the recent theory of damping and absorption of Helicon modes in conducting waveguides [A. Ganguli et al., Phys. Plasmas 14, 113503 (2007)]. The effort has also been made to detect the warm electrons, which are necessary for ionization, because Helicon discharges are of high density, low T{sub e} discharges and the tail of the bulk electron population may not have sufficient high-energy electrons. Experimental set up also comprises of the mirror magnetic field. Measurements using RF compensated Langmuir probes [A. Ganguli et al., Plasma Sources Sci. Technol. 17, 015003 (2008)], B-dot probe and computations based on the theory shows that the warm electrons at low pressure (0.2-0.3 mTorr) Helicon discharges, are because of the Landau damping of TG waves. In collisional environment, at a pressure Almost-Equal-To 10 mTorr, these high-energy electrons are due to the acceleration of bulk electrons from the neighboring regions across steep potential gradients possibly by the formation of double layers.« less

Energetic Neutral Atom Imaging of the Lunar Poles and Night-Side

NASA Astrophysics Data System (ADS)

Vorburger, Audrey; Wurz, Peter; Barabash, Stas; Wieser, Martin; Futaana, Yoshifumi; Bhardwaj, Anil; Dhanya, Mb; Asamura, Kazushi

2016-04-01

So far all reported scientific results derived from measurements of the Chandrayaan-1 Energetic Neutral Analyzer (CENA) on board the Indian lunar mission Chandrayaan-1 focused on the sun-lit part of the Moon. Here, for the first time, we present the analysis of the Moon - solar wind interaction in Energetic Neutral Atoms (ENAs) from measurements over the poles and the night-side of the Moon. The Moon, not being protected by a global magnetic field or an atmosphere, is constantly bombarded by solar wind ions. Until recently, it was tacitly assumed that the solar wind ions that impinge onto the lunar surface are almost completely absorbed ( < 1% reflection) by the lunar surface (e.g. Crider and Vondrak [Adv. Space Res., 2002]; Feldman et al. [J. Geophys. Res., 2000]). However, recent observations conducted by the two ENA sensors of NASA's Interstellar Boundary Explorer and by Chandrayaan-1/CENA showed an average global energetic neutral atom (ENA) albedo of 10% - 20% (e.g. McComas et al. [Geophys. Res. Lett., 2009], Wieser et al. [Planet. Space Sci., 2009], Vorburger et al. [J. Geophys. Res., 2013]). In the past 6 years, several studies have closely investigated this solar wind - lunar surface interaction from various viewpoints. The main findings of these studies include (1) the dependency of the hydrogen reflection ratio on the local crustal magnetic fields (e.g., Wieser et al. [Geophys. Res. Lett. ,2010] and Vorburger et al. [J. Geophys. Res., 2012]), (2) the determination of the energy spectra of backscattered neutralized solar wind protons (Futaana et al. [J. Geophys. Res., 2012]) (3) the use of the spectra shape to remotely define an electric potential above a lunar magnetic anomaly (Futaana et al. [Geophys. Res. Lett., 2012]), (4) the favouring of backscattering over forward-scattering of impinging solar wind hydrogen particles (Vorburger et al. [Geophys. Res. Lett., 2011]), (5) the first-ever measurements of sputtered lunar oxygen (Vorburger et al. [J. Geophys. Res., 2012]), (6) the first-ever observation of backscattered solar wind helium (Vorburger et al. [J. Geophys. Res., 2012]), and (7) the determination of the scattering properties of backscattered solar wind hydrogen measured when the Moon transversed Earth's magneto-sheath (Lue et al. [J. Geophys. Res., 2016]). All findings above are based on measurements from the sun-lit side of the Moon's surface, where solar wind particles can impinge freely onto the lunar surface. On the night-side, in contrast, a large scale wake structure is formed as a result of the high absorption of solar wind plasma on the lunar day-side. Very recent ion measurements of Chandrayaan-1's Solar Wind Monitor (SWIM) have revealed the presence of protons in the near-lunar wake, though (Dhanya et al., [Icarus 2016 (submitted)]). The presence of protons in the near lunar wake implies that there is also some sort of solar wind - lunar surface interaction on the lunar night-side. A complete analysis of this interaction will be presented herein.

FE Furukawa poses for a photo during VolSci Session

NASA Image and Video Library

2011-06-25

ISS028-E-009727 (25 June 2011) --- Japan Aerospace Exploration Agency astronaut Satoshi Furukawa, Expedition 28 flight engineer, is pictured near the Cell Biology Experiment Facility (CBEF) in the Kibo laboratory of the International Space Station.

In situ analysis of Mars soil sample with the sam gcms instrumentation onboard Curiosity : interpretation and comparison of measurements done at Rocknest and Yelloknife bay sites

NASA Astrophysics Data System (ADS)

Szopa, Cyril; Coll, Patrice; Cabane, Michel; Coscia, David; Buch, Arnaud; Francois, Pascaline; Millan, Maeva; Teinturier, Sammy; Navarro-Gonzales, Rafael; Glavin, Daniel; Freissinet, Caro; Steele, Andrew; Eigenbrode, Jen; Mahaffy, Paul

2014-05-01

The characterisation of the chemical and mineralogical composition of regolith samples collected with the Curiosity rover is a primary objective of the SAM experiment. These data should provide essential clues on the past habitability of Gale crater. Amongst the SAM suite of instruments [1], SAM-GC (Gas Chromatograph) is devoted to identify and quantify volatiles evolved from the thermal (heating up to about 900°C)/chemical (derivatization procedure) treatment of any soil sample collected by the Curiosity rover. With the aim to search for potential organic molecules outgassed from the samples, a SAM-GC analytical channel composed of thermal-desorption injector and a MXT-CLP chromatographic column was chosen to achieve all the measurements done up today, as it was designed for the separation of a wide range of volatile organic molecules. Three solid samples have been analyzed with GCMS, one sand sample collected at the Rocknest site, and two rock samples (John Klein and Cumberland respectively) collected at the Yellowknife Bay site using the Curiosity driller. All the measurements were successful and they produced complex chromatograms with both detectors used for SAM GC, i.e. a thermal conductivity detector and the SAM quandrupole mass spectrometer. Their interpretation already revealed the presence of an oxychlorine phase present in the sample which is at the origin of chlorohydrocarbons clearly identified [2] but this represents only a fraction of the GCMS signal recorded [3,4]. This work presents a systematic comparison of the GCMS measurements done for the different samples collected, supported by reference data obtained in laboratory with different spare models of the gas chromatograph, with the aim to bring new elements of interpretation of the SAM measurements. References: [1] Mahaffy, P. et al. (2012) Space Sci Rev, 170, 401-478. [2] Glavin, D. et al. (2013), JGR. [3] Leshin L. et al. (2013), Science, [4] Ming D. et al. (2013), Science, 32, 64-67. Acknowledgements: SAM-GC team acknowledges support from the French Space Agency (CNES), French National Programme of Planetology (PNP), National French Council (CNRS), Pierre Simon Laplace Institute, Institut Universitaire de France (IUF) and ESEP Labex.

High Resolution Continuous Flow Analysis System for Polar Ice Cores

NASA Astrophysics Data System (ADS)

Dallmayr, Remi; Azuma, Kumiko; Yamada, Hironobu; Kjær, Helle Astrid; Vallelonga, Paul; Azuma, Nobuhiko; Takata, Morimasa

2014-05-01

In the last decades, Continuous Flow Analysis (CFA) technology for ice core analyses has been developed to reconstruct the past changes of the climate system 1), 2). Compared with traditional analyses of discrete samples, a CFA system offers much faster and higher depth resolution analyses. It also generates a decontaminated sample stream without time-consuming sample processing procedure by using the inner area of an ice-core sample.. The CFA system that we have been developing is currently able to continuously measure stable water isotopes 3) and electrolytic conductivity, as well as to collect discrete samples for the both inner and outer areas with variable depth resolutions. Chemistry analyses4) and methane-gas analysis 5) are planned to be added using the continuous water stream system 5). In order to optimize the resolution of the current system with minimal sample volumes necessary for different analyses, our CFA system typically melts an ice core at 1.6 cm/min. Instead of using a wire position encoder with typical 1mm positioning resolution 6), we decided to use a high-accuracy CCD Laser displacement sensor (LKG-G505, Keyence). At the 1.6 cm/min melt rate, the positioning resolution was increased to 0.27mm. Also, the mixing volume that occurs in our open split debubbler is regulated using its weight. The overflow pumping rate is smoothly PID controlled to maintain the weight as low as possible, while keeping a safety buffer of water to avoid air bubbles downstream. To evaluate the system's depth-resolution, we will present the preliminary data of electrolytic conductivity obtained by melting 12 bags of the North Greenland Eemian Ice Drilling (NEEM) ice core. The samples correspond to different climate intervals (Greenland Stadial 21, 22, Greenland Stadial 5, Greenland Interstadial 5, Greenland Interstadial 7, Greenland Stadial 8). We will present results for the Greenland Stadial -8, whose depths and ages are between 1723.7 and 1724.8 meters, and 35.520 to 35.636 kyr b2k 7), respectively. The results show the conductivity measured upstream and downstream of the debubbler. We will calculate the depth resolution of our system and compare it with earlier studies. 1) Bigler at al, "Optimization of High-Resolution Continuous Flow Analysis For Transient Climate Signals in Ice Cores". Environ. Sci. Technol. 2011, 45, 4483-4489 2) Kaufmann et al, "An Improved Continuous Flow Analysis System for High Resolution Field Measurements on Ice Cores". Environmental Environ. Sci. Technol. 2008, 42, 8044-8050 3) Gkinis, V., T. J. Popp, S. J. Johnsen and T, Blunier, 2010: A continuous stream flash evaporator for the calibration of an IR cavity ring down spectrometer for the isotopic analysis of water. Isotopes in Environmental and Health Studies, 46(4), 463-475. 4) McConnell et al, "Continuous ice-core chemical analyses using inductively coupled plasma mass spectrometry. Environ. Sci. Technol. 2002, 36, 7-11 5) Rhodes et al, "Continuous methane measurements from a late Holocene Greenland ice core : Atmospheric and in-situ signals" Earth and Planetary Science Letters. 2013, 368, 9-19 6) Breton et al, "Quantifying Signal Dispersion in a Hybrid Ice Core Melting System". Environ. Sci. Technol. 2012, 46, 11922-11928 7) Rasmussen et al, " A first chronology for the NEEM ice core". Climate of the Past. 2013, 9, 2967--3013

Understanding the limits of Marxist approaches to sociocultural studies of science education

NASA Astrophysics Data System (ADS)

Lima Junior, Paulo; Ostermann, Fernanda; Rezende, Flavia

2014-09-01

In the first three sections of this paper we comment on some of the ideas developed in the forum papers, pointing out possible misunderstandings and constructing new explanations that clarify arguments we made in the original article. In the last section we expand the discussion raised in the original paper, elaborating on the limits of the use of Marxist approaches to sociocultural studies of science education. Following insights suggested by Loxley et al. (Cult Stud Sci Edu. doi: 10.1007/s11422-013-9554-z, 2013) and detailed by Zuss (Cult Stud Sci Edu, 2014) on the commodification of knowledge, we sketch an analysis of how knowledge is transformed into capital to understand why contemporary scholars are likely to be engaged in a relation of production that resembles capitalist exploitation.

Characteristic Times of Gradual Solar Energetic Particle Events and Their Dependence on Associated Coronal Mass Ejection Properties

DTIC Science & Technology

2005-08-01

differences, including longer event durations for SEPs from quasi- Yago & Kamide (2003) have shown that the lognormal plot is parallel shocks due to the longer...Urpo, S. 1999, A&A, 348, 271 ApJ, 598, 1392 Klein, K.-L., & Trottet, G. 2001, Space Sci. Rev., 95, 215 Yago , K., & Kamide, Y. 2003, Space Weather, 1

Defense AT and L. Volume 43, Number 1

DTIC Science & Technology

2014-02-01

community on the strategic direction of future space system acquisitions. Should we continue and/or improve aggregated space systems over time or move...desirable. Schedulers must have a firm command of project manage- ment theory and practice and possess leadership and communication skills. Scorecard...idea was recommended by the Defense Sci- ence Board’s Munitions System Reliability report. In the future, such systems conceivably could communicate

Gravity Waves in the Atmosphere of Mars as seen by the Radio Science Experiment MaRS on Mars Express

NASA Astrophysics Data System (ADS)

Tellmann, S.; Paetzold, M.; Häusler, B.; Bird, M. K.; Tyler, G. L.; Hinson, D. P.

2016-12-01

Gravity waves are atmospheric waves whose restoring force is the buoyancy. They are known to play an essential role in the redistribution of energy, momentum and atmospheric constituents in all stably stratified planetary atmospheres. Possible excitation mechanisms comprise convection in an adjacent atmospheric layer, other atmospheric instabilities like wind shear instabilities, or air flow over orographic obstacles especially in combination with the strong winter jets on Mars. Gravity waves on Mars were observed in the lower atmosphere [1,2] but are also expected to play a major role in the cooling of the thermosphere [3] and the polar warming [4]. A fundamental understanding of the possible source mechanisms is required to reveal the influence of small scale gravity waves on the global atmospheric circulation. Radio occultation profiles from the MaRS experiment on Mars Express [5] with their exceptionally high vertical resolution can be used to study small-scale vertical gravity waves and their global distribution in the lower atmosphere from the planetary boundary layer up to 40 km altitude. Atmospheric instabilities, which are clearly identified in the data, are used to gain further insight into possible atmospheric processes contributing to the excitation of gravity waves. [1] Creasey, J. E., et al.,(2006), Geophys. Res. Lett., 33, L01803, doi:10.1029/2005GL024037. [2]Tellmann, S., et al.(2013), J. Geophys. Res. Planets, 118, 306-320, doi:10.1002/jgre.20058. [3]Medvedev, A. S., et al.(2015), J. Geophys. Res. Planets, 120, 913-927. doi:10.1002/2015JE004802.[4] Barnes, J. R. (1990), J. Geophys. Res., 95, B2, 1401-1421. [5] Pätzold, M., et al. (2016), Planet. Space Sci., 127, 44 - 90.

Water vapor in Titan's stratosphere from Cassini CIRS far-infrared spectra

NASA Astrophysics Data System (ADS)

Cottini, V.; Nixon, C. A.; Jennings, D. E.; Anderson, C. M.; Gorius, N.; Bjoraker, G. L.; Coustenis, A.; Teanby, N. A.; Achterberg, R. K.; Bézard, B.; de Kok, R.; Lellouch, E.; Irwin, P. G. J.; Flasar, F. M.; Bampasidis, G.

2012-08-01

Here we report the measurement of water vapor in Titan's stratosphere using the Cassini Composite Infrared Spectrometer (CIRS, Flasar, F.M. et al. [2004]. Space Sci. Rev. 115, 169-297). CIRS senses water emissions in the far infrared spectral region near 50 μm, which we have modeled using two independent radiative transfer codes (NEMESIS (Irwin, P.G.J. et al. [2008]. J. Quant. Spectrosc. Radiat. Trans. 109, 1136-1150) and ART (Coustenis, A. et al. [2007]. Icarus 189, 35-62; Coustenis, A. et al. [2010]. Icarus 207, 461-476). From the analysis of nadir spectra we have derived a mixing ratio of 0.14 ± 0.05 ppb at an altitude of 97 km, which corresponds to an integrated (from 0 to 600 km) surface normalized column abundance of 3.7 ± 1.3 × 1014 molecules/cm2. In the latitude range 80°S to 30°N we see no evidence for latitudinal variations in these abundances within the error bars. Using limb observations, we obtained mixing ratios of 0.13 ± 0.04 ppb at an altitude of 115 km and 0.45 ± 0.15 ppb at an altitude of 230 km, confirming that the water abundance has a positive vertical gradient as predicted by photochemical models (e.g. Lara, L.M., Lellouch, F., Lopez-Moreno, J.J., Rodrigo, R. [1996]. J. Geophys. Res. 101(23), 261; Wilson, E.H., Atreya, S.K. [2004]. J. Geophys. Res. 109, E6; Hörst, S.M., Vuitton, V., Yelle, R.V. [2008]. J. Geophys. Res., 113, E10). We have also fitted our data using scaling factors of ˜0.1-0.6 to these photochemical model profiles, indicating that the models over-predict the water abundance in Titan's lower stratosphere.

Natural time analysis and Tsallis non-additive entropy statistical mechanics.

NASA Astrophysics Data System (ADS)

Sarlis, N. V.; Skordas, E. S.; Varotsos, P.

2016-12-01

Upon analyzing the seismic data in natural time and employing a sliding natural time window comprising a number of events that would occur in a few months, it has been recently uncovered[1] that a precursory Seismic Electric Signals activity[2] initiates almost simultaneously with the appearance of a minimum in the fluctuations of the order parameter of seismicity [3]. Such minima have been ascertained [4] during periods of the magnitude time series exhibiting long range correlations [5] a few months before all earthquakes of magnitude 7.6 or larger that occurred in the entire Japanese area from 1 January 1984 to 11 March 2011 (the day of the M9 Tohoku-Oki earthquake). Before and after these minima, characteristic changes of the temporal correlations between earthquake magnitudes are observed which cannot be captured by Tsallis non-additive entropy statistical mechanics in the frame of which it has been suggested that kappa distributions arise [6]. Here, we extend the study concerning the existence of such minima in a large area that includes Aegean Sea and its surrounding area which exhibits in general seismo-tectonics [7] different than that of the entire Japanese area. References P. A. Varotsos et al., Tectonophysics, 589 (2013) 116. P. Varotsos and M. Lazaridou, Tectonophysics 188 (1991) 321. P.A. Varotsos et al., Phys Rev E 72 (2005) 041103. N. V. Sarlis et al., Proc Natl Acad Sci USA 110 (2013) 13734. P. A. Varotsos, N. V. Sarlis, and E. S. Skordas, J Geophys Res Space Physics 119 (2014), 9192, doi: 10.1002/2014JA0205800. G. Livadiotis, and D. J. McComas, J Geophys Res 114 (2009) A11105, doi:10.1029/2009JA014352. S. Uyeda et al., Tectonophysics, 304 (1999) 41.

Influence of homogeneity of student characteristics in a group-based social competence intervention.

PubMed

Stichter, Janine P; Herzog, Melissa J; Malugen, Emily; Schoemann, Alexander M

2018-06-18

Although some literature reviews cited mixed results for group-based social competence interventions in schools, existing descriptions of intervention efficacy often lack attention on important factors that may moderate differential response. Some studies suggest that individual characteristics such as diagnosis (i.e., specific deficit clusters) or behavioral profiles may be important social outcome moderators. Given the interactive nature of group-based interventions, understanding how individual characteristics combine to influence outcomes for the group as a whole is an important next step. By using a multisite cluster randomized control trial (n = 274), the current study explores the impact that varying student characteristics have on outcomes of the Social Competence Intervention for Adolescents (SCI-A; Stichter, Herzog, Owens, & Malugen, 2016; Stichter et al., 2010) compared to outcomes of business-as-usual (BAU) practices. Researchers hypothesized that (a) SCI-A would be more effective than BAU in improving ratings of students' social functioning when students within groups were more similar to each other on relevant diagnostic and behavioral indicators, and (b) that within SCI-A only, more versus less homogenous groups would demonstrate greater social outcome gains. Results offer some support for these hypotheses: SCI-A was more effective in improving social communication and motivation when groups were diagnostically similar (ds > 0.55). Considering changes in social awareness and communication, SCI-A was more effective when groups were heterogeneous on socially competent behavior (ds > 1.32) and less effective when groups were heterogeneous on antisocial behavior (ds > 1.00). The authors discuss the implications and importance of research exploring factors such as group composition that may moderate intervention response in applied settings. (PsycINFO Database Record (c) 2018 APA, all rights reserved).

Ceres: Evolution and Present State

NASA Astrophysics Data System (ADS)

Castillo-Rogez, J.; McCord, T.

2007-08-01

Introduction:We consider Ceres as a prototype for planetary evolution [1]. From thermal modeling by McCord and Sotin [2, 3, 4], Ceres was inferred to have differentiated into a rocky core of hydrated silicates, and an icy outer shell. Thomas et al. [5] confirmed such a model from direct observation of Ceres's shape from Hubble Space Telescope observations, and pervious occultation measurements. McCord and Sotin [4] also suggest that Ceres could have preserved a deep ocean, especially if ammonia or some other ice melting point depressant, such as salts, was incorporated during accretion. We continue to develop thermal modeling of Ceres, using increasingly sophisticated models and new observational information in order to match the observed shape. . In particular, we investigate the evolution of the core. Approach: Our models require the following initial input: initial planetesimal temperature (after [6]); composition; time of formation with respect to Calcium-Aluminum Inclusions (CAIs); and an internal heat profile after initial accretion. Modeling begins with a porous Ceres (after [7, 8]). The rock phase has the composition of an ordinary chondrite (after [9]). Short-lived radiogenic isotopes, including 26Al and 60Fe, have initial concentrations as measured by [10, 11]. Conductive thermal evolution is computed for one-dimensional models following the approach of [4] and [12]. The silicate core evolves through hydration, then dehydration and melting stages. Currently, hydrothermal cooling is not included in our algorithm. Model Results: Conditions were present for full differentiation of Ceres if accretion time t0-CAIs was less than 7 My and/or if ammonia was accreted. For times of formation t0-CAIs shorter than 2 My, the boiling point of water was reached within a few My after accretion, and may have led to major water loss.Under these conditions, hydrothermal activity was inevitable, and might still be taking place inside Ceres. Whether a deep ocean is still present within Ceres or not depends on the initial conditions, especially the presence of ammonia. The core follows very different evolutionary paths, given the range of input values. Core evolution is most strongly affected by the time of accretion, with respect to inclusion of CAIs. With the inclusion of short-lived radioisotopes, pressure and temperature conditions in the core can lead to dehydration of the silicate phase [13], and layering of the core. An outer layer consisting of hydrated silicates, and a deep core consisting of dry silicate is the result, due to the equation of state of hydrated silicates. Explosive volcanism is expected to occur [14]. Conditions can even lead to partial differentiation of a metallic core.It is these model runs, resulting in the differentiation of Ceres's core into an outer hydrated layer, dehydrated inner layer and a tiny metallic center, that also produce the observed shape. Acknowledgement: This work was supported in part by the NASA Dawn Discovery Program under contract to the Space Science Institute by the UCLA and funded by JPL/NASA. Part of this work was performed at the Jet Propulsion Laboratory - California Institute of Technology under contract to NASA. References: [1] McCord T. B. et al. 2006. Eos 87(10). [2] McCord, T. B., Sotin, C. 2003. American Astronomical Society, DPS meeting #35, #34.17; Bull. Amer. Astron. Soc. 35, 979. [3] McCord, T., Sotin, C. 2004. 35th COSPAR Scientific Assembly. Held 18 - 25 July 2004, in Paris, France., 1148. [4] McCord, T.B., C. Sotin 2005. J. Geophys. Res., 110, E05009, doi: 10.1029/2004JE002244. 1-14. [5] Thomas, P. C., et al. 2005. Nature 437, doi: 10.1038/nature03938, 224-226. [6] Mousis O. and Alibert Y. (2005) MNRAS, 358, 188-192. [7] Leliwa-Kopystynski, J., Kossacki, K. J. 1995. Planet. Space Sci. 43, 851-861. [8] Leliwa-Kopystynski, J., Kossacki, K. J. 2000. Planet. Space Sci. 48, 727-745. [9] Wasson, J. T., Kalleymen, G. W. 1988. Phil. Trans. Roy. Soc. London A 325, 535. [10] Wasserburg, G. J., Papanastassiou, D. A. 1982. in Essays in Nuclear Astrophysics, ed. C.A. Barnes, D.D. Clayton, & D.N. Schramm (New York: Cambridge Univ. Press), 77. [11] Tachibana, S., et al. 2006. Astroph. J., 639, L87-L90, doi: 10.1086/503201. [12] Castillo et al. Submitted to Icarus. [13] Ellis D. E., Wyllie P. J. 1979. Am. Miner. 64, 41-48. [14] Wilson L. et al. (1999) MPS, 34, 541-557.

Voxel inversion of airborne electromagnetic data for improved model integration

NASA Astrophysics Data System (ADS)

Fiandaca, Gianluca; Auken, Esben; Kirkegaard, Casper; Vest Christiansen, Anders

2014-05-01

Inversion of electromagnetic data has migrated from single site interpretations to inversions including entire surveys using spatial constraints to obtain geologically reasonable results. Though, the model space is usually linked to the actual observation points. For airborne electromagnetic (AEM) surveys the spatial discretization of the model space reflects the flight lines. On the contrary, geological and groundwater models most often refer to a regular voxel grid, not correlated to the geophysical model space, and the geophysical information has to be relocated for integration in (hydro)geological models. We have developed a new geophysical inversion algorithm working directly in a voxel grid disconnected from the actual measuring points, which then allows for informing directly geological/hydrogeological models. The new voxel model space defines the soil properties (like resistivity) on a set of nodes, and the distribution of the soil properties is computed everywhere by means of an interpolation function (e.g. inverse distance or kriging). Given this definition of the voxel model space, the 1D forward responses of the AEM data are computed as follows: 1) a 1D model subdivision, in terms of model thicknesses, is defined for each 1D data set, creating "virtual" layers. 2) the "virtual" 1D models at the sounding positions are finalized by interpolating the soil properties (the resistivity) in the center of the "virtual" layers. 3) the forward response is computed in 1D for each "virtual" model. We tested the new inversion scheme on an AEM survey carried out with the SkyTEM system close to Odder, in Denmark. The survey comprises 106054 dual mode AEM soundings, and covers an area of approximately 13 km X 16 km. The voxel inversion was carried out on a structured grid of 260 X 325 X 29 xyz nodes (50 m xy spacing), for a total of 2450500 inversion parameters. A classical spatially constrained inversion (SCI) was carried out on the same data set, using 106054 spatially constrained 1D models with 29 layers. For comparison, the SCI inversion models have been gridded on the same grid of the voxel inversion. The new voxel inversion and the classic SCI give similar data fit and inversion models. The voxel inversion decouples the geophysical model from the position of acquired data, and at the same time fits the data as well as the classic SCI inversion. Compared to the classic approach, the voxel inversion is better suited for informing directly (hydro)geological models and for sequential/Joint/Coupled (hydro)geological inversion. We believe that this new approach will facilitate the integration of geophysics, geology and hydrology for improved groundwater and environmental management.

Soft x-ray microscopy and extreme ultraviolet lithography: Imaging in the 20-50 nm regime (abstract) (invited)

NASA Astrophysics Data System (ADS)

Attwood, David

2002-03-01

Advances in short wavelength optics, covering the range from 1 to 14 nm, are providing new results and new opportunities. Zone plate lenses [E. Anderson et al., J. Vac. Sci. Techno. B 18, 2970 (2000)] for soft x-ray microscopy [G. Denbeaux, Rev. Sci. Instrum. (these proceedings); W. Chao, Proc. SPIE 4146, 171 (2000)] are now made to high accuracy with outer zone widths of 25 nm, and demonstrated resolution of 23 nm with proper illumination and stability. These permit important advances in the study of protein specific transport and structure in the life sciences [C. Larabell (private communication); W. Meyer-Ilse et al., J. Microsc. 201, 395 (2001)] and the study of magnetic materials [P. Fischer et al., J. Synchrotron. Radiat. 8, 325 (2001)] with elemental sensitivity at the resolution of individual domains. Major corporations (members of the EUV Limited Liability Company are Intel, Motorola, AMD, Micron, Infineon, and IBM) are now preparing the path for the fabrication of future computer chips, in the years 2007 and beyond, using multilayer coated reflective optics, which achieve reflectivities of 70% in the 11-14 nm region [T. Barbee et al., Appl. Opt. 24, 883 (1985); C. Montcalm et al., Proc. SPIE 3676, 710 (1999)]. These coated optics are to be incorporated in extreme ultraviolet (EUV) print cameras, known as "steppers." Electronic patterns with features in the range of 50-70 nm have been printed. The first alpha tool stepper recently demonstrated all critical technologies [D. Tichenor et al., Proc. SPIE 4343, 19 (2001)] needed for EUV lithography. Preproduction beta tools are targeted for delivery by leading suppliers [ASML, the Netherlands, at the SPIE Microlithography Conference, Santa Clara, CA, March 2001] in 2004, with high volume production tools available in late 2006 for manufacturing in 2007. New results in these two areas will be discussed in the context of the synergy of science and technology.

Constraining Initiation and Onset Time of Plate Tectonics on Earth

NASA Astrophysics Data System (ADS)

Roller, G.

2014-12-01

The onset time for modern-style plate tectonics is still heavily debated among geoscientists. Proposed timings range from the Phanerozoic to the Hadean. Here I present a new theoretical approach to tackle this question. I combine ideas of nuclear astrophysics and geochronology and apply the concept of sudden nucleosynthesis to calculate so-called nucleogeochronometric Rhenium-Osmium model ages. Sudden nucleosynthesis has been suggested by nuclear theory [1-2] as a possible mechanism for the creation of the heavy isotopes. Hence, this concept may generally be used to identify rapid (r-) neutron-capture process events. For Earth, nucleogeochronometric model age calculations based upon published pyroxenite and komatiite data [3-5] point to an r-process event around 3 Ga. Since the r-process requires high neutron densities and temperatures within seconds, a gravitational core collapse forming at least a part of the inner core is discussed as a possible cause, thus initiating modern-style plate tectonics at that time. This age is in line with an earlier proposed value of 2.7 Ga for an inner core forming event [6], pronounced changes in the magnitude of the geomagnetic field and geological evidence like the onset of extensive plutonism and crust formation starting around the Archean-Proterozoic transition. Besides, results from nucleogeochronometric age calculations for published peridotitic pentlandites [7] lead to corrections as to their previously inconsistent model ages: These are now in good agreement with their Proterozoic 1.43 Ga isochronous regression line, supporting the model. [1] Burbidge et al. (1957) Revs. Mod. Phys. 29, 547 - 650. [2] Hoyle et al. (1960) ApJ 132, 565 - 590. [3] Reisberg et al. (1991) Earth Planet. Sci. Lett. 105, 196 - 213. [4] Roy-Barman et al. (1996) Chem. Geol. 130, 55 - 64. [5] Luck et al. (1984) Earth Planet Sci. Lett. 68, 205 - 208. [6] Hale (1987) Nature 329, 233 -237. [7] Smit et al. (2010) Geochim. Cosmochim. Acta 74, 3292 - 3306.

Behaviour of Rare Earth Elements during the Earth's core formation

NASA Astrophysics Data System (ADS)

Faure, Pierre; Bouhifd, Mohamed Ali; Boyet, Maud; Hammouda, Tahar; Manthilake, Geeth

2017-04-01

Rare Earth Elements (REE) are classified in the refractory group, which means that they have a high temperature condensation and their volatility-controlled fractionation is limited to high-temperature processes. Anomalies have been measured for Eu, Yb and Sm, which are the REE with the lowest condensation temperatures in CAIs and chondrules (e.g. [1]). REE are particularly abundant in the sulfides of enstatite chondrites, 100 to 1000 times the CI value [e.g. 2,3], proving that these elements are not strictly lithophile under extremely reducing conditions. However by investigating experimentally the impact of Earth's core formation on the behavior of Sm and Nd, we have shown the absence of fractionation between Sm and Nd during the segregation of the metallic phase [4]. Recently, Wohlers and Wood [5] proposed that Nd and Sm could be fractionated in presence of a S-rich alloy phase. However, their results were obtained at pressure and temperature conditions below the plausible conditions of the Earth's core formation. Clearly, large pressure range needs to be covered before well-constrained model can be expected. Furthermore, our preliminary metal-silicate partitioning results show that Ce and Eu have higher metal/silicate partition coefficients than their neighboring elements, and that the presence of sulphur enhances the relative difference between partition coefficients. In this presentation, we will present and discuss new metal-silicate partition coefficients of all REE at a deep magma ocean at pressures ranging from those of the uppermost upper mantle ( 5 GPa) to a maximum pressure expected in the range of 20 GPa, temperatures ranging from 2500 to about 3000 K, and oxygen fugacities within IW-1 to IW-5 (1 to 5 orders of magnitude lower than the iron-wüstite buffer). We will discuss the effect of S, as well as the effect of H2O on the behaviour of REE during the Earth's core formation: recent models suggest that contrary to currently accepted beliefs, the presence of water during the formation of metallic core of terrestrial planets is very plausible [e.g. 6-8]. References [1] Pack et al. (2004) Science 303, 997-1000. [2] Crozaz and Lundberg (1995) Geochim. Cosmochim. Acta 59, 3817-3831. [3] Gannoun et al. (2011) Geochim. Cosmochim. Acta 75, 3269-3289. [4] Bouhifd et al. (2015) Earth Planet. Sci. Lett. 413, 158-166. [5] Wohlers and Wood (2015) Nature 520, 337-340. [6] Marty (2012) Earth Planet. Sci. Lett. 313-314, 56-66. [7] Morbidelli et al. (2000) Meteor. Planet. Sci. 1320, 1309-1320. [8] Sarafian et al. (2014 Science 346, 623-626.

2-20 ns interframe time 2-frame 6.151 keV x-ray imaging on the recently upgraded Z Accelerator: A progress report

NASA Astrophysics Data System (ADS)

Bennett, G. R.; Smith, I. C.; Shores, J. E.; Sinars, D. B.; Robertson, G.; Atherton, B. W.; Jones, M. C.; Porter, J. L.

2008-10-01

When used for the production of an x-ray imaging backlighter source on Sandia National Laboratories' recently upgraded 26MA Z Accelerator, the terawatt-class, multikilojoule, 526.57nm Z-Beamlet laser (ZBL) [P. K. Rambo et al., Appl. Opt. 44, 2421 (2005)], in conjunction with the 6.151keV (1s2-1s2p triplet line of He-like Mn) curved-crystal imager [D. B. Sinars et al., Rev. Sci. Instrum. 75, 3672 (2004); G. R. Bennett et al., Rev. Sci. Instrum. 77, 10E322 (2006)], is capable of providing a high quality x radiograph per Z shot for inertial confinement fusion (ICF), complex hydrodynamics, and other high-energy-density physics experiments. For example, this diagnostic has recently afforded microgram-scale mass perturbation measurements on an imploding ignition-scale 1mg ICF capsule [G. R. Bennett et al., Phys. Rev. Lett. 99, 205003 (2007)], where the perturbation was initiated by a surrogate deuterium-tritium (DT) fuel fill tube. Using an angle-time multiplexing technique, ZBL now has the capability to provide two spatially and temporally separated foci in the Z chamber, allowing "two-frame" imaging to be performed, with an interframe time range of 2-20ns. This multiplexing technique allows the full area of the four-pass amplifiers to be used for the two pulses, rather than split the amplifiers effectively into two rectangular sections, with one leg delayed with respect to the other, which would otherwise double the power imposed onto the various optics thereby halving the damage threshold, for the same irradiance on target. The 6.151keV two frame technique has recently been used to image imploding wire arrays, using a 7.3ns interframe time. The diagnostic will soon be converted to operate with p-rather than s-polarized laser light for enhanced laser absorption in the Mn foil, plus other changes (e.g., operation at the possibly brighter 6.181keV Mn 1s2-1s2p singlet line), to increase x-ray yields. Also, a highly sensitive inline multiframe ultrafast (1ns gate time) digital x-ray camera is being developed [G. R. Bennett et al., Rev. Sci. Instrum. 77, 10E322 (2006)] to extend the system to "four-frame" and markedly improve the signal-to-noise ratio. [At present, time-integrating Fuji BAS-TR2025 image plate (scanned with a Fuji BAS-5000 device) forms the time-integrated image-plane detector.

Fast SiPM Readout of the PANDA TOF Detector

NASA Astrophysics Data System (ADS)

Böhm, M.; Lehmann, A.; Motz, S.; Uhlig, F.

2016-05-01

For the identification of low momentum charged particles and for event timing purposes a barrel Time-of-Flight (TOF) detector surrounding the interaction point is planned for the PANDA experiment at FAIR . Since the boundary conditions in terms of available radial space and radiation length are quite strict the favored layout is a hodoscope composed of several thousand small scintillating tiles (SciTils) read out by silicon photomultipliers (SiPMs). A time resolution of well below 100 ps is aimed for. With the originally proposed 30 × 30 × 5 mm3 SciTils read out by two single 3 × 3 mm2 SiPMs at the rims of the scintillator the targeted time resolution can be just reached, but with a considerable position dependence across the scintillator surface. In this paper we discuss other design options to further improve the time resolution and its homogeneity. It will be shown that wide scintillating rods (SciRods) with a size of, e.g., 50 × 30 × 5 mm3 or longer and read out at opposite sides by a chain of four serially connected SiPMs a time resolution down to 50 ps can be reached without problems. In addition, the position dependence of the time resolution is negligible. These SciRods were tested in the laboratory with electrons of a 90Sr source and under real experimental conditions in a particle beam at CERN. The measured time resolutions using fast BC418 or BC420 plastic scintillators wrapped in aluminum foil were consistently between 45 and 75 ps dependent on the SciRod design. This is a significant improvement compared to the original SciTil layout.

Long-term community reintegration: concepts, outcomes and dilemmas in the case of a military service member with a spinal cord injury.

PubMed

Fritz, Heather Ann; Lysack, Cathy; Luborsky, Mark R; Messinger, Seth D

2015-01-01

Despite growing knowledge about medical and functional recovery in clinical settings, the long-term issue of community reintegration with a spinal cord injury (SCI) in the military context remains virtually unexamined. Thus, the U.S. Department of Defense created the SCI Qualitative Research Program to advance knowledge about service members' reintegration into civilian life. The purpose of this paper is to better characterize the long-term outcomes related to the community participation experienced and desired vis-à-vis a case study of a military veteran who suffered a service-related traumatic SCI. An in-depth anthropological interview was used with Jake, a 28-year old marine with a service-related C5/C6 SCI. Data were analyzed using content analysis. Three significant themes were identified: opportunities for better engaging socially meaningful others may not be adequately included in so-called "client-centered" interventions; how management of the social self in inter-personal interactions and public spaces is critical to gaining broader societal acceptance; and how meaningful age normative relationships and activities are essential to establish lasting inclusive social connections. Jake's case challenges existing models of rehabilitation predominantly focused on physical capacity building. Study findings point to the need for rehabilitation to invest more resources in efforts to address the existential and social elements of long-term social reintegration. Implications for Rehabilitation Both the veteran with SCI and their meaningful support network face challenges socially reintegrating after injury and rehabilitation. Empowering clients to envision future possibilities in terms of family, intimate relationships, and meaningful work are important to successful long-term social reintegration. Addressing the existential desires and social capacities of the individual may be as important as addressing physical functioning skills after SCI.

The electron-phonon interaction with forward scattering peak is dominant in high T c superconductors of FeSe films on {{\\rm{SrTiO}}}_{3} (TiO2)

NASA Astrophysics Data System (ADS)

Kulić, M. L.; Dolgov, O. V.

2017-01-01

The theory of the electron-phonon interaction (EPI) with strong forward scattering peak (FSP) in an extreme delta-peak limit (Kulić and Zeyher 1994 Phys. Rev. B 49 4395; Kulić 2000 Phys. Rep. 38 1-264 Kulić and Dolgov 2005 Phys. Status Solidi b 242 151; Danylenko et al 1999 Eur. Phys. J. B 9 201) is recently applied in (Lee et al 2014 Nature 515 245; Rademaker et al 2016 New J. Phys. 18 022001; Wang et al 2016 Supercond. Sci. Technol. 29 054009) for the explanation of high {T}{{c}}(˜ 100 {{K}}) in a monolayer FeSe grown on {{{SrTiO}}}3 (Lee et al 2014 Nature 515 245) and TiO2 (Rebec et al 2016 arXiv:1606.09358v1) substrates. The EPI is due to a long-range dipolar electric field created by high-energy oxygen vibrations ({{Ω }}˜ 90 meV) at the interface (Lee et al 2014 Nature 515 245; Rademaker et al 2016 New J. Phys. 18 022001; Wang et al 2016 Supercond. Sci. Technol. 29 054009). In leading order (with respect to {T}{{c}0}/{{Ω }}) the mean-field critical temperature {T}{{c}0}={< {V}{{epi}}(q)> }q/4) ˜ {({{aq}}{{c}})}2{V}{{epi}}(0) and the gap {{{Δ }}}0=2{T}{{c}0\\text{}} are due to an interplay between the maximal EPI pairing potential {V}{{epi}}(0) and the FSP-width q c. For {T}{{c}0}˜ 100 K one has {{{Δ }}}0˜ 16 meV in a satisfactory agreement with ARPES experiments. In leading order T c0 is mass-independent and a very small oxygen isotope effect is expected in next to leading order. In clean systems T c0 for s-wave and d-wave pairing is degenerate but both are affected by non-magnetic impurities, which are pair-weakening in the s-channel and pair-breaking in the d-channel. The self-energy and replica bands at T = 0 and at the Fermi surface are calculated and compared with experimental results at T> 0 ( Rademaker et al 2016 New J. Phys. 18 022001; Wang et al 2016 Supercond. Sci. Technol. 29 054009). The EPI coupling constant {λ }{{m}}={< {V}{{epi}}(q)> }q/2{{Ω }} is mass-dependent ({M}1/2) and at ω (\\ll {{Ω }}) makes the slope of the self-energy {{Σ }}(k,ω )(≈ -{λ }{{m}}ω ) and the replica intensities {A}i(˜ {λ }{{m}}) mass-dependent. This result, overlooked in the literature, is contrary to the prediction of the standard Migdal-Eliashberg theory for EPI. The small oxygen isotope effect in {T}{{c}0} and pronounced isotope effect in {{Σ }}(k,ω ) and ARPES spectra A i of the replica bands in FeSe films on SrTiO3 and TiO2 is a smoking-gun experiment for validity of the EPI-FSP theory to these systems. The EPI-FSP theory predicts a large number of low-laying pairing states, thus causing internal pair fluctuations. The latter reduce T c0 additionally, by creating a pseudogap state for {T}{{c}}< T< {T}{{c}0}. Possibilities to increase T c0, by designing novel structures are discussed in the framework of the EPI-FSP theory.

Re-Thinking Science Capital: The Role of "Capital" and "Identity" in Mediating Students' Engagement with Mathematically Demanding Programmes at University

ERIC Educational Resources Information Center

Black, Laura; Hernandez-Martinez, Paul

2016-01-01

A wide body of literature has highlighted how high achievement in mathematics in secondary school does not necessarily motivate students to both choose and succeed on mathematically demanding programmes at post-compulsory level. The recent Enterprising Science project [Archer et al. (2015, "J. Res. Sci. Teach.," 52, 922-948)] and before…

Consistency of Students' Conceptions of Wave Propagation: Findings from a Conceptual Survey in Mechanical Waves

ERIC Educational Resources Information Center

Tongchai, Apisit; Sharma, Manjula Devi; Johnston, Ian D.; Arayathanitkul, Kwan; Soankwan, Chernchok

2011-01-01

We recently developed a multiple-choice conceptual survey in mechanical waves. The development, evaluation, and demonstration of the use of the survey were reported elsewhere [A. Tongchai et al. Int. J. Sci. Educ. 31 2437 (2009)]. We administered the survey to 902 students from seven different groups ranging from high school to second year…

Strained InGaAs/InAlAs Quantum Wells for Complementary III-V Transistors

DTIC Science & Technology

2014-01-01

GaAs substrates for low power and high frequency applications, J. Appl. Phys. 109 (2011) 033706. [28] A. Ali, H. Madan , A. Agrawal, I. Ramirez, R...Growth of InAsSb-channel high electron mobility transistor structures, J. Vac. Sci. Technol. B 23 (2005) 1441–1444. [30] A. Ali, H. Madan , M.J

The Earth System Prediction Suite: Toward a Coordinated U.S. Modeling Capability

DTIC Science & Technology

2015-01-01

517 regional information products ( Goodall et al. 2013). 518 A critical aspect of future work is the evaluation and evolution of NUOPC and ESMF...Atmosphere (NUMA). SIAM J. Sci. Comp. 35(5), B1162-700 B1194. 701 Goodall , J. L., K. D. Saint, M. B. Ercan, L. J. Baily, S. Murphy, C. DeLuca, R. B

Efficacy of a Commercial Bacterin in Protecting Strain 13 Guinea Pigs against Bordetella bronchiseptica Pneumonia.

DTIC Science & Technology

1986-12-01

colonies have continued to occur (2-4). In addition to bronchopneumonia, it also induces abortion, still births, infertility, and otitis media (5-7...New York, NY 1976; 121-35. 7. Wagner JE, Owens DR, Kusewitt DF, et al. Otitis media of guinea pigs. Lab Anim Sci 1976; 26:902-7. 8. Shimizu T

The Plasmodium falciparum Sexual Development Transcriptome: A Microarray Analysis using Ontology-Based Pattern Identification

DTIC Science & Technology

2005-06-17

ciparum. Mol Biochem Parasitol 1992;56(2):239–50. [56] Vinetz JM, Dave SK, Specht CA, et al. The chitinase PfCHT1 from the human malaria parasite Plasmodium...falciparum lacks proenzyme and chitin -binding domains and displays unique substrate prefer- ences. Proc Natl Acad Sci USA 1999;96(24):14061–6. [57

Parents' Translations of Child Gesture Facilitate Word Learning in Children with Autism, Down Syndrome and Typical Development

ERIC Educational Resources Information Center

Dimitrova, Nevena; Özçaliskan, Seyda; Adamson, Lauren B.

2016-01-01

Typically-developing (TD) children frequently refer to objects uniquely in gesture. Parents translate these gestures into words, facilitating children's acquisition of these words (Goldin-Meadow et al. in "Dev Sci" 10(6):778-785, 2007). We ask whether this pattern holds for children with autism (AU) and with Down syndrome (DS) who show…

Progress towards an effective model for FeSe from high-accuracy first-principles quantum Monte Carlo

NASA Astrophysics Data System (ADS)

Busemeyer, Brian; Wagner, Lucas K.

While the origin of superconductivity in the iron-based materials is still controversial, the proximity of the superconductivity to magnetic order is suggestive that magnetism may be important. Our previous work has suggested that first-principles Diffusion Monte Carlo (FN-DMC) can capture magnetic properties of iron-based superconductors that density functional theory (DFT) misses, but which are consistent with experiment. We report on the progress of efforts to find simple effective models consistent with the FN-DMC description of the low-lying Hilbert space of the iron-based superconductor, FeSe. We utilize a procedure outlined by Changlani et al.[1], which both produces parameter values and indications of whether the model is a good description of the first-principles Hamiltonian. Using this procedure, we evaluate several models of the magnetic part of the Hilbert space found in the literature, as well as the Hubbard model, and a spin-fermion model. We discuss which interaction parameters are important for this material, and how the material-specific properties give rise to these interactions. U.S. Department of Energy, Office of Science, Office of Advanced Scientific Computing Research, Scientific Discovery through Advanced Computing (SciDAC) program under Award No. FG02-12ER46875, as well as the NSF Graduate Research Fellowship Program.

Formation of epitaxial Al 2O 3/NiAl(1 1 0) films: aluminium deposition

NASA Astrophysics Data System (ADS)

Lykhach, Y.; Moroz, V.; Yoshitake, M.

2005-02-01

Structure of epitaxial Al 2O 3 layers formed on NiAl(1 1 0) substrates has been studied by means of reflection high-energy electron diffraction (RHEED). The elucidated structure was compared to the model suggested for 0.5 nm-thick Al 2O 3 layers [K. Müller, H. Lindner, D.M. Zehner, G. Ownby, Verh. Dtsch. Phys. Ges. 25 (1990) 1130; R.M. Jaeger, H. Kuhlenbeck, H.J. Freund, Surf. Sci. 259 (1991) 235]. The stepwise growth of Al 2O 3 film, involving deposition and subsequent oxidation of aluminium onto epitaxial 0.5 nm-thick Al 2O 3 layers, has been investigated. Aluminium was deposited at room temperature, whereas its oxidation took place during annealing at 1070 K. The Al 2O 3 thickness was monitored by means of Auger electron spectroscopy (AES). It was found that Al 2O 3 layer follows the structure of 0.5 nm thick Al 2O 3 film, although a tilting of Al 2O 3(1 1 1) surface plane with respect to NiAl(1 1 0) surface appeared after Al deposition.

Whistler wave propagation in the antenna near and far fields in the Naval Research Laboratory Space Physics Simulation Chamber

DOE Office of Scientific and Technical Information (OSTI.GOV)

Blackwell, David D.; Walker, David N.; Amatucci, William E.

2010-01-15

In previous papers, early whistler propagation measurements were presented [W. E. Amatucci et al., IEEE Trans. Plasma Sci. 33, 637 (2005)] as well as antenna impedance measurements [D. D. Blackwell et al., Phys. Plasmas 14, 092106 (2007)] performed in the Naval Research Laboratory Space Physics Simulation Chamber (SPSC). Since that time there have been major upgrades in the experimental capabilities of the laboratory in the form of improvement of both the plasma source and antennas. This has allowed access to plasma parameter space that was previously unattainable, and has resulted in measurements that provide a significantly clearer picture of whistlermore » propagation in the laboratory environment. This paper presents some of the first whistler experimental results from the upgraded SPSC. Whereas previously measurements were limited to measuring the cyclotron resonance cutoff and elliptical polarization indicative of the whistler mode, now it is possible to experimentally plot the dispersion relation itself. The waves are driven and detected using balanced dipole and loop antennas connected to a network analyzer, which measures the amplitude and phase of the wave in two dimensions (r and z). In addition the frequency of the signals is also swept over a range of several hundreds of megahertz, providing a comprehensive picture of the near and far field antenna radiation patterns over a variety of plasma conditions. The magnetic field is varied from a few gauss to 200 G, with the density variable over at least 3 decades from 10{sup 7} to 10{sup 10} cm{sup -3}. The waves are shown to lie on the dispersion surface for whistler waves, with observation of resonance cones in agreement with theoretical predictions. The waves are also observed to propagate without loss of amplitude at higher power, a result in agreement with previous experiments and the notion of ducted whistlers.« less

Muscle synergy space: learning model to create an optimal muscle synergy

PubMed Central

Alnajjar, Fady; Wojtara, Tytus; Kimura, Hidenori; Shimoda, Shingo

2013-01-01

Muscle redundancy allows the central nervous system (CNS) to choose a suitable combination of muscles from a number of options. This flexibility in muscle combinations allows for efficient behaviors to be generated in daily life. The computational mechanism of choosing muscle combinations, however, remains a long-standing challenge. One effective method of choosing muscle combinations is to create a set containing the muscle combinations of only efficient behaviors, and then to choose combinations from that set. The notion of muscle synergy, which was introduced to divide muscle activations into a lower-dimensional synergy space and time-dependent variables, is a suitable tool relevant to the discussion of this issue. The synergy space defines the suitable combinations of muscles, and time-dependent variables vary in lower-dimensional space to control behaviors. In this study, we investigated the mechanism the CNS may use to define the appropriate region and size of the synergy space when performing skilled behavior. Two indices were introduced in this study, one is the synergy stability index (SSI) that indicates the region of the synergy space, the other is the synergy coordination index (SCI) that indicates the size of the synergy space. The results on automatic posture response experiments show that SSI and SCI are positively correlated with the balance skill of the participants, and they are tunable by behavior training. These results suggest that the CNS has the ability to create optimal sets of efficient behaviors by optimizing the size of the synergy space at the appropriate region through interacting with the environment. PMID:24133444

Water vapor on Titan: the stratospheric vertical profile from Cassini/CIRS infrared spectra

NASA Astrophysics Data System (ADS)

Cottini, V.; Jennings, D. E.; Nixon, C. A.; Anderson, C. M.; Gorius, N.; Bjoraker, G. L.; Coustenis, A.; Achterberg, R. K.; Teanby, N. A.; de Kok, R.; Irwin, P. G. J.; Bézard, B.; Lellouch, E.; Flasar, F. M.; Bampasidis, G.

2012-04-01

Water vapor in Titan’s middle atmosphere has previously been detected only by disk-average observations from the Infrared Space Observatory (Coustenis et al., 1998). We report here the successful detection of stratospheric water vapor using the Cassini Composite Infrared Spectrometer (CIRS, Flasar et al., 2004) following an earlier null result (de Kok et al., 2007a). CIRS senses water emissions in the far-infrared spectral region near 50 microns, which we have modeled using two independent radiative transfer and inversion codes (NEMESIS, Irwin et al 2008 and ART, Coustenis et al., 2010). From the analysis of nadir spectra we have derived a mixing ratio of (0.14 ± 0.05) ppb at 100 km, corresponding to a column abundance of approximately (3.7 ± 1.3) × 10^14 mol/cm2. Using limb observations, we obtained mixing ratios of (0.13 ± 0.04) ppb at 125 km and (0.45 ± 0.15) ppb at 225 km of altitude, confirming that the water abundance has a positive vertical gradient as predicted by photochemical models. In the latitude range (80˚S - 30˚N) we see no evidence for latitudinal variations in these abundances within the error bars. References: Coustenis, A.; Salama, A.; Lellouch, E.; Encrenaz, Th.; Bjoraker, G. L.; Samuelson, R. E.; de Graauw, Th.; Feuchtgruber, H.; Kessler, M. F., 1998. Evidence for water vapor in Titan's atmosphere from ISO/SWS data. Astronomy and Astrophysics, v.336, p.L85-L89 Coustenis, A.; Jennings, D. E.; Nixon, C. A.; Achterberg, R. K.; Lavvas, P.; Vinatier, S.; Teanby, N. A.; Bjoraker, G. L.; Carlson, R. C.; Piani, L.; Bampasidis, G.; Flasar, F. M.; Romani, P. N., 2010. Titan trace gaseous composition from CIRS at the end of the Cassini-Huygens prime mission. Icarus, Volume 207, Issue 1, p. 461-476. de Kok, R.; Irwin, P. G. J.; Teanby, N. A.; Lellouch, E.; Bézard, B.; Vinatier, S.; Nixon, C. A.; Fletcher, L.; Howett, C.; Calcutt, S. B.; Bowles, N. E.; Flasar, F. M.; Taylor, F. W. , 2007a. Oxygen compounds in Titan's stratosphere as observed by Cassini CIRS. Icarus, Volume 186, Issue 2, p. 354-363 Flasar, F. M., and 44 colleagues, 2004. Exploring the Saturn system in the thermal infrared: The Composite Infrared Spectrometer. Space Sci. Rev. 115, 169 - 297

Bayesian deconvolution of [corrected] fMRI data using bilinear dynamical systems.

PubMed

Makni, Salima; Beckmann, Christian; Smith, Steve; Woolrich, Mark

2008-10-01

In Penny et al. [Penny, W., Ghahramani, Z., Friston, K.J. 2005. Bilinear dynamical systems. Philos. Trans. R. Soc. Lond. B Biol. Sci. 360(1457) 983-993], a particular case of the Linear Dynamical Systems (LDSs) was used to model the dynamic behavior of the BOLD response in functional MRI. This state-space model, called bilinear dynamical system (BDS), is used to deconvolve the fMRI time series in order to estimate the neuronal response induced by the different stimuli of the experimental paradigm. The BDS model parameters are estimated using an expectation-maximization (EM) algorithm proposed by Ghahramani and Hinton [Ghahramani, Z., Hinton, G.E. 1996. Parameter Estimation for Linear Dynamical Systems. Technical Report, Department of Computer Science, University of Toronto]. In this paper we introduce modifications to the BDS model in order to explicitly model the spatial variations of the haemodynamic response function (HRF) in the brain using a non-parametric approach. While in Penny et al. [Penny, W., Ghahramani, Z., Friston, K.J. 2005. Bilinear dynamical systems. Philos. Trans. R. Soc. Lond. B Biol. Sci. 360(1457) 983-993] the relationship between neuronal activation and fMRI signals is formulated as a first-order convolution with a kernel expansion using basis functions (typically two or three), in this paper, we argue in favor of a spatially adaptive GLM in which a local non-parametric estimation of the HRF is performed. Furthermore, in order to overcome the overfitting problem typically associated with simple EM estimates, we propose a full Variational Bayes (VB) solution to infer the BDS model parameters. We demonstrate the usefulness of our model which is able to estimate both the neuronal activity and the haemodynamic response function in every voxel of the brain. We first examine the behavior of this approach when applied to simulated data with different temporal and noise features. As an example we will show how this method can be used to improve interpretability of estimates from an independent component analysis (ICA) analysis of fMRI data. We finally demonstrate its use on real fMRI data in one slice of the brain.

Constraining martian atmospheric dust particle size distributions from MER Navcam observations.

NASA Astrophysics Data System (ADS)

Soderblom, J. M.; Smith, M. D.

2017-12-01

Atmospheric dust plays an important role in atmospheric dynamics by absorbing energy and influencing the thermal structure of the atmosphere [1]. The efficiency by which dust absorbs energy depends on its size and single-scattering albedo. Characterizing these properties and their variability is, thus, important in modeling atmospheric circulation. Near-sun observations of the martian sky from Viking Lander, Mars Pathfinder, and MER Pancam images have been used to characterize the atmospheric scattering phase function. The forward-scattering peak the atmospheric phase function is primarily controlled by the size of aerosol particles and is less sensitive to atmospheric opacity or particle shape and single-scattering albedo [2]. These observations, however, have been limited to scattering angles >5°. We use the MER Navcams, which experience little-to-no debilitating internal instrumental scattered light during near-Sun imaging, enabling measurements of the brightness of the martian sky down to very small scattering angles [3], making them more sensitive to aerosol particle size. Additionally, the Navcams band-pass wavelength is similar to the dust effective particle size, further increasing this sensitivity. These data sample a wide range of atmospheric conditions, including variations in the atmospheric dust loading across the entire martian year, as well as more rapid variations during the onset and dissipation of a global-scale dust storm. General circulation models (GCMs) predict a size-dependence for the transport of dust during dust storms that would result in both spatial (on regional-to-global scales) and temporal (days-to-months) variations in the dust size distribution [4]. The absolute calibration of these data, however, is limited. The instrument temperature measurement is limited to a single thermocouple on the Opportunity left Navcam CCD, and observations of the calibration target by Navcam are infrequent. We discuss ways to mitigate these uncertainties and provide improved recovery of dust particle size distributions from these data. [1] Gierasch and Goody, 1972, J. Atmos. Sci., 29, 400-402. [2] Hansen and Travis, 1974, Space Sci. Rev., 16, 527-610. [3] Soderblom et al., 2008; JGR E06S19. [4] Murphy et al., 1993, JGR 98(E2), 3197-3220.

Gym-based exoskeleton walking: A preliminary exploration of non-ambulatory end-user perspectives.

PubMed

Cahill, Aoife; Ginley, Orna Mc; Bertrand, Courtney; Lennon, Olive

2018-07-01

Robotic walking devices (RWD) have shown many physical benefits in Spinal Cord Injury (SCI) rehabilitation. No study to date has explored end-user perceptions of these devices or gained insight into the use of these devices in a gym-based setting. This preliminary study explores the perspectives of four non-ambulatory individuals with SCI on using an exoskeleton walking device in a gym-based community setting. In-depth, semi-structured interviews were conducted with four SCI individuals living in the community. Interviews were audio-recorded and transcribed verbatim. Inductive thematic analysis established common overarching themes and subthemes. Four primary themes emerged addressing "The Psychological Adjustments Around Using RWDs with Respect to Disability", "Perceived Physical, Social and Psychological Benefits of Using an Exoskeleton", "The Role of External Influences", and "A Wellness Model to Health". A fully integrated gym setting was found to provide a positive and encouraging space to utilise the device. In addition, both the ability to set training goals and the positive attitude of robotic trainers were deemed to be important factors. This preliminary study provides detailed perspectives of four non-ambulatory individuals with SCI on utilising an exoskeleton walking device in a community setting. It suggests that gym-based RWDs impact positively on the users' lives and enhance their perceived wellbeing and sense of community integration. Enabling access to similar, community-based facilities should be prioritised for those with longstanding SCI disability. Copyright © 2018 Elsevier Inc. All rights reserved.

Modulation of corticospinal input to the legs by arm and leg cycling in people with incomplete spinal cord injury.

PubMed

Zhou, R; Alvarado, L; Kim, S; Chong, S L; Mushahwar, V K

2017-10-01

The spinal cervico-lumbar interaction during rhythmic movements in humans has recently been studied; however, the role of arm movements in modulating the corticospinal drive to the legs is not well understood. The goals of this study were to investigate the effect of active rhythmic arm movements on the corticospinal drive to the legs ( study 1 ) and assess the effect of simultaneous arm and leg training on the corticospinal pathway after incomplete spinal cord injury (iSCI) ( study 2). In study 1 , neurologically intact (NI) participants or participants with iSCI performed combinations of stationary and rhythmic cycling of the arms and legs while motor evoked potentials (MEPs) were recorded from the vastus lateralis (VL) muscle. In the NI group, arm cycling alone could facilitate the VL MEP amplitude, suggesting that dynamic arm movements strongly modulate the corticospinal pathway to the legs. No significant difference in VL MEP between conditions was found in participants with iSCI. In study 2 , participants with iSCI underwent 12 wk of electrical stimulation-assisted cycling training: one group performed simultaneous arm and leg (A&L) cycling and the other legs-only cycling. MEPs in the tibialis anterior (TA) muscle were compared before and after training. After training, only the A&L group had a significantly larger TA MEP, suggesting increased excitability in the corticospinal pathway. The findings demonstrate the importance of arm movements in modulating the corticospinal drive to the legs and suggest that active engagement of the arms in lower limb rehabilitation may produce better neural regulation and restoration of function. NEW & NOTEWORTHY This study aimed to demonstrate the importance of arm movements in modulating the corticospinal drive to the legs. It provides direct evidence in humans that active movement of the arms could facilitate corticospinal transmission to the legs and, for the first time, shows that facilitation is absent after spinal cord injury. Active engagement of the arms in lower limb rehabilitation increased the excitability of the corticospinal pathway and may produce more effective improvement in leg function. Copyright © 2017 the American Physiological Society.

Intermittent fasting in mice does not improve hindlimb motor performance after spinal cord injury.

PubMed

Streijger, Femke; Plunet, Ward T; Plemel, Jason Ryan; Lam, Clarrie K; Liu, Jie; Tetzlaff, Wolfram

2011-06-01

Previously, we reported that every-other-day-fasting (EODF) in Sprague-Dawley rats initiated after cervical spinal cord injury (SCI) effectively promoted functional recovery, reduced lesion size, and enhanced sprouting of the corticospinal tract. More recently, we also showed improved behavioral recovery with EODF after a moderate thoracic contusion injury in rats. In order to make use of transgenic mouse models to study molecular mechanisms of EODF, we tested here whether this intermittent fasting regimen was also beneficial in mice after SCI. Starting after SCI, C57BL/6 mice were fed a standard rodent chow diet either with unrestricted access or feeding every other day. Over a 14-week post-injury period, we assessed hindlimb locomotor function with the Basso Mouse Scale (BMS) open-field test and horizontal ladder, and the spinal cords were evaluated histologically to measure white and grey matter sparing. EODF resulted in an overall caloric restriction of 20% compared to animals fed ad libitum (AL). The EODF-treated animals exhibited a ∼ 14% reduction in body weight compared to AL mice, and never recovered to their pre-operative body weight. In contrast to rats on an intermittent fasting regimen, mice exhibited no increase in blood ketone bodies by the end of the second, third, and fourth day of fasting. EODF had no beneficial effect on tissue sparing and failed to improve behavioral recovery of hindlimb function. Hence this observation stands in stark contrast to our earlier observations in Sprague-Dawley rats. This is likely due to the difference in the metabolic response to intermittent fasting as evidenced by different ketone levels during the first week of the EODF regimen.

On the ability of the Viking gas chromatograph–mass spectrometer to detect organic matter

PubMed Central

Biemann, Klaus

2007-01-01

A recent paper by Navarro-Gonzalez et al. [Navarro-Gonzalez R, Navarro KF, de la Rosa J, Iniguez E, Molina P, Miranda LD, Morales P, Cienfuegos E, Coll P, Raulin F, et al. (2006) Proc Natl Acad Sci USA 103:16089–16094] claims to show that the Viking GCMS (gas chromatograph–mass spectrometer) experiment, which carried out a search for organic matter at the surface of Mars in 1976, “may have been blind to low levels of organics.” To rebut this assertion, the Viking experiment, test data, and results on Mars are reviewed, and the fallacies in the design, execution, and interpretation of the new experiments presented by Navarro-Gonzalez et al. are critically examined. PMID:17548829

On the ability of the Viking gas chromatograph-mass spectrometer to detect organic matter.

PubMed

Biemann, Klaus

2007-06-19

A recent paper by Navarro-Gonzalez et al. [Navarro-Gonzalez R, Navarro KF, de la Rosa J, Iniguez E, Molina P, Miranda LD, Morales P, Cienfuegos E, Coll P, Raulin F, et al. (2006) Proc Natl Acad Sci USA 103:16089-16094] claims to show that the Viking GCMS (gas chromatograph-mass spectrometer) experiment, which carried out a search for organic matter at the surface of Mars in 1976, "may have been blind to low levels of organics." To rebut this assertion, the Viking experiment, test data, and results on Mars are reviewed, and the fallacies in the design, execution, and interpretation of the new experiments presented by Navarro-Gonzalez et al. are critically examined.

An independent evaluation of the Younger Dryas extraterrestrial impact hypothesis.

PubMed

Surovell, Todd A; Holliday, Vance T; Gingerich, Joseph A M; Ketron, Caroline; Haynes, C Vance; Hilman, Ilene; Wagner, Daniel P; Johnson, Eileen; Claeys, Philippe

2009-10-27

Based on elevated concentrations of a set of "impact markers" at the onset of the Younger Dryas stadial from sedimentary contexts across North America, Firestone, Kennett, West, and others have argued that 12.9 ka the Earth experienced an impact by an extraterrestrial body, an event that had devastating ecological consequences for humans, plants, and animals in the New World [Firestone RB, et al. (2007) Proc. Natl. Acad. Sci. USA 104:16016-16021]. Herein, we report the results of an independent analysis of magnetic minerals and microspherules from seven sites of similar age, including two examined by Firestone et al. We were unable to reproduce any results of the Firestone et al. study and find no support for Younger Dryas extraterrestrial impact.

Progress in NMR Studies of Liquid Ceramic Materials

NASA Astrophysics Data System (ADS)

Marzke, Robert F.; Piwowarczyk, Jeremy; Boucher, Susan; Wolf, George H.

2003-10-01

The availability of molten, levitated samples of Al-containing ceramics at temperatures of 2,000^oC and higher permits a broad range of important materials to be investigated by the powerful techniques of NMR.footnote Coutures, J-P., Massiot, D., Bessada, C., Echegut, P., Rifflet, J-C. & Taulelle F., Etude par RMN 27Al daluminates liquides dans le domaine 1600-2100 ^oC. C.R. Acad. Sci. Paris, 1990, 310, 1041. Standard measurements of chemical shift as a function of composition yield information concerning the bonding of Al and the structure of liquid phases, for both novel and well-studied refractory materials. Studies of incoherent motions in a sample, such as Al diffusion or time-dependent convective currents, may also be performed when magnetic field gradients are incorporated into the experimental NMR probe. Recent advances are reviewed, in several research areas.

Turbulent equipartition pinch of toroidal momentum in spherical torus

NASA Astrophysics Data System (ADS)

Hahm, T. S.; Lee, J.; Wang, W. X.; Diamond, P. H.; Choi, G. J.; Na, D. H.; Na, Y. S.; Chung, K. J.; Hwang, Y. S.

2014-12-01

We present a new analytic expression for turbulent equipartition (TEP) pinch of toroidal angular momentum originating from magnetic field inhomogeneity of spherical torus (ST) plasmas. Starting from a conservative modern nonlinear gyrokinetic equation (Hahm et al 1988 Phys. Fluids 31 2670), we derive an expression for pinch to momentum diffusivity ratio without using a usual tokamak approximation of B ∝ 1/R which has been previously employed for TEP momentum pinch derivation in tokamaks (Hahm et al 2007 Phys. Plasmas 14 072302). Our new formula is evaluated for model equilibria of National Spherical Torus eXperiment (NSTX) (Ono et al 2001 Nucl. Fusion 41 1435) and Versatile Experiment Spherical Torus (VEST) (Chung et al 2013 Plasma Sci. Technol. 15 244) plasmas. Our result predicts stronger inward pinch for both cases, as compared to the prediction based on the tokamak formula.

(Quasi)-convexification of Barta's (multi-extrema) bounding theorem: Inf_x\\big(\\ssty\\frac{H\\Phi(x)}{\\Phi(x)} \\big) \\le E_gr \\le Sup_x \\big(\\ssty\\frac{H\\Phi(x)}{\\Phi(x)} \\big)

NASA Astrophysics Data System (ADS)

Handy, C. R.

2006-03-01

There has been renewed interest in the exploitation of Barta's configuration space theorem (BCST) (Barta 1937 C. R. Acad. Sci. Paris 204 472) which bounds the ground-state energy, Inf_x\\big({{H\\Phi(x)}\\over {\\Phi(x)}} \\big ) \\leq E_gr \\leq Sup_x \\big({{H\\Phi(x)}\\over {\\Phi(x)}}\\big) , by using any Φ lying within the space of positive, bounded, and sufficiently smooth functions, {\\cal C} . Mouchet's (Mouchet 2005 J. Phys. A: Math. Gen. 38 1039) BCST analysis is based on gradient optimization (GO). However, it overlooks significant difficulties: (i) appearance of multi-extrema; (ii) inefficiency of GO for stiff (singular perturbation/strong coupling) problems; (iii) the nonexistence of a systematic procedure for arbitrarily improving the bounds within {\\cal C} . These deficiencies can be corrected by transforming BCST into a moments' representation equivalent, and exploiting a generalization of the eigenvalue moment method (EMM), within the context of the well-known generalized eigenvalue problem (GEP), as developed here. EMM is an alternative eigenenergy bounding, variational procedure, overlooked by Mouchet, which also exploits the positivity of the desired physical solution. Furthermore, it is applicable to Hermitian and non-Hermitian systems with complex-number quantization parameters (Handy and Bessis 1985 Phys. Rev. Lett. 55 931, Handy et al 1988 Phys. Rev. Lett. 60 253, Handy 2001 J. Phys. A: Math. Gen. 34 5065, Handy et al 2002 J. Phys. A: Math. Gen. 35 6359). Our analysis exploits various quasi-convexity/concavity theorems common to the GEP representation. We outline the general theory, and present some illustrative examples.

On Convergence of Extended Dynamic Mode Decomposition to the Koopman Operator

NASA Astrophysics Data System (ADS)

Korda, Milan; Mezić, Igor

2018-04-01

Extended dynamic mode decomposition (EDMD) (Williams et al. in J Nonlinear Sci 25(6):1307-1346, 2015) is an algorithm that approximates the action of the Koopman operator on an N-dimensional subspace of the space of observables by sampling at M points in the state space. Assuming that the samples are drawn either independently or ergodically from some measure μ , it was shown in Klus et al. (J Comput Dyn 3(1):51-79, 2016) that, in the limit as M→ ∞, the EDMD operator K_{N,M} converges to K_N, where K_N is the L_2(μ )-orthogonal projection of the action of the Koopman operator on the finite-dimensional subspace of observables. We show that, as N → ∞, the operator K_N converges in the strong operator topology to the Koopman operator. This in particular implies convergence of the predictions of future values of a given observable over any finite time horizon, a fact important for practical applications such as forecasting, estimation and control. In addition, we show that accumulation points of the spectra of K_N correspond to the eigenvalues of the Koopman operator with the associated eigenfunctions converging weakly to an eigenfunction of the Koopman operator, provided that the weak limit of the eigenfunctions is nonzero. As a by-product, we propose an analytic version of the EDMD algorithm which, under some assumptions, allows one to construct K_N directly, without the use of sampling. Finally, under additional assumptions, we analyze convergence of K_{N,N} (i.e., M=N), proving convergence, along a subsequence, to weak eigenfunctions (or eigendistributions) related to the eigenmeasures of the Perron-Frobenius operator. No assumptions on the observables belonging to a finite-dimensional invariant subspace of the Koopman operator are required throughout.

Changes in redox properties of humic acids upon sorption to alumina

NASA Astrophysics Data System (ADS)

Subdiaga, Edisson; Orsetti, Silvia; Jindal, Sharmishta; Haderlein, Stefan B.

2016-04-01

1. Introduction A prominent role of Natural Organic Matter (NOM) in biogeochemical processes is its ability to act as an electron shuttle, accelerating rates between a bulk electron donor and an acceptor. The underlying processes are reversible redox reactions of quinone moieties.1 This shuttling effect has been studied in two major areas: transformation of redox active pollutants and microbial respiration.2-3 Previous studies primarily compared effects in the presence or absence of NOM without addressing the redox properties of NOM nor its speciation. The interaction between humic acids (HA) and minerals might change properties and reactivity of organic matter. Specifically, we investigate whether changes in the redox properties of a HA occur upon sorption to redox inactive minerals. Since fractionation and conformational rearrangements of NOM moieties upon sorption are likely to happen, the redox properties of the NOM fractions upon sorption might differ as well. 2. Materials and methods Elliot Soil Humic Acid (ESHA), Pahokee Peat Humic Acid (PPHA) and Suwannee River Humic Acid (SRHA) were used as received from IHSS. Aluminum oxide (Al2O3) was suspended in 0.1M KCl. Sorption was studied at pH 7.0 in duplicate batch experiments for several HA/Al2O3 ratios. For the suspension (mineral + sorbed HA, plus dissolved HA), the filtrate (0.45μm) and the HA stock solution, the electron donating and accepting capacities (EDC and EAC) were determined following established procedures.4 3. Results All studied HA-Al2O3 systems showed similar behavior with regard to changes in redox properties. There was a significant increase in the EDC of the whole suspension compared to the stock solutions and the non-sorbed HA in the filtrate (up to 300% for PPHA). This effect was more pronounced with increasing amounts of sorbed HA in the suspension. Although ESHA had the highest sorption capacity on Al2O3 (~ 6 times higher than PPHA & SRHA), it showed the smallest changes in redox properties upon sorption. Considering the total electron exchange capacities, significant changes were found mainly at higher amounts of sorbed PPHA and SRHA. 4. Conclusions Overall, our results suggest a change in the redox properties of sorbed HA but not for the dissolved fraction. The sorbed fraction showed a higher redox capacity than the stock samples. Given the absence of redox transfer between the HA and the redox inert aluminum oxide, such changes might be due to conformational changes in the humic substances. 5. References [1] Scott D., Mcknight, D., Blunt-Harris, E., Kolesar, S., Lovley, A. Environ. Sci. Technol. 1998, 32, 2984-2989. [2] Dunnivant, F. Schwarzenbach, R., Macalady, D. Environ. Sci. Technol. 1992, 26(11), 2133-2141. [3] Jiang, J. & Kappler, A. Environ. Sci. Technol. 2008, 42(10), 3562-3569. [4] Aeschbacher, M., Sander M., Schwarzenbach, R. Environ. Sci. Technol. 2010, 44(1), 87-93.

Rhenium - osmium heterogeneity of enriched mantle basalts explained by composition and behaviour of mantle-derived sulfides

NASA Astrophysics Data System (ADS)

Harvey, J.; Dale, C. W.; Gannoun, A.; Burton, K. W.

2010-12-01

Analyses of enriched mantle (EM) -basalts, using lithophile element-based isotope systems have long provided evidence for discrete, but variable mantle reservoirs [1]. Upon partial melting, the isotopic fingerprint of each reservoir is imparted upon the partial melt produced. However, recent work involving the Re-Os isotope systematics of EM-basalts [2] suggests that it may not be so simple to delimit these previously well defined mantle reservoirs; the “mantle zoo” [3] may contain more reservoirs than previously envisaged. However, a simple model, with varying contributions from two populations of compositionally distinct mantle sulfides can readily account for the observed heterogeneities in Re-Os isotope systematics of such basalts without additional mantle reservoirs. Rhenium-osmium elemental and isotopic analyses of individual sulfide grains separated from spinel lherzolites from Kilbourne Hole, NM, USA demonstrate that two discrete populations of mantle sulfide exist in terms of both Re-Os systematics and textural relationship with co-existing silicates. One population, with a rounded morphology, is preserved in silicate grains and typically possesses high [Os], low [Re] with unradiogenic, typically sub-chondritic, 187Os/188Os attributable to long term isolation in a low-Re environment. By contrast, irregular-shaped sulfides, preserved along silicate grain boundaries, possess low [Os], higher [Re] and a wider range of, but generally supra-chondritic, 187Os/188Os ([Os] typically ≤ 1-2 ppm, 187Os/188Os ≤ 0.3729; this study). This population is thought to represent metasomatic sulfide (e.g. [4,5]). Uncontaminated silicate phases contain negligible Os (<100 ppt) therefore the Os elemental and isotope composition of basalts is dominated by volumetrically insignificant sulfide ([Os] ≤ 37 ppm, this study). During the early stages of partial melting, supra-chondritic interstitial sulfides are mobilized and incorporated into the melt, adding their radiogenic 187Os/188Os signature. Only when sulfides armored within silicates are exposed to the melt through continued partial melting will enclosed sulfides add their high [Os] and unradiogenic 187Os/188Os to the aggregate melt. Platinum-group element data for whole rocks are also consistent with this scenario. The sequence of (i) addition of all the metasomatic sulfide, followed by (ii) the incorporation of small amounts of armored sulfide can thus account for the range of both [Os] and 187Os/188Os of EM-basalts worldwide without the need for contributions from additional silicate mantle reservoirs. References: [1] Zindler & Hart, (1986) Annu. Rev. Earth Planet. Sci. 14, 493-571. [2] Class et al. (2009) Earth Planet. Sci. Lett. 284, 219-227. [3] Stracke, et al. (2005) Geochem., Geophys., Geosys. 6, doi:10.1029/2004GC000824. [4] Burton et al., Earth Planet. Sci. Lett. (1999) 172, 311-322. [5] Alard et al., (2002) Earth Planet. Sci. Lett. 203, 651-663

Correlation of Comet 67P/CG'S Morphology with the Occurrence of Exposed Water Ice Patches

NASA Astrophysics Data System (ADS)

Arnold, G.; Weller, D.; Zeilinger, G.; Kappel, D.; Hviid, S.; Kührt, E.; Moroz, L. V.; Markus, K.; Henckel, D.; Capaccioni, F.; Filacchione, G.; Erard, S.; Bockelee-Morvan, D.

2017-04-01

Introduction: Comet 67P's surface is quite homogeneously covered by dark refractory materials rich in organics [1,2]. Rare water ice expo- sures on the surface, most likely originating from sub-surface layers, have recently been discovered [3,4]. Such H2O ice patches on 67P's Imhotep region in the pre-perihelion phase were ex- amined and related to the local morphology to understand the exposure mechanisms [5]. Methods: H2O ice was identified in two study areas using characteristic H2O spectral features observed by the VIRTIS-M instrument [1]: absorption bands at 1.04, 1.25, 1.52, 2.02, 2.96 μm, and the VIS spectral slope (0.5-0.8 μm). Corresponding normalized spectral indicators were projected onto a 3D digital shape model (DSM) of 67P [6], along with high spatial resolution images acquired by OSIRIS [7] for morphological context. Results and conclusions: The 2.0-μm absorption band proved to be the most sensitive H2O indicator in the IR. Flat (bluer) normalized VIS slopes correlate very well with depths of H2O ice absorption bands. The DSM projections show a significant spatial correlation between spectral H2O indicators and morphological features. H2O ice deposits were identified in two areas, each extending over hundreds of square meters. Both are located at the bases of steep-sloped (>60°) walls of Consolidated Cometary Material (CCM) on debris falls that came to rest on moderately inclined (20°-30°) terrain, pointing towards gravitational lows. Both deposits are located in poorly illuminated areas due to shadowing from close-by steep walls. The morphological and photometrical properties of these deposits appear to be stable over months. Spectral modeling [3,4] indicated the presence of large (mm-sized) H2O ice grains. Such grains form through vapor diffusion in ice-rich colder layers or by sintering and are exposed by erosion [3]. The CCM in both study areas was fractured and weakened by thermal fatigue and sublimation, leading to the collapse of overhangs in one single event or in small steps over a longer time. For study area 1 this interpretation is supported by a small remnant H2O ice patch in the upper part of the steep wall indicating the original location of the collapse overhang. Sinkhole-structures on the CCM in study area 2 indicate sub-surface activity connected to ice sublimation, thermal stress, and occasional outbursts. Even though the nucleus structure probably is mostly homogeneous and primordial, the variable size and irregular distribution of sink-holes and erosional features strongly imply a highly active and heterogeneous sub-surface layer of at least tens of meters [8,9]. References: [1] Capaccioni F. et al. (2015) Sci- ence, 347, 628. [2] Quirico E. et al. (2016) Ica- rus, 272, 32-47. [3] Filacchione G. et al. (2016) Nature, 529, 368-372. [4] Barucci A. et al. (2016) A&A, 595, A102. [5] Weller D. (2016) Master thesis, University of Potsdam. [6] Preusker F. et al. (2015) A&A, 583, A33. [7] Keller H. et al. (2007) Space Sci. Rev., 128(1), 433-506. [8] Thomas N. et al. (2015) Science, 347, 440. [9] Vincent J.B. et al. (2015) Nature, 523, 63-66.

Ion Acceleration in Solar Flares Determined by Solar Neutron Observations

NASA Astrophysics Data System (ADS)

Watanabe, K.; Solar Neutron Observation Group

2013-05-01

Large amounts of particles can be accelerated to relativistic energy in association with solar flares and/or accompanying phenomena (e.g., CME-driven shocks), and they sometimes reach very near the Earth and penetrate the Earth's atmosphere. These particles are observed by ground-based detectors (e.g., neutron monitors) as Ground Level Enhancements (GLEs). Some of the GLEs originate from high energy solar neutrons which are produced in association with solar flares. These neutrons are also observed by ground-based neutron monitors and solar neutron telescopes. Recently, some of the solar neutron detectors have also been operating in space. By observing these solar neutrons, we can obtain information about ion acceleration in solar flares. Such neutrons were observed in association with some X-class flares in solar cycle 23, and sometimes they were observed by two different types of detectors. For example, on 2005 September 7, large solar neutron signals were observed by the neutron monitor at Mt. Chacaltaya in Bolivia and Mexico City, and by the solar neutron telescopes at Chacaltaya and Mt. Sierra Negra in Mexico in association with an X17.0 flare. The neutron signal continued for more than 20 minutes with high statistical significance. Intense gamma-ray emission was also registered by INTEGRAL, and by RHESSI during the decay phase. We analyzed these data using the solar-flare magnetic-loop transport and interaction model of Hua et al. (2002), and found that the model could successfully fit the data with intermediate values of loop magnetic convergence and pitch angle scattering parameters. These results indicate that solar neutrons were produced at the same time as the gamma-ray line emission and that ions were continuously accelerated at the emission site. In this paper, we introduce some of the solar neutron observations in solar cycle 23, and discuss the tendencies of the physical parameters of solar neutron GLEs, and the energy spectrum and population of the accelerated particles produced in these solar flares, etc. We also report recent solar neutron observations by the Space Environment Data Acquisition equipment-Attached Payload (SEDA-AP) which has been installed on the international space station, and introduce the plan for the new solar neutron detector of the SciBar for the Cosmic Ray Telescope (SciCRT) at Mt. Sierra Negra in Mexico.

Methods of editing cloud and atmospheric layer affected pixels from satellite data

NASA Technical Reports Server (NTRS)

Nixon, P. R. (Principal Investigator); Wiegand, C. L.; Richardson, A. J.; Johnson, M. P.

1981-01-01

Plotted transects made from south Texas daytime HCMM data show the effect of subvisible cirrus (SCI) clouds in the emissive (IR) band but the effect is unnoticable in the reflective (VIS) band. The depression of satellite indicated temperatures ws greatest in the center of SCi streamers and tapered off at the edges. Pixels of uncontaminated land and water features in the HCMM test area shared identical VIS and IR digital count combinations with other pixels representing similar features. A minimum of 0.015 percent repeats of identical VIS-IR combinations are characteristic of land and water features in a scene of 30 percent cloud cover. This increases to 0.021 percent of more when the scene is clear. Pixels having shared VIS-IR combinations less than these amounts are considered to be cloud contaminated in the cluster screening method. About twenty percent of SCi was machine indistinguishable from land features in two dimensional spectral space (VIS vs IR).

Performance evaluation of different diamond-like carbon samples as charge state conversion surfaces for neutral atom imaging detectors in space applications

NASA Astrophysics Data System (ADS)

Brigitte Neuland, Maike; Allenbach, Marc; Föhn, Martina; Wurz, Peter

2017-04-01

The detection of energetic neutral atoms is a substantial requirement on every space mission mapping particle populations of a planetary magnetosphere or plasma of the interstellar medium. For imaging neutrals, these first have to be ionised. Regarding the constraints of weight, volume and power consumption, the technique of surface ionisation complies with all specifications of a space mission. Particularly low energy neutral atoms, which cannot be ionised by passing through a foil, are ionised by scattering on a charge state conversion surface [1]. Since more than 30 years intense research work is done to find and optimise suitable materials for use as charge state conversion surfaces for space application. Crucial parameters are the ionisation efficiency of the surface material and the scattering properties. Regarding these parameters, diamond-like carbon was proven advantageously: While efficiently ionising incoming neutral atoms, diamond stands out by its durability and chemical inertness [2]. In the IBEX-Lo sensor, a diamond-like carbon surface is used for ionisation of neutral atoms. Building on the successes of the IBEX mission [3], the follow up mission IMAP (InterstellarMApping Probe) will take up to further explore the boundaries of the heliosphere. The IMAP mission is planned to map neutral atoms in a larger energy range and with a distinct better angular resolution and sensitivity than IBEX [4]. The aspired performance of the IMAP sensors implies also for charge state conversion surfaces with improved characteristics. We investigated samples of diamond-like carbon, manufactured by the chemical vapour deposition (CVD) method, regarding their ionisation efficiency, scattering and reflexion properties. Experiments were carried out at the ILENA facility at the University of Bern [5] with hydrogen and oxygen atoms, which are the species of main interest in magnetospheric research [1]. We compare the results of earlier investigations of a metallised CVD sample [6] to our latest measurements of a Boron-doped CVD diamond sample. We additionally measured the B-concentration in the sample to prove our predictions of the B-concentration needed to reach sufficient conductibility for the sample not getting electrostatically charged during instrument operation. The results of narrower scattering cones and higher ionisation efficiency show that diamond-like carbon still is the preferred material for charge state conversion surfaces and that new surface technologies offer improved diamond conversion surfaces with different properties and hence the possibility for improvement of the performance of neutral atom imaging instruments. References: [1] P. Wurz, Detection of Energetic Neutral Atoms, in The Outer Heliosphere: Beyond the Planets, Copernicus Gesellschaft e.V., Katlenburg-Lindau, Germany, 2000, p. 251-288. [2] P. Wurz, R. Schletti, M.R. Aellig, Surf. Sci. 373(1997), 56-66. [3] D.J. McComas et al., Geophys. Res. Lett. 38(2011), L18101. [4] N.A. Schwadron et al., J. of Phys.. Conf. Series 767(2016): 012025 [5] P. Wahlström, J.A. Scheer, A. Riedo, P. Wurz and M. Wieser, J. Spacecr. Rockets 50 (2013): 402-410. [6] M.B. Neuland, J.A. Scheer, A. Riedo and P. Wurz, Appl. Surf. Sci. 313(2014):293-303.

JANUS: the visible camera onboard the ESA JUICE mission to the Jovian system

NASA Astrophysics Data System (ADS)

Palumbo, Pasquale; Jaumann, Ralf; Cremonese, Gabriele; Hoffmann, Harald; Debei, Stefano; Della Corte, Vincenzo; Holland, Andrew; Lara, Luisa Maria

2014-05-01

The JUICE (JUpiter ICy moons Explorer) mission [1] was selected in May 2012 as the first Large mission in the frame of the ESA Cosmic Vision 2015-2025 program. JUICE is now in phase A-B1 and its final adoption is planned by late 2014. The mission is aimed at an in-depth characterization of the Jovian system, with an operational phase of about 3.5 years. Main targets for this mission will be Jupiter, its satellites and rings and the complex relations within the system. Main focus will be on the detailed investigation of three of Jupiter's Galilean satellites (Ganymede, Europa, and Callisto), thanks to several fly-bys and 9 months in orbit around Ganymede. JANUS (Jovis, Amorum ac Natorum Undique Scrutator) is the camera system selected by ESA to fulfill the optical imaging scientific requirements of JUICE. It is being developed by a consortium involving institutes in Italy, Germany, Spain and UK, supported by respective Space Agencies, with the support of Co-Investigators also from USA, France, Japan and Israel. The Galilean satellites Io, Europa, Ganymede and Callisto show an increase in geologic activity with decreasing distance to Jupiter [e.g., 2]. The three icy Galilean satellites Callisto, Ganymede and Europa show a tremendous diversity of surface features and differ significantly in their specific evolutionary paths. Each of these moons exhibits its own fascinating geologic history - formed by competition and also combination of external and internal processes. Their origins and evolutions are influenced by factors such as density, temperature, composition (volatile compounds), stage of differentiation, volcanism, tectonism, the rheological reaction of ice and salts to stress, tidal effects, and interactions with the Jovian magnetosphere and space. These interactions are still recorded in the present surface geology. The record of geological processes spans from possible cryovolcanism through widespread tectonism to surface degradation and impact cratering. Observation of the Jupiter atmosphere, satellite's exo-spheres, Jupiter ring system, minor satellites and Ganymede rotational status are additional important objec-tives shared with other JUICE instruments. JANUS will allow orders-of-magnitude steps ahead in terms of coverage and/or resolution and/or time evolution on many targets in Jupiter system. JANUS ground sampling ranges from 400 m/pixel to < 3 m/pixel for the three main Galilean satellites, and from few to few tens of km/pixel for Jupiter and the other targets in the Jovian system. Assuming the available scientific data volume (about 20% allocated to JANUS out of 1.4 Gb/day during operations), JANUS observations will cover about 100% of Ganymede in 4 colours at 400 m/pixel. About 3% of the surface of Ganymede will be covered with sampling better than 24 m/pixel and 60 targeted areas will be observed with best sampling of about 3 m/pixel. This will represent a dramatic improvement with respect to Galileo coverage. References: [1] Grasset O. et al. (2013) Planet. and Space Sci 78, 1-21. [2] Stephan K. et al.(2013) The Science of Solar System Ices, M. S. Gutipati and J. Castillo-Rogez editors. Astrophys. and Space Sci. Libr. 356, 279 - 367.

Investigation of detection conditions of captured microbes in space with PCR Microbes capture experiment on ISS proposed in "Tanpopo" mission

NASA Astrophysics Data System (ADS)

Kawaguchi, Yuko; Sugino, Tomohiro; Yang, Yinjie; Yoshimura, Yoshitaka; Tsuji, Takashi; Kobayashi, Kensei; Tabata, Makoto; Hashimoto, Hirofumi; Mita, Hajime; Imai, Eiichi; Kawai, Hideyuki; Okudaira, Kyoko; Hasegawa, Sunao; Yamashita, Masamichi; Yano, Hajime; Yokobori, Shin-Ichi; Yamagishi, Akihiko

Terrestrial life may fly off into outer space by volcanic eruption meteorological impacts, and so on. Microbes have been collected from high altitude up to 70 km since 1936 [1]. We also isolated microbes at high altitude up to 35 km using an airplane and balloons [2, 3]. The two isolates of these microbes are new species, one of which shows higher UV ray tolerance than Deinococcus radiodurans [2, 3]. On the other hand, there is a hypothesis on the origin of terrestrial life called panspermia [4, 5], in which terrestrial life is thought to have come from space (or astronomical bodies other than Earth). This hypothesis suggests that life may migrate between Earth and other planets. If microbes were to exist at the high altitude of low earth orbit (400 km), it would endorse the possibility of interplanetary migration of terrestrial lifeWe proposed, the Tanpopo mission to examine interplanetary migration of microbes and organic compounds on Japan Experimental Module (JEM) of the International Space Station (ISS). We will capture micro-particles including microbes and micro-meteoroids at the altitude of ISS orbit (400 km) with ultra low-density aerogel exposed to space for a given period of time. After retreaving the aerogel, we will investigate captured micro particles and tracks followed by microbiological, organic chemical and mineralogical analyses.Captured particles will be analyzed after the initial curation of the aerogel and tracks. Particles potentially containing microbes will be used for PCR amplification of small subunit (ss) rRNA gene followed by DNA sequencing. Comparision between the determined sequences and known ss rRNA gene sequences of terrestrial organisms will suggest the origin and properties of the organism.The density of microbes at the ISS altitude might be quite low, and microbe cell number on each captured particle may be quite limited. Therefore, it is necessary to establish the effective PCR procedure for quite small amount of DNA template in the presence of other materials such as clay and aerogel.We will report current status of the PCR identification of microbes from test samples. The PCR conditions to amplify ss rRNA gene from quite small number of cells and quite low concentration of genomic DNA with/without clay and aerogel are examined. References. [1] Y. Yang et al. (2009) Biol. Sci. in Space, 23, 151-163[2] Y. Yang et al. (2009) Int. J. Syst. Evol. Microbiol, 59, 1862-1866[3] Y. Yang et al. (2010) Int. J. Syst. Evol. Microbiol, (in press)[4] S. Arrhenius (1908) Worlds in the Making-the Evolution of the Universe. Harper and Brothers Publishers.[5] F. Crick (1981) Life Itself. Simon Schuster.

Le Carbonifère du Maroc central : les formations de Migoumess, de Tirhela et d'Idmarrach. Lithologie, biostratigraphie et conséquences géodynamiquesThe Carboniferous formations of Migoumess, Tirhela and Idmarrach (central Morocco): lithology, biostratigraphy and geodynamic consequences

NASA Astrophysics Data System (ADS)

Berkhli, Mostafa; Vachard, Daniel

2002-01-01

New biostratigraphical data based on foraminifers, algae and pseudo-algae indicate that the limestone pebbles of the channelized polygenic conglomerates of the Migoumess formation contain Late Visean (V3b γ-V3c) assemblages. That confirms the Westphalian age attributed to this formation by Hollard [Zdt. Geol. Ges. 129 (1978) 495-512]. The Tournaisian age assigned to it by palynology [C. R. Acad. Sci. Paris, série II 310 (1990) 1573-1576] cannot be retained. The Tirhela formation, Late Visean and Serpukhovian (E1) in age, is coeval with the Akerchi formation [Berkhli, thèse d'État, 1999; Berkhli et al., J. Afr. Earth Sci. (accepté)]. The Idmarrach formation, mapped as a thrust sheet [C. R. Acad. Sci. Paris, série II 310 (1990) 1573-1576], is dated as Serpukhovian (E1) and its thrusting is consequently post-Serpukhovian. Palaeogeographic and geodynamic consequences are listed. To cite this article: M. Berkhli, D. Vachard, C. R. Geoscience 334 (2002) 67-72

Exposure Histories of Calcalong Creek and LEW 88516 Meteorites

NASA Astrophysics Data System (ADS)

Nishiizumi, K.; Arnold, J. R.; Caffee, M. W.; Finkel, R. C.; Southon, J.

1992-07-01

We report here preliminary results of cosmogenic radionuclides in lunar meteorite Calcalong Creek and shergottite LEW 88516 for study of exposure histories. Table 1 shows ^36Cl and ^10Be results for these two meteorites along with previous measurements of ^36Cl and ^10Be of SNC meteorites. The AMS measurements were performed at LLNL. Measured ^36Cl activities, in dpm/kg meteorite, were normalized to the target element concentration, dpm/kg (8Ca+Fe), for comparison and shown in the table. The ^36Cl saturation activity is ~22 +- 2 dpm/kg (8Ca+Fe) for 4-pi irradiation. Calcalong Creek: This is the first lunar meteorite found outside Antarctica (Hill et al., 1991; Marvin and Holmberg, 1992). ^36Cl and ^10Be activity levels are slightly (10-20%) higher than the production rate of these nuclides on the moon. One possibility is that the meteorite was ejected from near the surface (<70 g/cm^2) of the moon and transferred to the earth. The transition time from moon to earth was ~0.2 My. The other simple case is that the meteorite was ejected from deep (at least a few meters) in the moon, like Yamato 82192, and exposed to cosmic rays as a small body. The transition time in this case was ~2 My. The terrestrial age must be <70 ky for either case. Other cosmogenic nuclide measurements (in progress) are required to constrain the history further. LEW 88516: This meteorite was classified as a shergottite (Mason, 1991). The recovered mass is 13.2 g. We measured ^36Cl and ^10Be in 93.9 mg of homogenized bulk sample. All aspects of petrography and bulk chemical composition of LEW 88516 are remarkably similar to those of ALH 77005 (Boynton et al., 1992; Lindstrom et al., 1992). Since the ^10Be activities of ALH 77005 samples vary from 13.7 to 16.2 dpm/kg with increasing shielding depth (Nishiizumi et al., 1986a), the average of ^10Be in ALH 77005 is slightly lower than ^10Be in LEW 88516. The calculated ^10Be exposure age is ~3.0 My. The normalized ^36Cl activity of LEW 88516 is near saturation for a small object (no significant thermal neutron effect). On this assumption, the terrestrial age of the meteorite is shorter than 50 ky. The ^36Cl terrestrial age of ALH 77005 is ~0.2 My and in good agreement with the ^81Kr terrestrial age of (0.19 +- 0.07) My (Schultz and Freundel, 1986). LEW 88516 and ALH 77005 are separate falls. Probably, however, these two meteorites and Shergotty were ejected in the same event on the parent body, since they have same exposure age within error. Table 1, which in the hard copy appears here, shows the concentration of ^36Cl and ^10Be. References: Boynton W. V. et al. (1992) Lunar Planet. Sci. XXIII, 147-148. Hill D. H. et al. (1991) Nature 352, 614-617. Lindstrom M. M. et al. (1992) Lunar Planet. Sci. XXIII, 783-784. Marvin U. B. and Holmberg B. B. (1992) Lunar Planet. Sci. XXIII, 849- 850. Mason B. (1991) Antarctic Meteorite Newsletter 14 (2), 19. Nishiizumi K. et al. (1986a) Meteoritics 21, 472-473. Nishiizumi K. et al. (1986b) Geochim. Cosmochim. Acta 50, 1017- 1021. Pal D. K. et al. (1986) Geochim. Cosmochim. Acta 50, 2405-2409. Schultz L. and Freundel M. (1984) Meteoritics 19, 310.

Label-free carbon particulates detection in bio (medical) settings (Conference Presentation)

NASA Astrophysics Data System (ADS)

Steuwe, Christian; Bové, Hannelore; vandeVen, Martin J.; Ameloot, Marcel; Roeffaers, Maarten B. J.

2017-02-01

The adverse health effects of particulate matter exposure are a generally accepted concern. Dramatic statistical figures suggest that fine dust is a main environmental risk in Europe and can be held accountable for hundreds of thousands of deaths per year [1]. Locating and tracking these nanometer sized particles, however, is not straight forward: In epidemiological and toxicology research only measurements based on labels [2] such as radionuclide markers have been applied. In this paper we present a direct, label-free optical contrast mechanism to detect carbon nanoparticles immersed in aqueous environments [3]. The virtue of this technique is its ability to perform in body fluids such as urine but also in cells and tissues. The mechanism is based on white light (WL) generation upon illumination with femtosecond pulsed near-infrared and is therefore non-incandescence related. We demonstrate the technique in various biological settings with dry and suspended carbon black particles (CB), a widely used model compound for soot [4]. Our approach allows for the unequivocal localization of CB alongside of common fluorophores and markers and can be performed on multiphoton laser-scanning microscopy platforms, a system commonly available in research laboratories. [1] European Environment Agency (2015). Press release. [2] Kong et al. Int. J. Mol. Sci. 2013, 14, (11), 22529-22543 [3] Bové and Steuwe et al. Nano letters, 2016, (16) , pages 3173-3178 [4] Arnal et al. Combust. Sci. Technol. 2012, 184, (7-8), 1191-1206.

Application of remote sensing and geographical information system for generation of runoff curve number

NASA Astrophysics Data System (ADS)

Meshram, S. Gajbhiye; Sharma, S. K.; Tignath, S.

2017-07-01

Watershed is an ideal unit for planning and management of land and water resources (Gajbhiye et al., IEEE international conference on advances in technology and engineering (ICATE), Bombay, vol 1, issue 9, pp 23-25, 2013a; Gajbhiye et al., Appl Water Sci 4(1):51-61, 2014a; Gajbhiye et al., J Geol Soc India (SCI-IF 0.596) 84(2):192-196, 2014b). This study aims to generate the curve number, using remote sensing and geographical information system (GIS) and the effect of slope on curve number values. The study was carried out in Kanhaiya Nala watershed located in Satna district of Madhya Pradesh. Soil map, Land Use/Land cover and slope map were generated in GIS Environment. The CN parameter values corresponding to various soil, land cover, and land management conditions were selected from Natural Resource Conservation Service (NRCS) standard table. Curve number (CN) is an index developed by the NRCS, to represent the potential for storm water runoff within a drainage area. The CN for a drainage basin is estimated using a combination of land use, soil, and antecedent soil moisture condition (AMC). In present study effect of slope on CN values were determined. The result showed that the CN unadjusted value are higher in comparison to CN adjusted with slope. Remote sensing and GIS is very reliable technique for the preparation of most of the input data required by the SCS curve number model.

Understanding the limits of Marxist approaches to sociocultural studies of science education

NASA Astrophysics Data System (ADS)

Lima, Paulo; Ostermann, Fernanda; Rezende, Flavia

2014-12-01

In the first three sections of this paper we comment on some of the ideas developed in the forum papers, pointing out possible misunderstandings and constructing new explanations that clarify arguments we made in the original article. In the last section we expand the discussion raised in the original paper, elaborating on the limits of the use of Marxist approaches to sociocultural studies of science education. Following insights suggested by Loxley et al. (Cult Stud Sci Educ. doi: 10.1007/s11422-013-9554-z, 2013) and detailed by Zuss (Cult Stud Sci Educ. doi: 10.1007/s11422-013-9555-y, 2014) on the commodification of knowledge, we sketch an analysis of how knowledge is transformed into capital to understand why contemporary scholars are likely to be engaged in a relation of production that resembles capitalist exploitation.

Assembling Large, Multi-Sensor Climate Datasets Using the SciFlo Grid Workflow System

NASA Astrophysics Data System (ADS)

Wilson, B. D.; Manipon, G.; Xing, Z.; Fetzer, E.

2008-12-01

NASA's Earth Observing System (EOS) is the world's most ambitious facility for studying global climate change. The mandate now is to combine measurements from the instruments on the A-Train platforms (AIRS, AMSR-E, MODIS, MISR, MLS, and CloudSat) and other Earth probes to enable large-scale studies of climate change over periods of years to decades. However, moving from predominantly single-instrument studies to a multi-sensor, measurement-based model for long-duration analysis of important climate variables presents serious challenges for large-scale data mining and data fusion. For example, one might want to compare temperature and water vapor retrievals from one instrument (AIRS) to another instrument (MODIS), and to a model (ECMWF), stratify the comparisons using a classification of the cloud scenes from CloudSat, and repeat the entire analysis over years of AIRS data. To perform such an analysis, one must discover & access multiple datasets from remote sites, find the space/time matchups between instruments swaths and model grids, understand the quality flags and uncertainties for retrieved physical variables, and assemble merged datasets for further scientific and statistical analysis. To meet these large-scale challenges, we are utilizing a Grid computing and dataflow framework, named SciFlo, in which we are deploying a set of versatile and reusable operators for data query, access, subsetting, co-registration, mining, fusion, and advanced statistical analysis. SciFlo is a semantically-enabled ("smart") Grid Workflow system that ties together a peer-to-peer network of computers into an efficient engine for distributed computation. The SciFlo workflow engine enables scientists to do multi-instrument Earth Science by assembling remotely-invokable Web Services (SOAP or http GET URLs), native executables, command-line scripts, and Python codes into a distributed computing flow. A scientist visually authors the graph of operation in the VizFlow GUI, or uses a text editor to modify the simple XML workflow documents. The SciFlo client & server engines optimize the execution of such distributed workflows and allow the user to transparently find and use datasets and operators without worrying about the actual location of the Grid resources. The engine transparently moves data to the operators, and moves operators to the data (on the dozen trusted SciFlo nodes). SciFlo also deploys a variety of Data Grid services to: query datasets in space and time, locate & retrieve on-line data granules, provide on-the-fly variable and spatial subsetting, and perform pairwise instrument matchups for A-Train datasets. These services are combined into efficient workflows to assemble the desired large-scale, merged climate datasets. SciFlo is currently being applied in several large climate studies: comparisons of aerosol optical depth between MODIS, MISR, AERONET ground network, and U. Michigan's IMPACT aerosol transport model; characterization of long-term biases in microwave and infrared instruments (AIRS, MLS) by comparisons to GPS temperature retrievals accurate to 0.1 degrees Kelvin; and construction of a decade-long, multi-sensor water vapor climatology stratified by classified cloud scene by bringing together datasets from AIRS/AMSU, AMSR-E, MLS, MODIS, and CloudSat (NASA MEASUREs grant, Fetzer PI). The presentation will discuss the SciFlo technologies, their application in these distributed workflows, and the many challenges encountered in assembling and analyzing these massive datasets.

Assembling Large, Multi-Sensor Climate Datasets Using the SciFlo Grid Workflow System

NASA Astrophysics Data System (ADS)

Wilson, B.; Manipon, G.; Xing, Z.; Fetzer, E.

2009-04-01

NASA's Earth Observing System (EOS) is an ambitious facility for studying global climate change. The mandate now is to combine measurements from the instruments on the "A-Train" platforms (AIRS, AMSR-E, MODIS, MISR, MLS, and CloudSat) and other Earth probes to enable large-scale studies of climate change over periods of years to decades. However, moving from predominantly single-instrument studies to a multi-sensor, measurement-based model for long-duration analysis of important climate variables presents serious challenges for large-scale data mining and data fusion. For example, one might want to compare temperature and water vapor retrievals from one instrument (AIRS) to another instrument (MODIS), and to a model (ECMWF), stratify the comparisons using a classification of the "cloud scenes" from CloudSat, and repeat the entire analysis over years of AIRS data. To perform such an analysis, one must discover & access multiple datasets from remote sites, find the space/time "matchups" between instruments swaths and model grids, understand the quality flags and uncertainties for retrieved physical variables, assemble merged datasets, and compute fused products for further scientific and statistical analysis. To meet these large-scale challenges, we are utilizing a Grid computing and dataflow framework, named SciFlo, in which we are deploying a set of versatile and reusable operators for data query, access, subsetting, co-registration, mining, fusion, and advanced statistical analysis. SciFlo is a semantically-enabled ("smart") Grid Workflow system that ties together a peer-to-peer network of computers into an efficient engine for distributed computation. The SciFlo workflow engine enables scientists to do multi-instrument Earth Science by assembling remotely-invokable Web Services (SOAP or http GET URLs), native executables, command-line scripts, and Python codes into a distributed computing flow. A scientist visually authors the graph of operation in the VizFlow GUI, or uses a text editor to modify the simple XML workflow documents. The SciFlo client & server engines optimize the execution of such distributed workflows and allow the user to transparently find and use datasets and operators without worrying about the actual location of the Grid resources. The engine transparently moves data to the operators, and moves operators to the data (on the dozen trusted SciFlo nodes). SciFlo also deploys a variety of Data Grid services to: query datasets in space and time, locate & retrieve on-line data granules, provide on-the-fly variable and spatial subsetting, perform pairwise instrument matchups for A-Train datasets, and compute fused products. These services are combined into efficient workflows to assemble the desired large-scale, merged climate datasets. SciFlo is currently being applied in several large climate studies: comparisons of aerosol optical depth between MODIS, MISR, AERONET ground network, and U. Michigan's IMPACT aerosol transport model; characterization of long-term biases in microwave and infrared instruments (AIRS, MLS) by comparisons to GPS temperature retrievals accurate to 0.1 degrees Kelvin; and construction of a decade-long, multi-sensor water vapor climatology stratified by classified cloud scene by bringing together datasets from AIRS/AMSU, AMSR-E, MLS, MODIS, and CloudSat (NASA MEASUREs grant, Fetzer PI). The presentation will discuss the SciFlo technologies, their application in these distributed workflows, and the many challenges encountered in assembling and analyzing these massive datasets.

Networks and Models with Heterogeneous Population Structure in Epidemiology

NASA Astrophysics Data System (ADS)

Kao, R. R.

Heterogeneous population structure can have a profound effect on infectious disease dynamics, and is particularly important when investigating “tactical” disease control questions. At times, the nature of the network involved in the transmission of the pathogen (bacteria, virus, macro-parasite, etc.) appears to be clear; however, the nature of the network involved is dependent on the scale (e.g. within-host, between-host, or between-population), the nature of the contact, which ranges from the highly specific (e.g. sexual acts or needle sharing at the person-to-person level) to almost completely non-specific (e.g. aerosol transmission, often over long distances as can occur with the highly infectious livestock pathogen foot-and-mouth disease virus—FMDv—at the farm-to-farm level, e.g. Schley et al. in J. R. Soc. Interface 6:455-462, 2008), and the timescale of interest (e.g. at the scale of the individual, the typical infectious period of the host). Theoretical approaches to examining the implications of particular network structures on disease transmission have provided critical insight; however, a greater challenge is the integration of network approaches with data on real population structures. In this chapter, some concepts in disease modelling will be introduced, the relevance of selected network phenomena discussed, and then results from real data and their relationship to network analyses summarised. These include examinations of the patterns of air traffic and its relation to the spread of SARS in 2003 (Colizza et al. in BMC Med., 2007; Hufnagel et al. in Proc. Natl. Acad. Sci. USA 101:15124-15129, 2004), the use of the extensively documented Great Britain livestock movements network (Green et al. in J. Theor. Biol. 239:289-297, 2008; Robinson et al. in J. R. Soc. Interface 4:669-674, 2007; Vernon and Keeling in Proc. R. Soc. Lond. B, Biol. Sci. 276:469-476, 2009) and the growing interest in combining contact structure data with phylogenetics to identify real contact patterns as they directly relate to diseases of interest (Cottam et al. in PLoS Pathogens 4:1000050, 2007; Hughes et al. in PLoS Pathogens 5:1000590, 2009).

Chronology of magmatic and biological events during mass extinctions

NASA Astrophysics Data System (ADS)

Schaltegger, U.; Davies, J.; Baresel, B.; Bucher, H.

2016-12-01

For mass extinctions, high-precision geochronology is key to understanding: 1) the age and duration of mass extinction intervals, derived from palaeo-biodiversity or chemical proxies in marine sections, and 2) the age and duration of the magmatism responsible for injecting volatiles into the atmosphere. Using high-precision geochronology, here we investigate the sequence of events linked to the Triassic-Jurassic boundary (TJB) and the Permian-Triassic boundary (PTB) mass extinctions. At the TJB, the model of Guex et al. (2016) invokes degassing of early magmas produced by thermal erosion of cratonic lithosphere as a trigger of climate disturbance in the late Rhaetian. We provide geochronological evidence that such early intrusives from the CAMP (Central Atlantic Magmatic Province), predate the end-Triassic extinction event (Blackburn et al. 2013) by 100 kyr (Davies et al., subm.). We propose that these early intrusions and associated explosive volcanism (currently unidentified) initiate the extinction, followed by the younger basalt eruptions of the CAMP. We also provide accurate and precise calibration of the PTB in marine sections in S. China: The PTB and the extinction event coincide within 30 kyr in deep water settings; a hiatus followed by microbial limestone deposition in shallow water settings is of <100 kyr duration. The PTB extinction interval is preceded by up to 300 kyr by the onset of partly alkaline explosive, extrusive and intrusive rocks, which are suggested as the trigger of the mass extinction, rather than the subsequent basalt flows of the Siberian Traps (Burgess and Bowring 2015). From temporal constraints, the main inferences that can be made are: The duration of extinction events is in the x10 kyr range during the initial intrusive activity of a Large Igneous Province, and is postdated by the majority of basalt flows over several 100 kyr. For modeling climate change associated with mass extinctions, volatiles released from the basalt flows may thus not be relevant. Initial igneous activity must be explosive for producing sufficient volumes of volatiles over a sufficiently long time that could generate climatic change. Baresel et al., submitted; Blackburn et al. 2013, Science; Burgess and Bowring 2015, Sci Advances; Davies et al., submitted; Guex et al., 2016, Sci. Rep.

A dual-porous, biophysical void structure model of soil for the understanding of the conditions causing nitrous oxide emission

NASA Astrophysics Data System (ADS)

Matthews, G. Peter; Maurizio Laudone, G.; Whalle, W. Richard; Bird, Nigel; Gregory, Andrew; Cardenas, Laura; Misselbrook, Tom

2010-05-01

Nitrous oxide is the fourth most important greenhouse gas. It is 300 times more potent than carbon dioxide, and two-thirds of anthropogenic nitrous oxide is emitted by agricultural land. This presentation will begin with a brief overview of the laboratory measurements of nitrous oxide emission from carefully characterised soils, presented in more detail by Cardenas et al.. The measurements were made in a twelve-chamber, gas chromatographic apparatus at North Wyke Research (formerly IGER). The presentation will then continue with a description of a void network model of sufficient accuracy and authenticity that it can be used to explain and predict the nitrous oxide production, and the modelling of the biological, chemical and physical processes for the production of nitrous oxide within the constructed network. Finally, conclusions will be drawn from a comparison of the model results with experiment. The void network model Nitrous oxide is produced by microbial activity located in ‘hotspots' within the microstructure of soil, and nutrients and gases flow or diffuse to and from these hotspots through the water or gas-filled macro-porosity. It is clear, therefore, that a network model to describe and explain nitrous oxide production must encompass the full size range of pore space active within the process, which covers 6 orders of magnitude, and must make realistic suppositions about the positional relationship of the hotspots relative to the soil macro-porosity. Previous experimental (Tsakiroglou, C. D. et al, European J.Soil Sci., 2008) and theoretical approaches to the modelling of soil void structure cannot generally meet these two requirements. We have therefore built on the success of the previous uni-porous model of soil (Matthews, G. P. et al, Wat.Resour.Res, 2010), and the concept of a critical percolation path, to develop a dual porous model (Laudone, G. M. et al, European J.Soil Sci., 2010) with the following features: • A porous unit cell, with periodic boundary conditions, and with a critical percolation path with the correct percolation characteristics and void volume of the macro-porosity of the soil. • A solid phase between the pores of the large unit cell, with the correct volume of the fraction of larger soil aggregates (larger 1 mm). • All the remaining pores of the large unit cell, which are not part of the critical percolation path, filled with smaller unit cells, which account for the micro-porosity of the soil sample. We describe the construction of a model that closely matches the following characteristics of a specific example of typical arable soil, taken from the Warren field of the Rothamsted experimental farm at Woburn, although the model can be used for a wide range of soils: (i) macroporosity and microporosity as measured by the water retention curve, (ii) the shape of the water retention characteristic under a wide range of tensions, (iii) the soil texture, and (iv) the extent of irreducible water content. Process model We will describe the insertion of Michaelis-Menten kinetics and Crank-Nicholson diffusion equations into the precisely scaled model, building on previous diffusion modelling (Laudone, G. M. et al, Chem.Eng.Sci., 2008). Comparison with experiment A comparison with experimental results sheds light on (i) the positional relationships of aerobic and anaerobic bacteria relative to the critical percolation path, (ii) the relationship between the critical percolation path and the preferential / critical flow path (Figure 4), (iii) the extent of ignorance about the reaction kinetics of some of the fundamental processes occurring, (iv) the soil conditions that cause nitrous oxide emission, and (v) the effect of soil compaction on the emission. Acknowledgement This presentation is a summary of the some of the work of the BBSRC funded U.K. soil research consortium "Soil Programme for Quality and Resilience" (BB/E001793/1 and others), of which Matthews is principal investigator.

Chemical Heterogeneity and Mineralogy of Halley's Dust

NASA Astrophysics Data System (ADS)

Schulze, H.; Kissel, J.

1992-07-01

It is commonly assumed that comets are pristine bodies which still contain relatively unaltered material from the beginning of our solar system. Therefore, in March 1986 the chemical composition of Halley's dust particles was investigated by time- of-flight mass spectrometers on board the Vega 1 & 2 and Giotto spacecraft using the high relative velocity of 70-80 km/s between spacecraft and Halley for the generation of ions by dust impact ionization (see e.g. Kissel, 1986; Jessberger et al., 1988). This paper investigates the overall chemical variation among the dust particles with special emphasis on rock-forming elements to derive a mineralogical model of the dust and to give constraints to the evolution of cometary and preplanetary matter. The interpretation is based on 123 selected spectra obtained by the mass spectrometer PUMA 1 on Vega 1. Selection criteria, interpretation of raw data and examined instrumental effects are described in more detail elsewhere (Schulze and Kissel, 1992). The bulk composition of Halley's dust is characterized for the rock-forming elements by cosmic abundances within the experimental uncertainty of factor two (see also Jessberger et al., 1988). A small systematic deviation of the abundances can be used for a revision of the ion yields. The volatile elements carbon and nitrogen, however, are significantly enriched to CI-chondrites. A histogram of the Mg/(Mg+Fe)-ratios shows typical peaks at about 0 and 1 which indicate separated phases for Mg and Fe and an anhydrous nature of the dust (e.g. Brownlee et al., 1987; Bradley, 1988). However, also a broad peak occurs at 0.5. Mg-rich spectra are characterized by an excellent Mg-Si correlation with a narrow range of Mg/Si ratios at about 1. Also oxygen is correlated with Mg and Si. Fe-rich spectra partly show a good Fe-S correlation. However, several spectra are rich only in Fe or S. A cluster analysis of the spectra regarding Na, Mg, Al, Si, S, Ca, and Fe revealed seven groups. These groups partly correspond to classifications of interplanetary dust particles (Brownlee et al., 1982). Half of the spectra have chondritic abundances within the experimental uncertainty. About 25% are dominated by Mg and Si indicating a significant portion of Fe-poor Mg silicates in the dust. Nearly 7% of the spectra are typically enriched in Fe and S due to pure Fe sulfide grains which seem to be partly enriched in Ni. Rarely, particles extremely rich in iron occur. Many silicatic spectra show a sulfur excess of unknown origin. Interpreting this heterogeneity in terms of mineralogy indicates that about half of Halley's dust grains are almost monomineralic and composed of Mg-rich silicates (enstatite and/or forsterite), Fe sulfides and Fe metal. Hydrated silicates and magnetite seem to play only a small role. The prevalence of minerals which were formed at rather high temperatures according to the condensation sequence (above ~600 K), is evidence that equilibration to Fe-rich and hydrated silicates by diffusion reactions at lower temperatures is a process too slow to affect these dust particles in their formation environment (Fegley and Prinn, 1988), and that these particles were not intensively altered at low temperatures in the comet. References: Bradley J.P. (1988) Geochim. Cosmochim. Acta. 52. 889-900. Brownlee D.E., Olszewski E., and Wheelock M.M. (1982) Lunar Planet. Sci. XIII, 71-72. Brownlee D.E., Wheelock M.M., Temple S., Bradley J.P., and Kissel J. (1987) Lunar Planet. Sci. XVIII, 134-135. Fegley B. and Prinn G. (1989) The formation and evolution of planetary systems (eds. H.A. Weaver and L. Danly), pp. 171-211. Cambridge. Jessberger E.K., Christoforidis A., and Kissel J. (1988) Nature 332, 691-695. Kissel J. (1986) Europ. Space Agency Spec. Publ. 1077, 67-83. Schulze H. and Kissel J. (1992) Earth Planet. Sci. Lett., submitted. Kissel J. and Krueger F.R. (1987) Appl. Phys. A42, 69-85.

MPF model ages of the Rembrandt basin and scarp system, Mercury.

NASA Astrophysics Data System (ADS)

Ferrari, Sabrina; Massironi, Matteo; Marchi, Simone; Byrne, Paul K.; Klimczak, Christian; Cremonese, Gabriele

2013-04-01

The 715-km-diameter Rembrandt basin is the largest well-preserved impact feature of the southern hemisphere of Mercury [1] (Fig. 1), and was imaged for the first time during the second flyby of the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission [2]. Much of the basin interior is covered by smooth, high-reflectance plains interpreted to be of volcanic origin [1-3] that host sets of contractional and extensional tectonic structures. Notably, Rembrandt basin and its smooth plains are cross-cut by a 1,000-km-long reverse fault system [1-5] that trends ~E-W, bending toward the north within the basin. The individual faults of this system accommodated crustal shortening that resulted from global contraction as Mercury's interior cooled [1]. The current shape of the reverse fault system may have been influenced by the formation of the Rembrandt basin [5]. The emplacement of the interior smooth plains predates both the basin-related tectonism and the final development of the giant scarp, which is suggestive of either short-lived volcanic activity immediately after basin formation or a later volcanic phase set against prolonged tectonic activity. In order to quantify the duration of volcanic and tectonic activity in and around Rembrandt basin, we determined the crater count-derived ages of the involved terrains by means of the Model Production Function (MPF) chronology of Mercury [6-8], which is rely on the knowledge of the impactors flux on the planet. Crater chronology allowed us to constrain the Rembrandt basin formation to the early Calorian period and a widespread resurfacing up to 3.5 Ga ago. The volcanic activity affected both the basin and its surroundings, but ended prior to some basin-related and regional faulting. Hence, if the giant scarp begun to develop even before the basin formation (as suggested by its length-displacement profile across the basin itself, [5]) the regional tectonic activity along this structure might have started even before the Late Heavy Bombardment period and lasted for more than 300 Ma, when the volcanic activity in this part of hermean surface was already accomplished. [1] Watters T. R. et al. (2009) Science, 324, 618. [2] Solomon S. C. et al. (2008) Science, 321, 59. [3] Denevi B. W. et al. (2009) Science, 324, 613. [4] Byrne P. K. et al. (2012) LPS, 43, abstract 1722. [5] Ferrari S. et al. (2012) EPSC, 7, abstract 2012-874. [6] Marchi S. et al. (2009) The Astron. Jour., 137, 4936. [7] Massironi M. et al. (2009) Geophys. Res. Lett., 36, L21204. [8] Marchi S. et al. (2011) Plaet. Space Sci., 59, 1968.

Governance of Cutaneous Photocarcinogenesis by Chronic UVA-Exposed Dermal Fibroblasts

DTIC Science & Technology

2014-09-01

UV lamp (Ted...repair of oxidative DNA damage and UV -induced photoproducts. Proc Natl Acad Sci USA 107:12180–5 RW Redmond et al. Bystander Oxidative Stress Due to UVA Irradiation 1090 Journal of Investigative Dermatology (2014), Volume 134 ...component of terrestrial UV radiation and is also the predominant constituent of indoor sunlamps, both of which have been shown to increase

Nutrient Recycling Impacts by Zebra Mussels in Harper’s Ferry Slough, Upper Mississippi River

DTIC Science & Technology

2000-12-01

ing pro duc tiv ity in the slough (also see Caraco et al. (1997)). In Harper’s Ferry Slough and other aquatic sys tems, the mag ni tude of ze bra mus...the Upper Mississippi River with zebra mussels (Dreissena polymorpha),” Environ. Sci. Technol. 33, 4385-4390. ERDC WQTN-PD-07 December 2000 11 Caraco , N

Combustion of Alane and Aluminum with Water for Hydrogen and Thermal Energy Generation

DTIC Science & Technology

2010-01-01

Herr, Green Rocket Propulsion by Reaction of Al and Mg Powders and Water, AIAA 2004-4037, 2004. [9] J.L. Sabourin , G.A. Risha, R.A. Yetter, S.F. Son...Wiley and Sons, Inc., 1992. [32] G.A. Risha, J.L. Sabourin , V. Yang, R.A. Yetter, S.F. Son, B.C. Tappan, Combust. Sci. Technol. 180 (2008) 2127–2142

Analysis of the application of the generalized monod kinetics model to describe the human corneal oxygen-consumption rate during soft contact lens wear.

PubMed

Compañ, V; Aguilella-Arzo, M; Del Castillo, L F; Hernández, S I; Gonzalez-Meijome, J M

2017-11-01

This work is an analysis of the application of the generalized Monod kinetics model describing human corneal oxygen consumption during soft contact lens wear to models previously used by Chhabra et al. (J Biomed Mater Res B Appl Biomater, 2009a;90:202-209, Optom Vis Sci 2009b;86:454-466) and Larrea and Büchler (Invest Ophthalmol Vis Sci 2009;50:1076-1080). We use oxygen tension from in vivo estimations provided by Bonanno [Bonanno et al., Invest Ophthalmol Vis Sci 2002;43:371-376, and Bonanno et al 2009]. We consider four hydrogel and six silicone hydrogel lenses. The cornea is considered a single homogeneous layer, with constant oxygen permeability regardless of the type of lens worn. Our calculations yield different values for the maximum oxygen consumption rate Q c,max , whith differents oxygen tensions (high and low p c ) at the cornea-tears interface. Surprisingly, for both models, we observe an increase in oxygen consumption near an oxygen tension of 105 mmHg until a maximum is reached, then decreasing for higher levels of oxygen pressure. That is, when lowering the pressure of oxygen, the parameter Q c,max initially increases depending on the intensity of the change in pressure. Which, it could be related with the variation of the pH. Furthermore, it is also noted that to greater reductions in pressure, this parameter decreases, possibly due to changes in the concentration of glucose related to the anaerobic respiration. The averaged in vivo human corneal oxygen consumption rate of 1.47 × 10 -4 cm 3 of O 2 /cm 3 tissue s, with Monod kinetics model, considering all the lenses studied, is smaller than the average oxygen consumption rate value obtained using the Larrea and Büchler model. The impact that these calculations have on the oxygen partial pressure available at different depths in the corneal tissue is presented and discussed, taking into consideration previous models used in this study. © 2016 Wiley Periodicals, Inc. J Biomed Mater Res Part B: Appl Biomater, 105B: 2269-2281, 2017. © 2016 Wiley Periodicals, Inc.

An updated protocol for a systematic review of implementation-related measures.

PubMed

Lewis, Cara C; Mettert, Kayne D; Dorsey, Caitlin N; Martinez, Ruben G; Weiner, Bryan J; Nolen, Elspeth; Stanick, Cameo; Halko, Heather; Powell, Byron J

2018-04-25

Implementation science is the study of strategies used to integrate evidence-based practices into real-world settings (Eccles and Mittman, Implement Sci. 1(1):1, 2006). Central to the identification of replicable, feasible, and effective implementation strategies is the ability to assess the impact of contextual constructs and intervention characteristics that may influence implementation, but several measurement issues make this work quite difficult. For instance, it is unclear which constructs have no measures and which measures have any evidence of psychometric properties like reliability and validity. As part of a larger set of studies to advance implementation science measurement (Lewis et al., Implement Sci. 10:102, 2015), we will complete systematic reviews of measures that map onto the Consolidated Framework for Implementation Research (Damschroder et al., Implement Sci. 4:50, 2009) and the Implementation Outcomes Framework (Proctor et al., Adm Policy Ment Health. 38(2):65-76, 2011), the protocol for which is described in this manuscript. Our primary databases will be PubMed and Embase. Our search strings will be comprised of five levels: (1) the outcome or construct term; (2) terms for measure; (3) terms for evidence-based practice; (4) terms for implementation; and (5) terms for mental health. Two trained research specialists will independently review all titles and abstracts followed by full-text review for inclusion. The research specialists will then conduct measure-forward searches using the "cited by" function to identify all published empirical studies using each measure. The measure and associated publications will be compiled in a packet for data extraction. Data relevant to our Psychometric and Pragmatic Evidence Rating Scale (PAPERS) will be independently extracted and then rated using a worst score counts methodology reflecting "poor" to "excellent" evidence. We will build a centralized, accessible, searchable repository through which researchers, practitioners, and other stakeholders can identify psychometrically and pragmatically strong measures of implementation contexts, processes, and outcomes. By facilitating the employment of psychometrically and pragmatically strong measures identified through this systematic review, the repository would enhance the cumulativeness, reproducibility, and applicability of research findings in the rapidly growing field of implementation science.

Effects of Composition and Iron Spin State on the Structural Transition of (Mg,Fe)CO3 in the Earth's Lower Mantle

NASA Astrophysics Data System (ADS)

Hsu, H.; Huang, S. C.; Wei, C. M.; Hsing, C. R.

2015-12-01

Iron-bearing magnesium carbonates (Mg,Fe)CO3 are believed the major carbon carriers in the Earth's deep lower mantle; they may play a crucial role in the Earth's deep carbon cycle. Knowledge of the physical and chemical properties of these carbonates is thus essential for our understanding of the mantle's role in global carbon cycle. Experiments have shown that (Mg,Fe)CO3 ferromagnesite (calcite structure) can be stable up to 80-100 GPa. At 45-50 GPa, ferromangsite undergoes a high-spin to low-spin transition, accompanied by a volume reduction and elastic anomalies. Starting ~100 GPa, ferromagnesite goes through a complicated structural transition. The detail of this transition and the atomic structures of high-pressure (Mg,Fe)CO3 phases are still highly debated. Experimental observations and theoretical results are inconsistent so far. In experiments, several distinct high-pressure (Mg,Fe)CO3 structures have been reported, including a P21/c phase [1] and a Pmm2 phase [2]. In theory, a C2/m phase [3] and a P-1 phase [4] have been suggested, while the Pmm2 phase is not found. One possible reason for such a discrepancy is that all available theoretical calculations so far are based on pure MgCO3, while experimental works are performed using (Mg,Fe)CO3 with high iron concentration ( > 50%). Clearly, the concentration of iron and the possible iron spin crossover can significantly affect the stability of these high-pressure (Mg,Fe)CO3 phases. Here, we use density functional theory + self-consistent Hubbard U (DFT+Usc) calculations to study this structural transition. The effects of composition and iron spin state on these (Mg,Fe)CO3 phases are also discussed. Our results can be expected to provide insightful information for better understanding the Earth's deep carbon cycle.[1] E. Boulard et al., Proc. Natl. Acad. Sci. USA 108, 5184 (2011).[2] J. Liu et al., Sci. Rep. 5, 7640 (2015). [3] A. R. Oganov et al., Earth Planet. Sci. Lett. 273, 38 (2008). [4] C. J. Pickard and R. J. Needs, Phys. Rev. B 91, 104101 (2015).

Erratum: Correction to: Soliton and shocks in pair ion plasma in presence of superthermal electron

NASA Astrophysics Data System (ADS)

Samanta, Utpal Kumar; Chatterjee, Prasanta; Nej, Monimala

2018-06-01

Correction to: Astrophys Space Sci (2013) 345:291-296 https://doi.org/10.1007/s10509-013-1403-8. There were typos in the last author's name in the original publication. The name is correctly shown here.

Kadomtsev-Petviashvili solitons propagation in a plasma system with superthermal and weakly relativistic effects

DOE Office of Scientific and Technical Information (OSTI.GOV)

Hafeez-Ur-Rehman; Mahmood, S.; Department of Physics and Applied Mathematics, PIEAS, Nilore, 44000 Islamabad

2011-12-15

Two dimensional (2D) solitons are studied in a plasma system comprising of relativistically streaming ions, kappa distributed electrons, and positrons. Kadomtsev-Petviashvili (KP) equation is derived through the reductive perturbation technique. Analytical solution of the KP equation has been studied numerically and graphically. It is noticed that kappa parameters of electrons and positrons as well as the ions relativistic streaming factor have an emphatic influence on the structural as well as propagation characteristics of two dimensional solitons in the considered plasma system. Our results may be helpful in the understanding of soliton propagation in astrophysical and laboratory plasmas, specifically the interactionmore » of pulsar relativistic wind with supernova ejecta and the transfer of energy to plasma by intense electric field of laser beams producing highly energetic superthermal and relativistic particles [L. Arons, Astrophys. Space Sci. Lib. 357, 373 (2009); P. Blasi and E. Amato, Astrophys. Space Sci. Proc. 2011, 623; and A. Shah and R. Saeed, Plasma Phys. Controlled Fusion 53, 095006 (2011)].« less

The new Electronic Grants Management System of the Space Telescope Science Institute

NASA Astrophysics Data System (ADS)

Beaser, R.; Wagner, E.

1999-12-01

The Space Telescope Science Institute has developed a new web-based Grants Management System which will be implemented at grantee institutions in the Spring of 2000. The system will feature on-line preparation and submission of budgets for all programs as well as e-mail notifications to Principal Investigators (PIs) and Authorizing Officials (AOs) of all Awards and Amendments. PDF versions of the documents will be available on the ST ScI web site. In addition, all financial and performance reports will be submitted via the web and grantees will be notified electronically of due and overdue reports. All administrative requests such as budget revisions, requests to extend the grant period, etc., will be submitted electronically to ST ScI. Detailed grant status information will be on-line and a variety of proposal and grant reports will be available to PIs and AOs. The system will also permit electronic routing of budgets and financial reports through the grantee institution.

Ways of Changing the Number and Size Distribution of Ecliptic Comets

NASA Astrophysics Data System (ADS)

Dones, Henry C. Luke; Womack, Maria; Alvarellos, Jose; Bierhaus, Edward B.; Bottke, William; Hamill, Patrick; Nesvorny, David; Robbins, Stuart J.; Zahnle, Kevin

2017-06-01

The existence of the Kuiper Belt was proposed because of the need for a low-inclination source for the Jupiter-family comets (JFCs). Indeed, the Kuiper Belt is thought to be the main reservoir of ecliptic comets (ECs), which include the JFCs and Centaurs. Ironically, we still do not know whether the belt, specifically its Scattered Disk, provides an adequate source for the ECs (Volk and Malhotra 2008). ECs are also thought to be the main source of Sun-orbiting impactors on the regular moons of the giant planets (Zahnle et al. 2003 [Z03]). Some models of the cometary orbital distribution used by Z03 and others to estimate impact rates assume comets are indestructible; in fact, many cometssplit, sometimes far from the Sun (Fernández 2009). Assuming shatterproof comets may lead to incorrect results for cometary orbital distributions. Other models impose a physical lifetime for bodies that approach within ~3 AU of the Sun, where sublimation of water ice begins, after which a comet is assumed to be dormant or disrupted (Nesvorný et al. 2017). In reality, some comets (e.g., 29P, Hale-Bopp) are active due to volatiles such as CO and CO2 beyond the orbit of Jupiter (Womack et al. 2017). 174P/Echeclus underwent a 7-magnitude outburst 13 AU from the Sun (Rousselot et al. 2016), and CO emission was recently detected from Echeclus at 6 AU (Wierzchos et al. 2017). We will estimate the effects of several mechanisms on the number and size distribution of comet nuclei as a function of distance from the Sun, including cometary activity and spontaneous disruption; tidal disruption by a giant planet, as happened for Shoemaker-Levy 9; and tidal disruption of binaries, which are numerous among "cold classical" Kuiper Belt Objects (Fraser et al. 2017). We thank the Cassini Data Analysis Program for support.Fernández Y (2009). Planet. Space. Sci. 57, 1218.Fraser WC, et al. (2017). Nat. Astron. 1, 0088.Nesvorný D, et al. (2017). In preparation.Rousselot P, et al. (2016). MNRAS 462, S432.Volk K, Malhotra R (2008). Astrophys. J. 687, 714.Wierzchos K, Womack M, Sarid G. (2017). Astron. J., in press.Womack M, Sarid G, Wierzchos, K (2017). Publ. Astron. Soc. Pac. 129, 031001.Zahnle K, et al. (2003). Icarus 163, 263.

Patient Monitoring

NASA Technical Reports Server (NTRS)

1978-01-01

In photo above, the electrocardiogram of a hospitalized patient is being transmitted by telemetry. Widely employed in space operations, telemetry is a process wherein instrument data is converted to electrical signals and sent to a receiver where the signals are reconverted to usable information. In this instance, heart readings are picked up by the electrode attached to the patient's body and delivered by wire to the small box shown, which is a telemetry transmitter. The signals are relayed wirelessly to the console in the background, which converts them to EKG data. The data is displayed visually and recorded on a printout; at the same time, it is transmitted to a central control station (upper photo) where a nurse can monitor the condition of several patients simultaneously. The Patient Monitoring System was developed by SCI Systems, Inc., Huntsville, Alabama, in conjunction with Abbott Medical Electronics, Houston, Texas. In developing the system, SCI drew upon its extensive experience as a NASA contractor. The company applied telemetry technology developed for the Saturn launch vehicle and the Apollo spacecraft; instrumentation technology developed for heart, blood pressure and sleep monitoring of astronauts aboard NASA's Skylab long duration space station; and communications technology developed for the Space Shuttle.

Evolution of the FUV Surface Properties of 67P/Churyumov-Gerasimenko through its 2015 Perihelion Passage

NASA Astrophysics Data System (ADS)

Feaga, Lori M.; Holt, Carrie E.; Steffl, Andrew; A'Hearn, Michael F.; Bertaux, Jean-Loup; Feldman, Paul D.; Noonan, John; Parker, Joel Wm; Schindhelm, Eric; Stern, S. Alan; Weaver, Harold A.

2016-10-01

Alice, NASA's lightweight and low-power far-ultraviolet (FUV) imaging spectrograph onboard ESA's comet orbiting spacecraft Rosetta (Stern et al. 2007, Space Sci. Rev. 128, 507), has just completed its characterization of the nucleus and coma of the Jupiter family comet 67P/Churyumov-Gerasimenko (C-G). With a spectral range from 700-2050 Å, Alice was able to monitor the sunlit surface of C-G in order to establish if there was variability in the FUV reflectivity across the nucleus, determine if there were distinct spectral features associated with various morphological regions, and infer compositional makeup of the comet. Using spatially resolved pre-perihelion data, the FUV phase dependence, albedo, and spectral slope were derived for the nucleus (Feaga et al. 2015, A&A 583, A27) and were consistent with a homogeneous layer of dust covering the northern hemisphere. During the increase in activity around perihelion and change of seasons on the comet, the Rosetta suite of instruments has shown evidence of surface changes, mass movement of material, and transient patches of ice. The FUV properties of the nucleus throughout the perihelion passage inside of 3 AU, including observations during a zero phase flyby and its associated opposition surge and a search for exposed water ice on the surface, will be presented here and compared to the early pre-perihelion characteristics.

Unstable infiltration fronts in porous media on laboratory scale

NASA Astrophysics Data System (ADS)

Schuetz, Cindi; Neuweiler, Insa

2014-05-01

Water flow and transport of substances in the unsaturated zone are important processes for the quality and quantity of water in the hydrologic cycle. The water movement through preferential paths is often much faster than standard models (e. g. Richards equation in homogeneous porous media) predict. One type/phenomenon of preferential flow can occur during water infiltration into coarse and/or dry porous media: the so-called gravity-driven fingering flow. To upscale the water content and to describe the averaged water fluxes in order to couple models of different spheres it is necessary to understand and to quantify the behavior of flow instabilities. We present different experiments of unstable infiltration in homogeneous and heterogeneous structures to analyze development and morphology of gravity-driven fingering flow on the laboratory scale. Experiments were carried out in two-dimensional and three-dimensional sand tanks as well as in larger two-dimensional sand tanks with homogeneous and heterogeneous filling of sand and glass beads. In the small systems, water content in the medium was measured at different times. We compare the experiments to prediction of theoretical approaches (e.g. Saffman and Taylor, 1958; Chuoke et al., 1959; Philip 1975a; White et al., 1976; Parlange and Hill, 1976a; Glass et al., 1989a; Glass et al., 1991; Wang et al., 1998c) that quantify properties of the gravity-driven fingers. We use hydraulic parameters needed for the theoretical predictions (the water-entry value (hwe), van Genuchten parameter (Wang et al., 1997, Wang et al., 2000) and saturated conductivity (Ks), van Genuchten parameter (Guarracino, 2007) to simplify the prediction of the finger properties and if necessary to identify a constant correction factor. We find in general that the finger properties correspond well to theoretical predictions. In heterogeneous settings, where fine inclusions are embedded into a coarse material, the finger properties do not change much, while the inclusions act as a storage that is filled during the infiltration process. References: Chouke, R.L., van Meurs, P., and van der Poel, C., 1959. The instability of slow immiscible, viscous liquid-liquid displacements in permeable media, Trans. AIME. 216:188-194. Glass, R.J., Steenhuis, T.S., and Parlange J.-Y., 1989a. Mechanism for finger persistence in homogeneous, unsaturated, porous media: Theory and verification, Soil Sci. 148:60-70. Glass R.J., Parlange, J.-Y., and Steenhuis, T.S., 1991. Immiscible displacement in porous media: Stability analysis of three-dimensional, axisymmetric disturbances with application to gravity-driven wetting front instability, Water Resour. Res., 27, 1947-1956. Guarracino, L., 2007. Estimation of saturated hydraulic conductivity Ks from the van Genuchten shape parameter , Water Resour. Res., 43, W11502. Parlange, J.-Y. and Hill, D.E., 1976a. Theoretical analysis of wetting front instability in soils, Soil Sci. 122:236-239. Philip, J. 1975a. Stability analysis of infiltration, Soil Sci. Soc. Am. Proc. 39:1042-1049. Saffman, P.G. and Taylor, G., 1958. The penetration of a fluid into a porous medium or hele-shaw cell containing a more viscous liquid, Proc. R. Soc. London, 245:312-329. Wang Z., Feyen, J., Nielsen, D.R., and van Genuchten, M.T., 1997. Two-phase flow infiltration equations accounting for air entrapment effects, Water Resour. Res., 33:2759-2767. Wang, Z., Feyen, J., and Elrick, D.E., 1998c. Prediction of fingering in porous media, Water Resour. Res. 34(9):2183-2190. Wang Z., Wu, L., and Wu, Q.J., 2000. Water-entry value as an alternative indicator of soil water-repellency and wettability, Journal of Hydrology., 231-232, 76-83. White, I., Colombera, P.M., and Philip, J.R., 1976. Experimental studies of wetting front instability induced by sudden changes of pressure gradient, Soil Sci. Soc. Am. Proc., 40:824-829.

Long-distance Dating: In situ geochronology for planetary missions

NASA Astrophysics Data System (ADS)

Cho, Y.; Cohen, B. A.

2016-12-01

Isotopic dating is an essential tool to establish an absolute chronology for geological events. It enables a planet's crystallization history, magmatic evolution, and alteration to be placed into the framework of solar system history. The capability for in situ geochronology will open up the ability for this crucial measurement to be accomplished as part of lander or rover complement. An in situ geochronology package can also complement sample return missions by identifying the most interesting rocks to cache or return to Earth. The capability of flight instruments to conduct in situ geochronology is called out in the NASA Planetary Science Decadal Survey and the NASA Technology Roadmap as needing development to serve the community's needs. Beagle 2 is the only mission launched to date with the explicit aim to perform in situ K-Ar isotopic dating [1], but it failed to communicate and was lost. The first in situ K-Ar date on Mars, using SAM and APXS measurements on the Cumberland mudstone [2], yielded an age of 4.21 ± 0.35 Ga and validated the idea of K-Ar dating on other planets, though the Curiosity method is not purpose-built for dating and requires many assumptions that degrade its precision. To get more precise and meaningful ages, multiple groups are developing dedicated in situ dating instruments [3-7], including the K-Ar Laser Experiment (KArLE) [5]. KArLE ablates a rock sample, measures K using laser-induced breakdown spectroscopy (LIBS), measures liberated Ar using mass spectrometry (MS), and relates the two by measuring the volume of the ablated pit with optical imaging. The KArLE breadboard tested planetary analog samples yielding ages with 25% uncertainty on very young samples (<50Ma) and 10% uncertainties on older samples. [1] Talboys, et al. (2009) Planetary and Space Science 57, 1237-1245, doi:10.1016/j.pss.2009.02.012. [2] Farley, et al. (2014) Science 343, doi:10.1126/science.1247166. [3] Anderson, et al. (2015) Rapid Comm. Mass Spec. 29, 191-204, doi:10.1002/rcm.7095. [4] Solé (2014) Chem. Geo. doi: 10.1016/j.chemgeo.2014.08.027. [5] Cohen, et al. (2014) Geostand. Geoanaly. Res. 38, 421-439, doi:10.1111/j.1751-908X.2014.00319.x. [6] Farley, et al. (2013) Geochim. Cosmochim. Acta 110, 1-12, doi:10.1016/j.gca.2013.02.010. [7] Cho, et al. (2016) Planet. Space Sci. 128, 14-29.

Late Holocene climate and environmental change from Asiul cave speleothems: interpretations in light of modern cave monitoring.

NASA Astrophysics Data System (ADS)

Smith, Andrew; Wynn, Peter; Barker, Philip; Leng, Melanie; Noble, Steve; Tych, Wlodek

2017-04-01

Northern Iberia offers an excellent location to study fluctuations in North Atlantic Ocean (NA) conditions and the impact that changes in the NA have on atmospheric systems, which dominate Europe's climate. Two speleothems from Cueva de Asiul (Matienzo, N. Spain) have been used to reconstruct rainfall variability in N. Spain throughout the Holocene (Smith et al., 2016a). The carbonate δ18O records from these speleothems are interpreted in the light of a rigorous modern cave monitoring program undertaken at Cueva de Asiul (Smith et al., 2016b). Drip water δ18O reflects a modern rainfall amount effect whilst δ13C appears influenced by Prior Calcite Precipitation (PCP) in the short term and changes in vegetation at long timescales. The speleothem δ18O shows that long duration ( 1500 year) cycles in wetting and drying are prevalent in N. Spain during the Holocene and that dry climate phases are related to the timing of cold events (Bond et al., 2001) in the NA. Here we look in more detail at one of these speleothems, assessing both δ18O and δ13C during the last two thousand years. We show that Cueva de Asiul speleothems not only preserve long duration climate cycles in δ18O, but that they also appear influenced by shorter duration changes in the North Atlantic Oscillation (NAO), in-sync with other NAO archives (Olsen et al., 2012). However, the Cueva de Asiul record does not appear to preserve a predominately positive NAO signal during the Medieval Climate Anomaly (MCA) as is common within many European archives (Trouet et al., 2009), possibly due to the sites' close proximity to the NA and localised oceanic weather systems (Moreno et al., 2012). Alongside climatic changes, the speleothem δ13C shows a clear transition toward higher isotope values around 360 years BP (BP=1950), signalling a major environmental change in the region possibly due to anthropogenic removal of vast swathes of natural forest to support ship building and industry related to the Spanish Armada. Bond et al., (2001), Science 294, 2130-2136. Moreno et al., (2012), Quat. Sci. Rev. 43, 16-32. Olsen et al., (2012), Nat. Geosci. 5, 1-14. Smith et al., (2016a), Sci. Reports.6:24745. Smith et al., (2016b) Int. J. Speleol. 45, 1-9. Trouet et al., (2009), Science 324, 78-80.

Investigation of diamond-like carbon samples as a charge state conversion surface for neutral atom imaging detectors in space applications

NASA Astrophysics Data System (ADS)

Brigitte Neuland, Maike; Riedo, Andreas; Scheer, Jürgen; Wurz, Peter

2014-05-01

The detection of energetic neutral atoms is a substantial requirement on every space mission mapping particle populations of a planetary magnetosphere or plasma of the interstellar medium. For imaging neutrals, these first have to be ionized. Regarding the constraints of weight, volume and power consumption, the technique of surface ionization complies with all specifications of a space mission. Particularly low energy neutral atoms, which cannot be ionized by passing through a foil, are ionized by scattering on a charge state conversion surface. Since more than 30 years intense research work is done to find suitable materials for use as charge state conversion surfaces. Crucial parameters are the ionisation efficiency of the surface material and the scattering properties. Against all expectations, insulators showed very promising characteristics for serving as conversion surfaces. Particularly diamond-like carbon was proven advantageously: While efficiently ionising incoming neutral atoms, diamond stands out by its durability and chemical inertness. In the IBEX-Lo sensor, a diamond-like carbon surface is used for ionisation of neutral atoms. Energy resolved maps of neutral atoms from the IBEX mission revealed phenomena of the interaction between heliosphere and local interstellar medium (LISM) that demand for new theory and explanations [McComas et al., 2011]. Building on the successes of the IBEX mission, a follow up mission concept to further explore the boundaries of the heliosphere already exists. The Interstellar MApping Probe (IMAP) is planned to map neutral atoms in a larger energy range and with a distinct better angular resolution and sensitivity than IBEX [McComas et al.]. The aspired performance of the IMAP sensors implies also for charge state conversion surfaces with improved characteristics. We investigated samples of diamond-like carbon, manufactured by the chemical vapour and pulsed laser deposition method, regarding their ionisation efficiency, scattering and reflexion properties. Experiments were carried out at the ILENA facility [Wahlström et al., 2013] with hydrogen and oxygen atoms, which are the species of main interest in magnetospheric research [Wurz et al., 1997]. Results of very narrow scattering cones and sufficient ionisation efficiency show that diamond-like carbon still is the preferred material for charge state conversion surfaces. But our measurements show that new surface technologies offer improved diamond conversion surfaces with different properties and hence the possibility for improvement of the performance of neutral atom imaging instruments. References: [McComas et al., 2011] D.J. McComas, H.O. Funsten, S.A. Fuselier, W.S. Lewis, E. Möbius and N.A. Schwadron, IBEX observations of Heliospheric energetic neutral atoms: Current understanding and future directions, Geophys. Res. Lett. 38, L18101, 2011 [McComas et al.] Interstellar Mapping Probe (IMAP) mission concept: Illuminating the dark boundaries at the edge of our solar system, decadal survey white paper [Wahlström et al., 2013] P. Wahlström, J.A. Scheer, A. Riedo, P. Wurz and M. Wieser, J. Spacecr. Rockets 50 (2), 402-410 [Wurz et al., 1997] P. Wurz, R. Schletti, M.R. Aellig, Hydrogen and oxygen negative ion production by surface ionization using diamond surfaces, Surf. Sci. 373, 56-66, 1997.

Data Position Statement to Be Updated

NASA Astrophysics Data System (ADS)

Von Holle, Kate

2008-04-01

AGU members have an opportunity to provide comments to a panel preparing to update a position statement for Council consideration in May 2008 concerning the archiving and availability of scientific data. There is currently a risk of losing important data that have been collected over the years, and these data need to be preserved and made publicly available where possible to help future generations understand the various Earth systems. The panel is being asked to address a broad range of data issues that affect Earth and space scientists globally. The current statement can be found at http://www.agu.org/sci_soc/policy/sci_pol.html#positions under the heading ``The importance of archiving and availability of geophysical data.''

Hydrogen-bond symmetrization in methane and hydrogen hydrates in the Mbar range

NASA Astrophysics Data System (ADS)

Bove, L. E.; Ranieri, U.; Gaal, R.; Finocchi, F.; Kuhs, W. F.; Falenty, A.; Klotz, S.; Gillet, P.

2016-12-01

Ice-VII and ice-X phases are the most stable forms of ice at high temperature and extreme pressures, typical of the interiors of satellites and planets. The phase transition between them is a prototypical case of quantum-driven phenomenon, as it can be described as a quantum delocalization of protons in the middle of O-O distances. Recent studies on LiCl- and NaCl-doped ice 1-3 have shown that the presence of salt inclusions in the ice lattice suppresses the quantum behavior of protons, hindering the appearance of the symmetric phase, and possibly suppressing the predicted high temperature superionic phase. This finding stimulated the investigation of similar effects in other water-based compounds, which are thought to be present in icy bodies, namely hydrogen and methane high pressure hydrates. Few experiments have been performed in the past to identify signatures of the hydrogen-bond symmetrization in methane and hydrogen hydrates without reaching conclusive results4,5. Here we present new results on the hydrogen-bond symmetrization of methane and hydrogen hydrates using Raman scattering in the Mbar range and semiclassical simulations including nuclear quantum effects. 1 Bove L. E. et al., E_ect of salt on the H-bond symmetrization in ice, Proc. Natl. Acad. Sci. USA 112, 8216, 2015 ; 2. Bronstein Y. et al., Quantum versus classical protons in pure and salty ice under pressure, Phys. Rev. B 93, 024104, 2016. 3. Klotz S. et al., Ice VII from aqueous salt solutions: From a glass to a crystal with broken H-bonds, Nature Sci. Rep. , in press. 4. Tanaka T. et al., Phase changes of _lled ice Ih methane hydrate under low temperature and high pressure, J. Chem. Phys. 139, 104701, 2013 5. Hirai H. et al., Structural changes of _lled ice Ic hydrogen hydrate under low temperatures and high pressures from 5 to 50 GPa, J. Chem. Phys. 137, 074505, 2012

Subsurface geomicrobiology in a Mars terrestrial analogue, Río Tinto (SW, Spain)

NASA Astrophysics Data System (ADS)

Amils, R.; Fernández-Remolar, D.; Gómez, F.; González-Toril, E.; Rodríguez, N.; Prieto-Ballesteros, O.; Sanz, J. L.; Díaz, E.; Stoker, C.

2008-09-01

Since its discovery, only few years ago, subsurface geomicrobiology is a matter of growing interest [1]. From a fundamental point of view, it seeks to determine whether life can be sustained in the absence of radiation. From an astrobiological point of view, it is an interesting model for life in other planetary bodies, e.g., Mars, as well as early life on Earth. Río Tinto is an unusual extreme acidic environment due to its size (around 100 km), constant acidic pH (mean pH 2.3), high concentrations of heavy metals and high level of microbial diversity [2]. Río Tinto rises in the core of the Iberian Pyritic Belt, one of the biggest sulfidic ore deposits in the world [3]. Today it is well stablished that the extreme characteristics of Río Tinto are not due to acid mine drainage from mining activity, as has been suggested in the past. To explore the hypothesis that a continuous underground reactor of chemolithotrophic microorganisms thriving in the rich sulfidic minerals of the Iberian Pyritic Belt is responsible for the extreme conditions found in the system, a drilling project has been developed to detect evidence of subsurface microbial activity and potential resources to support these microbial communities in situ (MARTE project) [4]. Here we report a search for subsurface life in volcanically hosted massive sulfidic deposits from the Iberian Pyritic Belt. Aseptic core samples were obtained within and down-gradient from the massive sulfide deposits and formation water was sampled within the resulting bore holes. Microbial activity was detected in un-contaminated samples by culture-dependent and culture-independent methods. Aerobic iron- and sulfide- oxidizing bacteria, and anaerobic denitrifying thiosulfate-oxidizing bacteria, sulfate reducing bacteria and methanogenic archaea have been identified. Potential energy fluxes detected in the system include oxidation of reduced iron and sulfur, or hydrogen gas coupled to nitrite, sulfate, ferric iron, inorganic carbon or transient oxygen. These results suggest that multiple energy sources are available from sulfide-mineral weathering to support microbial metabolism, even in the absence of atmospheric oxygen. [1] Stevens, T.O and McKinley, J.P. (1995) Scienc,, 270, 450-454. [2] Amis, R. et al. (2007) Planet Space Sci, 55, 370- 381. [3] Fernández-Remolar, D. et al. (2005) Earth Planet Sci Lett, 240, 149-167. [4] Amils, R. et al. (2008) Microbiology of Extreme Soils, 205-223.

High-Power Testing of 11.424-GHz Dielectric-Loaded Accelerating Structures

NASA Astrophysics Data System (ADS)

Gold, Steven; Gai, Wei

2001-10-01

Argonne National Laboratory has previously described the design, construction, and bench testing of an X-band traveling-wave accelerating structure loaded with a permittivity=20 dielectric (P. Zou et al., Rev. Sci. Instrum. 71, 2301, 2000.). We describe a new program to build a test accelerator using this structure. The accelerator will be powered by the high-power 11.424-GHz radiation from the magnicon facility at the Naval Research Laboratory ( O.A. Nezhevenko et al., Proc. PAC 2001, in press). The magnicon is expected to provide up to 30 MW from each of two WR-90 output waveguide arms in pulses of up to 1 microsecond duration, permitting tests up to a gradient of 40 MV/m. Still higher power pulses (100-500 MW) may be available at the output of an active pulse compressor driven by the magnicon ( A.L. Vikharev et al., Proc. 9th Workshop on Advanced Accelerator Concepts.).

Plant biotechnology for food security and bioeconomy.

PubMed

Clarke, Jihong Liu; Zhang, Peng

2013-09-01

This year is a special year for plant biotechnology. It was 30 years ago, on January 18 1983, one of the most important dates in the history of plant biotechnology, that three independent groups described Agrobacterium tumefaciens-mediated genetic transformation at the Miami Winter Symposium, leading to the production of normal, fertile transgenic plants (Bevan et al. in Nature 304:184-187, 1983; Fraley et al. in Proc Natl Acad Sci USA 80:4803-4807, 1983; Herrera-Estrella et al. in EMBO J 2:987-995, 1983; Vasil in Plant Cell Rep 27:1432-1440, 2008). Since then, plant biotechnology has rapidly advanced into a useful and valuable tool and has made a significant impact on crop production, development of a biotech industry and the bio-based economy worldwide.

An independent evaluation of the Younger Dryas extraterrestrial impact hypothesis

PubMed Central

Surovell, Todd A.; Holliday, Vance T.; Gingerich, Joseph A. M.; Ketron, Caroline; Haynes, C. Vance; Hilman, Ilene; Wagner, Daniel P.; Johnson, Eileen; Claeys, Philippe

2009-01-01

Based on elevated concentrations of a set of “impact markers” at the onset of the Younger Dryas stadial from sedimentary contexts across North America, Firestone, Kennett, West, and others have argued that 12.9 ka the Earth experienced an impact by an extraterrestrial body, an event that had devastating ecological consequences for humans, plants, and animals in the New World [Firestone RB, et al. (2007) Proc. Natl. Acad. Sci. USA 104:16016–16021]. Herein, we report the results of an independent analysis of magnetic minerals and microspherules from seven sites of similar age, including two examined by Firestone et al. We were unable to reproduce any results of the Firestone et al. study and find no support for Younger Dryas extraterrestrial impact. PMID:19822748

Upwelling Rates Beneath Hotspots : Evidence From U-Series in Basalts From the Mid-Atlantic Ridge and the Azores Islands

NASA Astrophysics Data System (ADS)

Bourdon, B. P.; Turner, S. P.

2001-12-01

In this study, we have analyzed U-series in lavas from the Azores islands and the nearby Mid-Atlantic Ridge (FAZAR cruise) in an attempt to assess the relative importance of melting processes versus source variations in the context of ridge-hotpsot interaction. The lavas were analyzed for 238U-230Th (Turner et al. 1997, Bourdon et al. 1996) 226Ra-230Th and 235U-231Pa disequilibria by thermal ionisation mass spectrometry. Our results for the historic lavas from the Azores islands show that the 231Pa excess are at the low end of the trend found for other OIB (Pickett et al. 1997 and Bourdon et al. 1998) and fall on a positive correlation in a 231Pa/235U versus 230Th/238U diagram. In contrast, lavas from the nearby Mid-Atlantic ridge are characterized by larger (231Pa/235U) activity ratios for similar and greater (230Th/238U) ratios. There is also a weak correlation between 226Ra/230Th and 231Pa/235U. These data do not indicate a simple mixing trend between an N-MORB and an enriched component in the 231Pa/235U versus 230Th/238U diagram since the MORBs which do not have the most radiogenic isotope signatures compared with the Azores island basalts have some of the largest (230Th/238U) and 231Pa/235U. Clearly, the dynamics of melting must have played a role in generating larger 230Th and 231Pa excesses beneath the Mid-Atlantic ridge. We infer that this must be due to the absence of a lithospheric lid as larger excesses of 230Th and 231Pa can be generated for longer melting columns. Thus, ridge-hotspot interaction cannot imply a simple transfer of melt from the hotspot to the ridge. The 230Th/238U and 226Ra/230Th data across the Azores plateau shows a maximum for the island of Terceira and mimics the depth anomaly which is thought to result from the hotspot. This trend is also consistent with observations of rare gases (M. Moreira pers. comm.) and suggests that it must be related to the presence of deep material. The U-series trend is the reverse of the trend found in Hawaii by Sims et al. (2000) which was attributed to variations in upwelling rates across the rising plume. This observation can be rationalized in the context of an equilibrium melt transport model (Spiegelman and Elliott, 1993) where U-series disequilibria are sensitive to upwelling rates. For slow upwelling rates such as below the Azores, larger 230Th excesses are predicted in the center of the plume. This suggests that the upwelling rate beneath the center of the plume must be of the order of a few cm per year which is an order of magnitude lower than values estimated for Hawaii. Turner et al. 1997, Chem. Geol. 139, 145-164. Bourdon et al. 1996, Earth Planet. Sci. Lett. 142, 175-189. Pickett et al. 1997, Earth Planet. Sci. Lett. 148, 259-271. Sims et al. 1999, Geochim. Cosmochim. Acta. 63, 4119-4138. Spiegelman and Elliot, 1993, Earth Planet. Sci. Lett., 118, 1-20.

Cloud level winds from UV and IR images obtained by VMC onboard Venus Express

NASA Astrophysics Data System (ADS)

Khatuntsev, Igor; Patsaeva, Marina; Titov, Dmitri; Ignatiev, Nikolay; Turin, Alexander; Bertaux, Jean-Loup

2017-04-01

During eight years Venus Monitoring Camera (VMC) [1] onboard the Venus Express orbiter has observed the upper cloud layer of Venus. The largest set of images was obtained in the UV (365 nm), visible (513 nm) and two infrared channels - 965 nm and 1010 nm. The UV dayside images were used to study the atmospheric circulation at the Venus cloud tops [2], [3]. Mean zonal and meridional profiles of winds and their variability were derived from cloud tracking of UV images. In low latitudes the mean retrograde zonal wind at the cloud top (67±2 km) is about 95 m/s with a maximum of about 102 m/s at 40-50°S. Poleward from 50°S the zonal wind quickly fades out with latitude. The mean poleward meridional wind slowly increases from zero value at the equator to about 10 m/s at 50°S. Poleward from this latitude, the absolute value of the meridional component monotonically decreases to zero at the pole. The VMC observations suggest clear diurnal signature in the wind field. They also indicate a long term trend for the zonal wind speed at low latitudes to increase from 85 m/s in the beginning of the mission to 110 m/s by the middle of 2012. The trend was explained by influence of the surface topography on the zonal flow [4]. Cloud features tracking in the IR images provided information about winds in the middle cloud deck (55±4 km). In the low and middle latitudes (5-65°S) the IR mean retrograde zonal velocity is about 68-70 m/s. In contrast to poleward flow at the cloud tops, equatorward motions dominate in the middle cloud with maximum speed of 5.8±1.2 m/s at latitude 15°S. The meridional speed slowly decreases to 0 at 65-70°S. At low latitudes the zonal and meridional speed demonstrate long term variations. Following [4] we explain the observed long term trend of zonal and meridional components by the influence of surface topography of highland region Aphrodite Terra on dynamic processes in the middle cloud deck through gravity waves. Acknowledgements: I.V. Khatuntsev, M.V. Patsaeva, N.I. Ignatiev, J.-L. Bertaux were supported by the Ministry of Education and Science of Russian Federation grant 14.W03.31.0017. References: [1] Markiewicz W. J. et al.: Venus Monitoring Camera for Venus Express // Planet. Space Sci., 55(12), 1701-1711. doi:10.1016/j.pss.2007.01.004, 2007. [2] Khatuntsev I.V. et al.: Cloud level winds from the Venus Express Monitoring Camera imaging // Icarus, 226, 140-158. 2013. [3] Patsaeva M.V. et al.: The relationship between mesoscale circulation and cloud morphology at the upper cloud level of Venus from VMC/Venus Express // Planet. Space Sci., 113(08), 100-108, doi:10.1016/j.pss.2015.01.013, 2015. [4] Bertaux J.-L. et al.: Influence of Venus topography on the zonal wind and UV albedo at cloud top level: The role of stationary gravity waves // J. Geophys. Res. Planets, 121, 1087-1101, doi:10.1002/2015JE004958, 2016.

EDITORIAL: The 20th European Sectional Conference on Atomic and Molecular Physics of Ionized Gases The 20th European Sectional Conference on Atomic and Molecular Physics of Ionized Gases

NASA Astrophysics Data System (ADS)

Petrović, Zoran Lj; Marić, Dragana; Malović, Gordana

2011-03-01

This special issue consists of papers that are associated with invited lectures, workshop papers and hot topic papers presented at the 20th European Sectional Conference on Atomic and Molecular Physics of Ionized Gases (ESCAMPIG XX). This conference was organized in Novi Sad (Serbia) from 13 to 17 July 2010 by the Institute of Physics of the University of Belgrade. It is important to note that this is not a conference 'proceedings'. Following the initial selection process by the International Scientific Committee, all papers were submitted to the journal by the authors and have been fully peer reviewed to the standard required for publication in Plasma Sources Science and Technology (PSST). The papers are based on presentations given at the conference but are intended to be specialized technical papers covering all or part of the topic presented by the author during the meeting. The ESCAMPIG conference is a regular biennial Europhysics Conference of the European Physical Society focusing on collisional and radiative aspects of atomic and molecular physics in partially ionized gases as well as on plasma-surface interaction. The conference focuses on low-temperature plasma sciences in general and includes the following topics: Atomic and molecular processes in plasmas Transport phenomena, particle velocity distribution function Physical basis of plasma chemistry Plasma surface interaction (boundary layers, sheath, surface processes) Plasma diagnostics Plasma and discharges theory and simulation Self-organization in plasmas, dusty plasmas Upper atmospheric plasmas and space plasmas Low-pressure plasma sources High-pressure plasma sources Plasmas and gas flows Laser-produced plasmas During ESCAMPIG XX special sessions were dedicated to workshops on: Atomic and molecular collision data for plasma modeling, organized by Professors Z Lj Petrovic and N Mason Plasmas in medicine, organized by Dr N Puac and Professor G Fridman. The conference topics were represented in the program by 16 invited lectures, 7 selected hot topics, and 191 poster presentations. The largest number of contributed papers was submitted in Topic 5: Plasma diagnostics (37). The workshop topics were addressed by 10 invited lectures, 5 oral presentations and 7 posters. A post-conference workshop with 5 invited lectures was organized, dealing with the data needs for modeling of plasma sources of light. ESCAMPIG XX was attended by 185 scientists from 31 countries. Of the participants, 30% were PhD students (55). The list includes scientists from the USA, Japan, Australia, Mexico and other non-European countries, which indicates the truly international status of the conference. We would like to thank the authors for their efforts in preparing stimulating lectures and interesting articles for the readers of PSST, and the scientific community dealing with ionized gases, plasma sources and atomic, molecular and chemical physics of low-temperature plasmas for continued interest in the field of ESCAMPIG. We would like to thank the organizers of all previous ESCAMPIG conferences for setting the standards for organization and, in particular, the organizers of ESCAMPIG XVIII and XIX for their direct help and insight. Finally the International Scientific Committee and its chairman in particular have worked hard to select the best possible program and to keep us in line with almost 40 years of tradition and standards of the conference. Most importantly this has been the 20th conference. The quality of new papers shows maturity and new vistas in the field that has produced so much fundamental understanding of complex, non-equilibrium, even nonlinear plasmas. At the same time the field has led to some of the key technologies of modern civilization and has shown that responsible science that pays attention to its societal benefits should have no fear for its future. All critical issues studied today were presented at the meeting and only a small part is represented here. For example, discharges in liquids or above liquids were covered by several lectures represented by two papers. Verreycken et al [1] studied optical emission spectroscopy and Rayleigh scattering in discharges above water electrodes in order to measure gas temperature. At the same time Starikovsky et al [2] showed that it is possible to strike a breakdown directly in the liquid phase without gaseous evaporation or bubbles. Another key issue of present-day low-temperature plasma physics is atmospheric pressure discharges. Application of atmospheric pressure microwave plasma was considered by Belmonte et al [3] as a source for plasma-enhanced chemical vapour deposition. Strategies to produce nanosize structures and high deposition rates have also been proposed. Akishev et al [4] presented modeling results showing why spatial reproducibility of the origins of micro-discharges in a dielectric barrier discharge (DBD) is very high while the stochastic nature of the breakdown leads to jitter. Associated with the application of plasmas in many systems is control plasma chemistry. Tanarro and Herrero [5] performed measurements and modeling of dominant species in a hollow cathode discharge with variation of pressure. Dramatic changes in composition were noticed in H2, H2/Ar, and air. For example, NO becomes the second most abundant neutral under some conditions while at high mean energies H2+ ions become more abundant than H3+. Loureiro et al [6] presented the most detailed self-consistent model of discharges in N2, both pure and in mixtures with H2 and CH4. The model includes coupling of different mechanisms in the gas phase and on surfaces. A further example of detailed plasma chemistry and modeling of possible industrial applications is the work of De Bie et al [7] who studied the conversion of methane to more complex hydrocarbons and other gases in a detailed model of kinetic and plasma chemistry of a DBD reactor. Associated with plasma chemistry models but with a completely different final goal is the work of Taccogna et al [8]. They provide a detailed model of negative ion production in an ITER source of fast neutrals for heating of fusion plasma. Low-temperature plasmas have made their most significant impact through application of etching and other plasma techniques in the production of integrated circuits. Associated with this there have been several papers dealing with control of plasmas relevant for plasma etching applications. Czarnetzki et al [9] presented the modeling of an electrical asymmetry effect which allows independent control of plasma symmetry, bias and consequently properties of ions reaching the surfaces. Separate control of the flux and energy of ions from capacitively coupled plasmas, while an interesting fundamental issue, is also one of the key issues in the manufacture of integrated circuits. Makabe and Yagisawa [10] gave a detailed presentation of the top-down model of plasma devices for etching and other plasma-related nanotechnologies. Their paper presents a complex model covering atomic and molecular collisions and transport, plasma kinetics in complex geometries, and plasma interaction with surfaces with the ability to calculate the development of etched profiles, and the damage-inducing potentials within the wafer. Finally, as the basis of all modeling of plasmas, atomic and molecular collision and transport data were a much more prominent part of ESCAMPIG conferences in the past. We tried to initiate the return of elementary processes to ESCAMPIG from numerous specialized conferences by organizing a workshop on the data for modeling. Bartschat and Zatsarinny [11] gave a presentation of the foundation of the B-spline R-matrix method and a number of cross section results that extend the databases for plasma modeling of atomic gases. State-of-the-art calculations presented here focus on threshold regions of electronic excitation cross sections where complex structures exist due to resonances. These threshold regions of the excitation cross sections, however, determine the distribution function in the region of the ionization, The interface between plasma modeling and atomic physics is swarm studies, and those are based on transport theory that has recently become quite complex and versatile. Dujko et al [12] considered a Boltzmann equation solution to the transport of charged particles, especially in crossed electric and magnetic fields. Apart from indicating the necessity to include transport properties in E × B fields in plasma modeling, these results show complexity and kinetic phenomena that require kinetic models to be properly included. Finally, Makabe and Tatsumi [13] presented the structure of a comprehensive model of plasma etching devices and focused on the requirements for the atomic and collision cross section data. The winner of the W Crookes Prize was Zoltán Donkó [14] who gave a review of particle-in-cell and Monte Carlo simulation methods and presented a review of a large number of systems where he and his co-workers have applied this technique. In particular the lecture gives examples of different kinetic phenomena that arise in modeling of different plasmas. This presentation covers both applications in the control of low-pressure capacitively coupled plasmas and DC breakdown and glow discharges as well as the issues of modeling of elementary processes in the gas phase and on surfaces. Finally, to reply to Harold Pinter and his famous quote, apart from the known and the unknown there is the joy of extending the border of the 'known' and sharing it with colleagues at conferences like ESCAMPIG. Every answer that is reached opens new horizons and new realms of the 'unknown' to explore, and conferences like ESCAMPIG have proven to be a continuous source of ideas and inspiration for all colleagues within the field of low-temperature plasmas and elementary processes. We can certainly hope that the 20th ESCAMPIG was no exception in this regard. References Verreycken T, van Gessel A F H, Pageau A and Bruggeman P 2011 Plasma Sources Sci. Technol. 20 024002 Starikovsky A, Yang Y, Cho Y I and Fridman A 2011 Plasma Sources Sci. Technol. 20 024003 Belmonte T, Gries T, Cardoso R P, Arnoult R, Kosior F and Henrion G 2011 Plasma Sources Sci. Technol. 20 024004 Akishev Y, Aponin G, Balakirev A, Grushin M, Karalnik V, Petryakov A and Trushkin N 2011 Plasma Sources Sci. Technol. 20 024005 Tanarro I and Herrero V J 2011 Plasma Sources Sci. Technol. 20 024006 Loureiro J, Guerra V, Sá P A, Pintassilgo C D and Lino da Silva M 2011 Plasma Sources Sci. Technol. 20 024007 De Bie C, Martens T, van Dijk, Paulussen S, Verheyde B and Bogaerts A 2011 Plasma Sources Sci. Technol. 20 024008 Taccogna F, Minelli P, Diomede P, Longo S, Capitelli M and Schneider R 2011 Plasma Sources Sci. Technol. 20 024009 Czarnetzki U, Schulze J, Schungel E and Donkó Z 2011 Plasma Sources Sci. Technol. 20 024010 Makabe T and Yagisawa T 2011 Plasma Sources Sci. Technol. 20 024011 Bartschat K and Zatsarinny O 2011 Plasma Sources Sci. Technol. 20 024012 Dujko S, White R D, Petrovic Z Lj and Robson R E 2011 Plasma Sources Sci. Technol. 20 024013 Makabe T and Tatsumi T 2011 Plasma Sources Sci. Technol. 20 024014 Donkó Z 2011 Plasma Sources Sci. Technol. 20 024001

On the calculation of line strengths, oscillator strengths and lifetimes for very large principal quantum numbers in hydrogenic atoms and ions by the McLean-Watson formula

NASA Astrophysics Data System (ADS)

Hey, J. D.

2014-08-01

As a sequel to an earlier study (Hey 2009 J. Phys. B: At. Mol. Opt. Phys. 42 125701), we consider further the application of the line strength formula derived by Watson (2006 J. Phys. B: At. Mol. Opt. Phys. 39 L291) to transitions arising from states of very high principal quantum number in hydrogenic atoms and ions (Rydberg-Rydberg transitions, n > 1000). It is shown how apparent difficulties associated with the use of recurrence relations, derived (Hey 2006 J. Phys. B: At. Mol. Opt. Phys. 39 2641) by the ladder operator technique of Infeld and Hull (1951 Rev. Mod. Phys. 23 21), may be eliminated by a very simple numerical device, whereby this method may readily be applied up to n ≈ 10 000. Beyond this range, programming of the method may entail greater care and complexity. The use of the numerically efficient McLean-Watson formula for such cases is again illustrated by the determination of radiative lifetimes and comparison of present results with those from an asymptotic formula. The question of the influence on the results of the omission or inclusion of fine structure is considered by comparison with calculations based on the standard Condon-Shortley line strength formula. Interest in this work on the radial matrix elements for large n and n‧ is related to measurements of radio recombination lines from tenuous space plasmas, e.g. Stepkin et al (2007 Mon. Not. R. Astron. Soc. 374 852), Bell et al (2011 Astrophys. Space Sci. 333 377), to the calculation of electron impact broadening parameters for such spectra (Watson 2006 J. Phys. B: At. Mol. Opt. Phys. 39 1889) and comparison with other theoretical methods (Peach 2014 Adv. Space Res. in press), to the modelling of physical processes in H II regions (Roshi et al 2012 Astrophys. J. 749 49), and the evaluation bound-bound transitions from states of high n during primordial cosmological recombination (Grin and Hirata 2010 Phys. Rev. D 81 083005, Ali-Haïmoud and Hirata 2010 Phys. Rev. D 82 063521, Ali-Haïmoud 2013 Phys. Rev. D 87 023526).

Updates in the IR responsivity of VIR, the spectrometer of the Dawn mission.

NASA Astrophysics Data System (ADS)

Ammannito, Eleonora; Mc Cord, Thomas B.; De Sanctis, Maria Cristina.; Combe, Jean-Philippe

VIR-MS (Visual and Infrared Mapping Spectrometer) is the imaging spectrometer of the Dawn mission (1,2). Here, first we describe the computation of a new instrument responsivity based on the internal calibration data acquired during the operations at Vesta, and then we describe its effect on the dataset and on the results published so far. VIR-MS was built in Italy by a scientific-industrial (IAPS/INAF in Rome (Italy) and Selex ES in Campi Bisenzio (Fi, Italy)) consortium financially supported by the Italian Space Agency. VIR-MS is an high spatial resolution spectrometer (FOV of 64mrad, IFOV of 250 µrad) in the 0.25-5 µm range with an IFOV of 250 µrad and a spectral sampling of about 2 nm in the visible range and 10 nm in the IR range. The results of the on-ground calibration held in the Selex calibration facility in September 2005 were already presented and discussed in a paper (2). This version has been used to calibrate the data available on the Planetary Data System (PDS) Small Bodies Node, dataset used in all the papers published so far. However, after the operations at the asteroid Vesta, we have identified some artifacts in the instrument responsivity in the 2.5-3.5 µm region, which is where several absorption bands of OH and H2O occur. Those artifacts were systematic, and therefore they did not prevent the detection of relative spectral variations associated to OH and H2O. Actually, the only paper published in which are discussed spectra in this range (3) used a different calibration method described in the paper itself. This method used a simple correction of the response function based on an empirical calibration correction that is appropriate to recover the signal in that specific range. However, the absolute absorption band depth of OH and H2O could not be calculated. To compute a new instrument responsivity we used the internal lamp of the spectrometer. This lamp, made of a tungsten filament, is characterized by a blackbody-like emission at about 2400K (4). Since the spectrum of the infrared radiation emitted by the tungsten filaments is featureless, a polystyrene filter was inserted for a wavelength calibration of the IR channel. The idea was to use the black body radiation of this lamp to retrieve a relative Instrument Responsivity in the 2.5-3.5 µm region. First we calibrated the signal from internal calibration lamp with the on-ground responsivity, and then we retrieved the equivalent temperature of the radiation fitting a Planck curve. The next step was to compute the Planck function at the equivalent temperature. The new Instrument Responsivity is the result of the ratio between the raw signal of the lamp and the Planck function. This ratio must be multiplied by a factor to take into account the integration time used to acquire the signal, the transmittance of the polystyrene filter, and the viewing geometry. The new instrument responsivity function minimizes most calibration residuals that was showing as artifact peaks between 2.5 and 2.9 µm in the previous calibration. It now allows the use of VIR spectra to identify absorption bands of OH and H2O, without requiring additional empirical corrections. As calibration is always an on-going process, we are looking forward to enable the interpretation of absolute absorption band depths, which is a required step for the calculation of surface material abundances. References: (1) C.T. Russell & C.A. Raymond, Space Sci. Rev., 163, 3 2011 (2) M.C. De Sanctis, A. Coradini, E. Ammannito, E., et al. Space Sci. Rev.,163, 329, 2011 (3) M.C. DeSanctis, J-Ph. Combe et al APJL 758:L36, 2013 (4)R. Melchiorri, G. Piccioni, A. Mazzoni, Rev. Sci. Instrum. 74(8), 3796-3801 2003

Electroacupuncture improves gait locomotion, H-reflex and ventral root potentials of spinal compression injured rats.

PubMed

Escobar-Corona, Carlos; Torres-Castillo, Sergio; Rodríguez-Torres, Erika Elizabeth; Segura-Alegría, Bertha; Jiménez-Estrada, Ismael; Quiroz-González, Salvador

2017-05-01

This study explored the effect of electroacupuncture stimulation (EA) on alterations in the Hoffman reflex (H-reflex) response and gait locomotion provoked by spinal cord injury (SCI) in the rat. A compression lesion of the spinal cord was evoked by insufflating a Fogarty balloon located in the epidural space at the T8-9 spinal level of adult Wistar male rats (200-250 gr; n=60). In different groups of SCI rats, EA (frequencies: 2, 50 and 100Hz) was applied simultaneously to Huantiao (GB30), Yinmen (BL37), Jizhong (GV6) and Zhiyang (GV9) acupoints from the third post-injury day until the experimental session. At 1, 2, 3 and 4 post-injury weeks, the BBB scores of the SCI group of rats treated with EA at 50Hz showed a gradual but greater enhancement of locomotor activity than the other groups of rats. Unrestrained gait kinematic analysis of SCI rats treated with EA-50Hz stimulation showed a significant improvement in stride duration, length and speed (p<0.05), whereas a discrete recovery of gait locomotion was observed in the other groups of animals. After four post-injury weeks, the H-reflex amplitude and H-reflex/M wave amplitude ratio obtained in SCI rats had a noticeable enhancement (217%) compared to sham rats (n=10). Meanwhile, SCI rats treated with EA at 50Hz manifested a decreased facilitation of the H-reflex amplitude and H/M amplitude ratio (154%) and a reduced frequency-dependent amplitude depression of the H-reflex (66%). In addition, 50 Hz-EA treatment induced a recovery of the presynaptic depression of the Gs-VRP evoked by PBSt conditioning stimulation in the SCI rat (63.2±8.1%; n=9). In concordance with the latter, it could be suggested that 50 Hz-EA stimulation reduced the hyper-excitability of motoneurons and provokes a partial improvement of the locomotive performance and H reflex responses by a possible recovery of presynaptic mechanisms in the spinal cord of experimentally injured rats. Copyright © 2017 Elsevier Inc. All rights reserved.

Vertical profiles for SO2 and SO on Venus from different one-dimensional simulations

NASA Astrophysics Data System (ADS)

Mills, Franklin P.; Jessup, Kandis-Lea; Yung, Yuk

2017-10-01

Sulfur dioxide (SO2) plays many roles in Venus’ atmosphere. It is a precursor for the sulfuric acid that condenses to form the global cloud layers and is likely a precursor for the unidentified UV absorber, which, along with CO2 near the tops of the clouds, appears to be responsible for absorbing about half of the energy deposited in Venus’ atmosphere [1]. Most published simulations of Venus’ mesospheric chemistry have used one-dimensional numerical models intended to represent global-average or diurnal-average conditions [eg, 2, 3, 4]. Observations, however, have found significant variations of SO and SO2 with latitude and local time throughout the mesosphere [eg, 5, 6]. Some recent simulations have examined local time variations of SO and SO2 using analytical models [5], one-dimensional steady-state solar-zenith-angle-dependent numerical models [6], and three-dimensional general circulation models (GCMs) [7]. As an initial step towards a quantitative comparison among these different types of models, this poster compares simulated SO, SO2, and SO/SO2 from global-average, diurnal-average, and solar-zenith-angle (SZA) dependent steady-state models for the mesosphere.The Caltech/JPL photochemical model [8] was used with vertical transport via eddy diffusion set based on observations and observationally-defined lower boundary conditions for HCl, CO, and OCS. Solar fluxes are based on SORCE SOLSTICE and SORCE SIM measurements from 26 December 2010 [9, 10]. The results indicate global-average and diurnal-average models may have significant limitations when used to interpret latitude- and local-time-dependent observations of SO2 and SO.[1] Titov D et al (2007) in Exploring Venus as a Terrestrial Planet, 121-138. [2] Zhang X et al (2012) Icarus, 217, 714-739. [3] Krasnopolsky V A (2012) Icarus, 218, 230-246. [4] Parkinson C D et al (2015) Planet Space Sci, 113-114, 226-236. [5] Sandor B J et al (2010) Icarus, 208, 49-60. [6] Jessup K-L et al (2015) Icarus, 258, 309-336. [7] Stolzenbach A et al (2014) EGU General Assembly 2014, 16, EGU2014-5315. [8] Allen M et al (1981) J Geophys Res, 86, 3617-3627. [9] Harder J W et al (2010) Sol Phys, 263, 3-24. [10] Snow M et al (2005) Sol Phys, 230, 295-324.

Carbon Monoxide Poisoning: Death on Mount McKinley,

DTIC Science & Technology

1987-05-08

Additionally, studies by Astrup(5) and Thomas(6) have reported decreased erythrocytic 2, 3- diphosphoglycerate (2, 3-DPG) concentrations with acute...Halebian, et al found no significant difference in measured 02 consumption or extraction between dogs subjected to CO poisoning vs nitrogen anoxia .(9...Astrup P: Intraerythrocytic 2,3- diphosphoglycerate and carbon monoxide exposure. Ann NY Acad Sci 1970;174:252-254. 6. Thomas MF, Penny DG: Hematologic

Zonally Asymmetric Ozone and the Morphology of the Planetary Waveguide

DTIC Science & Technology

2011-07-15

sections for the 271 troposphere , J. Atmos. Sci., 37, 2600-2616. 272 Eyring, V., et al. (2007), Multimodel projections of stratospheric ozone ...GEOPHYSICAL RESEARCH LETTERS, VOL. ???, XXXX, DOI:10.1029/, JULY 15, 2011 Zonally asymmetric ozone and the morphology of the 1 planetary waveguide...that zonally asymmetric 6 ozone (ZAO) profoundly changes the morphology of the Northern Hemisphere planetary 7 waveguide (PWG). ZAO causes the PWG to

Mechanics of Bimodular Composite Structures.

DTIC Science & Technology

1982-07-01

and P. de Meester (1978). The mechanical behaviour of porous austenitic stainless steel fibre structure. J. Matls. Sci., 13, 2650-2658. Gilbert, G.N.J...Investigator Material EClEt Kotlarskii & Karbasova (1968) Fabric/rubber 0.38 Ducheyne et al. (1978) Sintered, porous 0.1 stainless steel Zolotukhina & Lepetov...with aramid cord than when reinforced with polyester cord, This is probably related to the very low compressive strength of the aramid fibers

How Gender and Reformed Introductory Physics Impacts Student Success in Advanced Physics Courses and Continuation in the Physics Major

ERIC Educational Resources Information Center

Rodriguez, Idaykis; Potvin, Geoff; Kramer, Laird H.

2016-01-01

Active-learning approaches to teaching introductory physics have been found to improve student learning and affective gains on short-term outcomes [S. Freeman et al., "Proc. Natl. Acad. Sci. U.S.A. 111," 8410 (2014)]; however, whether or not the benefits of active learning impact women to the same degree as men has been a point of…

Design of a lens table for a double toroidal electron spectrometer

DOE Office of Scientific and Technical Information (OSTI.GOV)

Liu Xiaojng; Nicolas, Christophe; Miron, Catalin

2013-03-15

We report here on the method we developed to build a lens table for a four-element electrostatic transfer lens operated together with a double toroidal electron energy analyzer designed by one of us, and whose original design and further improvements are described in detail in Miron et al. [Rev. Sci. Instrum. 68, 3728 (1997)] and Le Guen et al. [Rev. Sci. Instrum. 73, 3885 (2002)]. Both computer simulations and laboratory instrument tuning were performed in order to build this lens table. The obtained result was tested for a broad range of electron kinetic energies and analyzer pass energies. Based onmore » this new lens table, allowing to easily computer control the spectrometer working conditions, we could routinely achieve an electron energy resolution ranging between 0.6% and 0.8% of the analyzer pass energy, while the electron count rate was also significantly improved. The establishment of such a lens table is of high importance to relieve experimentalists from the tedious laboring of the lens optimization, which was previously necessary prior to any measurement. The described method can be adapted to any type of electron/ion energy analyzer, and will thus be interesting for all experimentalists who own, or plan to build or improve their charged particle energy analyzers.« less

A Space of Their Own

ERIC Educational Resources Information Center

Lum, Lydia

2008-01-01

For decades, many universities have attached themes to some of its residence halls, encouraging students with similar interests to live among each other, such as outdoor enthusiasts or sci-fi buffs. Some schools also designate housing for students intent on fluency in a foreign language so that they can better immerse themselves. Meanwhile, ethnic…

Portfolio theory and the alternative decision rule of cost-effectiveness analysis: theoretical and practical considerations.

PubMed

Sendi, Pedram; Al, Maiwenn J; Gafni, Amiram; Birch, Stephen

2004-05-01

Bridges and Terris (Soc. Sci. Med. (2004)) critique our paper on the alternative decision rule of economic evaluation in the presence of uncertainty and constrained resources within the context of a portfolio of health care programs (Sendi et al. Soc. Sci. Med. 57 (2003) 2207). They argue that by not adopting a formal portfolio theory approach we overlook the optimal solution. We show that these arguments stem from a fundamental misunderstanding of the alternative decision rule of economic evaluation. In particular, the portfolio theory approach advocated by Bridges and Terris is based on the same theoretical assumptions that the alternative decision rule set out to relax. Moreover, Bridges and Terris acknowledge that the proposed portfolio theory approach may not identify the optimal solution to resource allocation problems. Hence, it provides neither theoretical nor practical improvements to the proposed alternative decision rule.

Noninvasive determination of optical lever sensitivity in atomic force microscopy

NASA Astrophysics Data System (ADS)

Higgins, M. J.; Proksch, R.; Sader, J. E.; Polcik, M.; Mc Endoo, S.; Cleveland, J. P.; Jarvis, S. P.

2006-01-01

Atomic force microscopes typically require knowledge of the cantilever spring constant and optical lever sensitivity in order to accurately determine the force from the cantilever deflection. In this study, we investigate a technique to calibrate the optical lever sensitivity of rectangular cantilevers that does not require contact to be made with a surface. This noncontact approach utilizes the method of Sader et al. [Rev. Sci. Instrum. 70, 3967 (1999)] to calibrate the spring constant of the cantilever in combination with the equipartition theorem [J. L. Hutter and J. Bechhoefer, Rev. Sci. Instrum. 64, 1868 (1993)] to determine the optical lever sensitivity. A comparison is presented between sensitivity values obtained from conventional static mode force curves and those derived using this noncontact approach for a range of different cantilevers in air and liquid. These measurements indicate that the method offers a quick, alternative approach for the calibration of the optical lever sensitivity.

A Temperature-Dependent Phase-Field Model for Phase Separation and Damage

NASA Astrophysics Data System (ADS)

Heinemann, Christian; Kraus, Christiane; Rocca, Elisabetta; Rossi, Riccarda

2017-07-01

In this paper we study a model for phase separation and damage in thermoviscoelastic materials. The main novelty of the paper consists in the fact that, in contrast with previous works in the literature concerning phase separation and damage processes in elastic media, in our model we encompass thermal processes, nonlinearly coupled with the damage, concentration and displacement evolutions. More particularly, we prove the existence of "entropic weak solutions", resorting to a solvability concept first introduced in Feireisl (Comput Math Appl 53:461-490, 2007) in the framework of Fourier-Navier-Stokes systems and then recently employed in Feireisl et al. (Math Methods Appl Sci 32:1345-1369, 2009) and Rocca and Rossi (Math Models Methods Appl Sci 24:1265-1341, 2014) for the study of PDE systems for phase transition and damage. Our global-in-time existence result is obtained by passing to the limit in a carefully devised time-discretization scheme.

Implications of a reducing and warm (not hot) Archaean ambient mantle for ancient element cycles

NASA Astrophysics Data System (ADS)

Aulbach, Sonja

2016-04-01

There is considerable uncertainty regarding the oxygen partial pressure (fO2) and potential temperature (TP) of the ambient convecting mantle throughout Earth's history. Rare Archaean eclogite suites have elemental and isotopic compositions indicative of formation of crustal protoliths in oceanic spreading ridges, hence unaffected by continental sources. These include some eclogite xenoliths derived from cratonic mantle lithosphere and orogenic eclogites marking the exhumation of oceanic crust at Pacific-type margins. Their compositions may retain a memory of the thermal and redox state of the Archaean convecting mantle sources that gave rise to their low-pressure protoliths. Archaean eclogites have TiO2-REE relationships consistent with fractional crystallisation of olivine±plagioclase and cpx during formation of picritic protoliths from a melt that separated from a garnet-free peridotite source, implying intersection of the solidus at ≤2.5 to 3.0 GPa [1]. Low melt fractions (<0.25) inferred from samples with the least fractionated (lowest TiO2) protoliths further argue against deep intersection of the mantle solidus. This suggests a moderately elevated TP ~ 1420-1470 degrees C (lower than some estimates for the ambient convecting mantle at that time [2]), which would support an early onset of plate tectonics [3] and emergence of continents [4], heralding a transition to modern chemical cycles. Moderate TP further indicates that deep recycling of carbon and water, though reduced compared to today, may have been possible in the Archaean [5,6]. Carefully screened eclogites have V/Sc (reflecting the redox state of the ambient mantle during protolith formation [7]) corresponding to ΔFMQ corrected to 1 GPa as low as -1.7 at 3 Ga [1]. Such low oxygen fugacities have consequences for the location of the peridotite solidus and for the types of melts generated during redox melting [5,8]. They also modulate the redox state of volatiles liberated at oceanic spreading ridges [7] in the Archaean, with implications for the composition and oxygenation of the palaeo-atmosphere. Subsequent subduction of such reducing oceanic crust must have also affected the cycling of volatile elements (soluble instead of molecular species [9]) and of redox-sensitive ore-forming metals [10] during metamorphic dehydration and melting reactions. [1] Aulbach&Viljoen (2015) Earth Planet Sci Lett 431; [2] Herzberg et al. (2010) Earth Planet Sci Lett 292; [3] Sizova et al. (2010) Lithos 116; [4] Rey&Coltice (2008) Geology 36; [5] Dasgupta (2013) RIMG 75; [6] Magni et al. (2014) G3 15; [7] Li&Lee (2004) EPSL 228; [8] Stagno et al. (2013) Nature 493; [9] Sverjensky et al. (2014) Nat Geosci 7; [10] Evans & Tomkins (2011) Earth Planet Sci Lett 308.

THE CD ISOTOPE SIGNATURE OF THE SOUTHERN OCEAN

NASA Astrophysics Data System (ADS)

Abouchami, W.; Galer, S. J.; Middag, R.; de Baar, H.; Andreae, M. O.; Feldmann, H.; Raczek, I.

2009-12-01

The availability of micronutrients can limit and control plankton ecosystems, notably in the Southern Ocean which plays a major role in regulating the CO2 biological pump. Cadmium has a nutrient-like distribution in seawater - it is directly incorporated into living plankton in the upper water column and re-mineralised at depth. The nutritional role of Cd (Price and Morel, 1990) makes it a potentially useful tracer of biological productivity. We report Cd concentration and Cd stable isotope data obtained using a double-spike TIMS method on seawater samples collected during the Zero and Drake Passage cruise (ANTXXIV-III, IPY-GEOTRACES 2008). Four vertical profiles were collected from 40 to 70°S across the Polar Front using the ultra-clean Titan frame (De Baar et al., 2008), providing a record of changes in biological productivity from the Subantarctic to the Antarctic region. Data from two profiles from the SE Atlantic (47.66°S, 4.28W) and Drake Passage (55.13°S, 65.53°W) obtained on 1 litre-sized samples are presented. Both profiles show a increase in Cd concentration with depth, with noticeably higher concentrations in the SE Atlantic. Cd and PO4 are positively correlated with distinct slopes for the two profiles. The Cd isotope data are expressed as ɛ112/110Cd relative to our JMC Mainz standard (± 8ppm, 2SD, N=17). ɛ112/110Cd values show a continuous decrease with increasing depth and a significant shift towards heavier values in the upper 400m at both stations resolvable outside analytical error (2SE ≤ 20ppm). The sense of Cd isotope fractionation confirms previous findings of uptake of “light” Cd by phytoplankton in the upper water column (Lacan et al., 2006; Ripperger et al., 2007; Schmidt et al., 2009). Most important is the evidence for a distinctive heavier Cd isotope signature in AASW relative to AAIW. This result demonstrates that different water masses carry distinct Cd isotopic compositions reflecting changes in Cd uptake by phytoplankton. Price and Morel(1990) Nature 344, 658-660. De Baar et al.(2008) Mar. Chem. 111, 4-21 Lacan et al.(2006) Geochim. Cosmochim. Acta 70, 5104-5118. Ripperger et al.(2007) Earth Planet. Sci. Lett 261,670-684. Schmidt et al.(2009)Earth Planet. Sci. Lett 277, 262-272.

The Cloud Paradigm: Geostable molecules as proxies for surface oxygenation

NASA Astrophysics Data System (ADS)

Summons, R. E.; Hallmann, C.

2011-12-01

Geoscientists continue to puzzle over when and by which means Earth's surface environment became oxygenated. One of the prevailing scenarios, articulated by Cloud, Holland and Walker, proposes an initially anoxic or very low O2 atmosphere. Although photosystem II is thought to have appeared early, there was an extended period of imbalance between sources & sinks of O2 due to pervasive feedback between biosphere, atmosphere, hydrosphere & lithosphere. Ultimately O2 accumulated in the atmosphere to such levels that it left geochemical and physical evidence for mobilization of redox-sensitive elements in what is currently referred to as the 'Great Oxidation Event' or GOE at c. 2.45 Ga. While some researchers hold that the GOE marks the advent of oxygenic photosynthesis (e.g. Kopp et al., 2005), a wealth of geochemical and paleontological data is consistent with the presence of both cyanobacteria (e.g. Bosak et al., 2009) and traces of environmental oxygen (e.g. Anbar et al., 2007) several hundred million years prior. Further, molecular fossils present in 2.7-2.5 Ga rocks from the Transvaal Supergroup of the Kaapvaal Craton include steroids and other molecules indicative of oxygen-dependent biosynthesis and oxygen-respiring methanotrophic bacteria (Waldbauer et al., 2008). New molecular data for samples from the Mount McRae Formation in the Mt Bruce Supergroup, Pilbara Craton, identifies a diverse array of hydrocarbons including steroids and carotenoid residues diagnostic of phototrophic green sulfur bacteria. Co-variance of biomarker ratios with inorganic proxies-each leading to similar environmental reconstructions- confirm the authenticity of this signal. The carotenoid biomarkers indicate that the surface waters of the Hamersley Basin provided a sustained supply of hydrogen sulfide for anoxygenic photosynthesis and, indirectly, suggest the presence of precursor sulfate derived from the oxidative weathering of metal sulfides. Anbar A.D. et al. A whiff of oxygen before the great oxidation event. Science 317, 1903-1906. (2007). Bosak T. et al., Morphological record of oxygenic photosynthesis in conical stromatolites. Proc. Natl. Acad. Sci. USA 106:10939-10943 (2009). Kopp, R.E. et al.,The Paleoproterozoic snowball Earth: A climate disaster triggered by the evolution of oxygenic photosynthesis. Proc. Natl. Acad. Sci. USA 102: 11131-11136 (2005). Waldbauer J.R. et al. Late Archean molecular fossils from the Transvaal Supergroup record the antiquity of microbial diversity and aerobiosis. Precambrian Research 169, 28-47 (2008).

Cuticular Biominerals of the Terrestrial Crustacean Oniscus asellus (Isopoda, Linnaeus 1758)

NASA Astrophysics Data System (ADS)

Mergelsberg, S. T.; Mukhopadhyay, B.; Dove, P. M.

2013-12-01

Biomineralization is a phenomenon observed in many eukaryotic organisms and evidence suggests this process began relatively early in the evolution of multicellular life (Marin F et al. 1996). Crustaceans form a large fraction of all eukaryotic biomineralizers by incorporating calcium carbonate (CaCO3) into their cuticle. Terrestrial species are challenged in their production of CaCO3 by the absence of calcium-rich waters. To cope with this limitation, the terrestrial crustacean Oniscus asellus recycles up to 80% (Auzou G 1953) of its total calcium during the molting process. This feat is accomplished by separate molting of the front and back cuticle, with temporary storage of the calcium carbonate as amorphous calcium carbonate (ACC) in the front half (Ziegler A 1997). These processes infer a highly efficient and regulated mechanism for biomineralization that is most likely orchestrated by a myriad of proteins (Ziegler A et al. 2012). Until recently, investigations of biomineralization were largely directed toward understanding morphology and large-scale chemistry of the minerals, ignoring the mechanistic roles of biomacromolecules in mineralization processes. More recent work suggests a high involvement of these compounds on the formation of biominerals and, in some cases, the specific polymorphs thereof (Keene EC et al. 2010). This study focuses on identifying the components of the biological mineralization matrix at each stage of the process. Using chemical demineralization of the stored ACC, all biomacromolecules can be separated and purified for subsequent analysis by MALDI-TOF mass spectrometry. To link the localized biochemistry more intimately to the polymorph of calcium carbonate that forms in the animal, the inorganic phase (';the mineral') will be monitored at each life stage using XRD and TEM. This analysis will reveal the organic components of a very precise biomineralization mechanism and may shed insight on its evolutionary origin. References: Marin F, Westbroek P et al., 1996, Proc Nat Acad Sci 93:1554-1559 Auzou G, 1953, L Ann Sci Nat 15:71-98 Ziegler A, 1997, Zoomorphology 117:181-187 Ziegler A et al., 2012, Cryst Growth Des 12:646-655 Keene EC et al., 2010, Cryst Growth Des 10:1383-1389

Scenarios of atmospheric rivers affecting Western Europe during the XXI Century

NASA Astrophysics Data System (ADS)

Trigo, Ricardo M.; Ramos, Alexandre M.; Tomé, Ricardo; Liberato, Margarida L. R.; Pinto, Joaquim G.

2017-04-01

Extreme precipitation events in Europe during the winter half of the year have major socio-economic impacts associated with floods, landslides, extensive property damage and life losses. In recent years, a number of works have shed new light on the role played by Atmospheric Rivers (ARs) in the occurrence of extreme precipitation events in Europe as was the case in major historical floods in Duero (Pereira et al., 2016) and Tagus (Trigo et al., 2015) rivers in Iberia. We analyse ARs reaching Europe, for the extended winter months (October to March), in simulations from six CMIP5 global climate models (CGMs) to quantify possible changes during the current century, with emphasis in five western European prone coastal areas. ARs are represented reasonably well in GCMs for recent climate conditions (1980-2005). Increased vertically integrated horizontal water transport is found for 2074- 2099 (RCP4.5 and RCP8.5) compared to 1980-2005, while the number of ARs is projected to double on average for the same period. These changes are robust between models and are associated with higher air temperatures and thus enhanced atmospheric moisture content, together with higher precipitation associated with extra-tropical cyclones. This suggests an increased risk of intense precipitation and floods along the Atlantic European Coasts from the Iberian Peninsula to Scandinavia (Ramos et al., 2016). References: Pereira et al., (2016) Spatial impact and triggering conditions of the exceptional hydro-geomorphological event of December 1909 in Iberia, Nat. Hazards Earth Syst. Sci., 16, 371-390. Ramos et al., (2016) Projected changes in atmospheric rivers affecting Europe in CMIP5 models, Geophys. Res. Lett., 43, 9315-9323. Trigo et al., (2015) The record precipitation and flood event in Iberia in December 1876: description and synoptic analysis, Front. Earth Sci. 2:3. Acknowledgements This work was supported by the project FORLAND - Hydrogeomorphologic risk in Portugal: driving forces and application for land use planning (PTDC/ATPGEO/1660/2014) funded by Fundação para a Ciência e a Tecnologia, Portugal (FCT). A. M. Ramos was also supported by a FCT postdoctoral grant (FCT/DFRH/ SFRH/BPD/84328/2012).

Polarimetric radar convective cell tracking reveals large sensitivity of cloud precipitation and electrification properties to CCN

NASA Astrophysics Data System (ADS)

Hu, J.; Rosenfeld, D.; Zhang, P.; Snyder, J.; Orville, R. E.; Ryzhkov, A.; Zrnic, D.; Williams, E. R.; Zhang, R.

2017-12-01

Here we apply the cell tracking methodology, shown in our companion poster, to quantifying factors affecting the vigor and the time-height evolution of hydrometeors and electrification properties of convective cells. Benefitting from the Dual-polarimetric NEXRAD radar network, we composite more than 5000 well-tracked cells among three radars (at Houston, Lubbock and Oklahoma City), stratified by CCN, CAPE and land/sea locations. The analyzed cell properties include Z, ZDR, Kdp, and ρhv, Dm (raindrop diameter) and Nw (raindrop concentration) by the algorithm of Bringi et al. (2003). Lightning Mapping Array (LMA) data is also included in the analysis, which provides a 3D structure of lightning occurrence and RF power. The contrasting CCN conditions over marine, land, pristine and polluted areas are identified based on the satellite retrieval technique described in Rosenfeld et al. (2016). The results show that more CCN are associated with: Increased echo top height, manifesting the invigoration effect. Enhanced reflectivities, especially above the freezing level at around 4.5 km. Raindrop sizes at the initial stage increase at the expense of their concentrations, due to the smaller cloud droplets and suppressed coalescence. Larger propensity for hail. Lightning sources increase with greater CCN concentration and is likely due to the delayed warm rain process and enhanced mixed phase process under more CCN condition, when activated CCN into cloud droplets is too high (> 1000 cm-3) the glaciation is delayed too much and leave little ice at lower levels and thus decrease lightning activity. Land pristine clouds have fewer lightning sources than polluted clouds. Marine pristine clouds seldom have lightning Increased CAPE had a similar effect to the effect of added CCN. The cloud tracking and properties are obtained by a new methodology of Multi-Cell Identification and Tracking (MCIT) algorithm (Hu et al, 2017), with details about the algorithm to be found in the author's accompanying poster session. References [1] Bringi, V. et al., J. Atmos. Sci., 60, 354-365. (2003) [2] Rosenfeld, D. et al., Proc. Natl. Acad. Sci., 113, 5828-5834. (2016) [3] Hu, J. et al., in preparation.

Ocean Compositions on Europa and Ganymede

NASA Astrophysics Data System (ADS)

Leitner, M. A.; Bothamy, N.; Choukroun, M.; Pappalardo, R. T.; Vance, S.

2014-12-01

The ocean compositions of icy Galilean satellites Europa and Ganymede are highly uncertain. Spectral observations of the satellites' surfaces provide clues for the interior composition. Putative sulfate hydration features in Galileo near-infrared reflectance spectra suggest fractionation of Na and Mg sulfates from a subsurface reservoir (McCord et al. 1998, Sci. 278, 271; McCord et al. 1998, Sci. 280, 1242; Dalton et al. 2005, Icarus, 177, 472). Recent spatially resolved spectral mapping of Europa hints at possible partitioning of near-surface brines in Europa's low-lying planes (Shirley et al. 2010; Icarus, 210, 358; Dalton et al. 2012; J. Geophys. Res. 117, E03003). Surface materials can be modified by the delivery of material from impacts and Io's active volcanoes as well as intense irradiation from Jupiter's magnetic field interaction with the jovian magnetosphere. These factors, combined with observations of high Cl/K ratios in Europa's exosphere, have led other investigators to suggest that Europa's ocean is dominated by dissolved chloride rather than sulfate (Brown and Hand 2013; Astr. J. 145, 110). There is still much uncertainty regarding how well the surface composition approximates the interior ocean composition. Exogenic materials, seafloor hydrothermal processes, and fractional crystallization during ice formation will determine the abundances of species in the ocean and by extension those present on Europa's surface. We develop a bottom-up model for oceans on Europa and Ganymede, assuming initial compositions of chondritic and cometary materials including an Fe core for Europa and an Fe-FeS eutectic core for Ganymede. We calculate an ocean composition by employing a Bulk Silicate Earth approach, also used by Zolotov and Shock (2001; J. Geophys. Res. 106, 32815) at Europa, which assess element partitioning between the rocky mantle, Fe-rich core, and water ocean. Partitioning factors are based on terrestrial estimates for Earth. The resulting ocean composition is used to assess solid precipitation into the ocean and ice shell using FREZCHEM modeling software (Marion et al. 2010; Icarus, 207, 675). These results are then compared with measured compositions of brines on Europa's surface. We develop the model in a way that permits ready application to other icy satellites, such as Titan or Enceladus.

Can Ecliptic Comets Be Created En Route from the Kuiper Belt?

NASA Astrophysics Data System (ADS)

Dones, Henry C. Luke; Womack, Maria; Nesvorny, David; Bierhaus, Edward B.; Zahnle, Kevin; Robbins, Stuart J.; Bottke, William; Alvarellos, Jose; Hamill, Patrick

2017-10-01

The Kuiper Belt is thought to be the reservoir of ecliptic comets (ECs), which include the Jupiter-family comets (JFCs) and Centaurs. ECs are also the main source of Sun-orbiting impactors on the regular moons of the giant planets (Zahnle et al. 2003). Ironically, we still do not know whether the belt, specifically its Scattered Disk, provides enough ECs (Volk and Malhotra 2008). We are investigating whether cometary breakup in the planetary region (Fernández 2009) can substantially increase the number of ECs. In support of this idea, the Kreutz sungrazers may derive from a hierarchical series of fragmentation events of a progenitor long-period comet (e.g., Sekanina and Chodas 2007), and the JFCs 42P and 53P appear to be fragments of a comet that split in 1845 (Kresák et al. 1984). On the other hand, although 16P was tidally disrupted by Jupiter in 1886, only one fragment survives.Models of the cometary orbital distribution ignore activity or apply a physical lifetime based on the number of passages within 2 or 3 AU of the Sun, where sublimation of water ice occurs (Nesvorný et al. 2017). In reality, some comets (e.g., 29P, Hale-Bopp) are active beyond Jupiter due to volatiles such as CO and CO2 (Womack et al. 2017). 174P/Echeclus underwent a 7-magnitude outburst at 13 AU (Rousselot et al. 2016), and CO emission was detected from Echeclus at 6 AU (Wierzchos et al. 2017). We will estimate how the number and size distribution of comet nuclei change with distance from the Sun due to cometary activity and spontaneous disruption, tidal disruption by a giant planet, and tidal disruption of binaries (Fraser et al. 2017).We thank the Cassini Data Analysis Program for support.Fernández Y (2009). Planet. Space. Sci. 57, 1218.Fraser WC, et al. (2017). Nat. Astron. 1, 0088.Kresák L, et al. (1984). IAU Circular 3940.Nesvorný D, et al. (2017). arXiv:1706.07447.Rousselot P, et al. (2016). MNRAS 462, S432.Sekanina, Z, Chodas, PW (2007). Astrophys. J. 663, 657.Volk K, Malhotra R (2008). Astrophys. J. 687, 714.Wierzchos K, Womack M, Sarid G. (2017). Astron. J. 153, id 230.Womack M, Sarid G, Wierzchos, K (2017). Publ. Astron. Soc. Pac. 129,031001.Zahnle K, et al. (2003). Icarus 163, 263.

Scientific Objectives of Small Carry-on Impactor (SCI) and Deployable Camera 3 Digital (DCAM3-D): Observation of an Ejecta Curtain and a Crater Formed on the Surface of Ryugu by an Artificial High-Velocity Impact

NASA Astrophysics Data System (ADS)

Arakawa, M.; Wada, K.; Saiki, T.; Kadono, T.; Takagi, Y.; Shirai, K.; Okamoto, C.; Yano, H.; Hayakawa, M.; Nakazawa, S.; Hirata, N.; Kobayashi, M.; Michel, P.; Jutzi, M.; Imamura, H.; Ogawa, K.; Sakatani, N.; Iijima, Y.; Honda, R.; Ishibashi, K.; Hayakawa, H.; Sawada, H.

2017-07-01

The Small Carry-on Impactor (SCI) equipped on Hayabusa2 was developed to produce an artificial impact crater on the primitive Near-Earth Asteroid (NEA) 162173 Ryugu (Ryugu) in order to explore the asteroid subsurface material unaffected by space weathering and thermal alteration by solar radiation. An exposed fresh surface by the impactor and/or the ejecta deposit excavated from the crater will be observed by remote sensing instruments, and a subsurface fresh sample of the asteroid will be collected there. The SCI impact experiment will be observed by a Deployable CAMera 3-D (DCAM3-D) at a distance of ˜1 km from the impact point, and the time evolution of the ejecta curtain will be observed by this camera to confirm the impact point on the asteroid surface. As a result of the observation of the ejecta curtain by DCAM3-D and the crater morphology by onboard cameras, the subsurface structure and the physical properties of the constituting materials will be derived from crater scaling laws. Moreover, the SCI experiment on Ryugu gives us a precious opportunity to clarify effects of microgravity on the cratering process and to validate numerical simulations and models of the cratering process.

Crustal stress, seismicity, acoustic emission (AE), and tectonics: the Kefallinì;a (Greece) case study

NASA Astrophysics Data System (ADS)

Gregori, G. P.; Poscolieri, M.; Paparo, G.; Ventrice, G.; de Simone, S.; Rafanelli, C.

2009-04-01

New inferences - confirming previous results (see references)- are presented dealing with a few years Acoustic Emission (AE) records collected at Kefallinìa (Ionian Islands, Greece). A physical distinction between HF (high frequency) vs. LF (low frequency) AE is required. Step-wise changes of the AE underground conductivity are evidenced, and can be suitably handled. "Smooth" results concern (i) the annual variation, (ii) some long-lasting stress "solitons" crossing through the area, and (iii) tidal effects. In particular, every AE station can be operated like a monitoring station both for Earth's tides and for the free oscillations of the Earth. In addition, Kefallinìa exhibits a much peculiar groundwater circulation, in which conduit flow is dominant, that originates a specific (and unique) AE effect. By means of AE time-series analysis, "extreme" or "catastrophic" events can be also monitored and possibly related to relevant tectonic occurrences (either earthquakes, or maybe other occasional phenomena). They can be investigated, and have a regional - rather than local - character. Therefore, every interpretation based on a single station record - being biased by some arbitrariness - can only result indicative. A standardized procedure and software is proposed for routine AE data handling and analysis. References.: Lagios et al., 2004. In Proc. SCI 2004 (The 8th World Multi-Conference on Systemics, Cybernetics and Informatic), Orlando, Florida, July 1004, 6 pp. Poscolieri et al., 2006. In. G. Cello and B. D. Malamud, (eds), 2006. Geol. Soc. London, Special Publ., 261, 63-78. Poscolieri et al., 2006a. Nat. Hazards Earth Syst. Sci., 6, 961-971.

Titan's Gas Behavior During the South Pole Fall

NASA Astrophysics Data System (ADS)

Cottini, Valeria; Nixon, Conor A.; Achterberg, Richard K.; Jennings, Donald E.; Gorius, Nicolas; Irwin, Patrick G. J.

2015-11-01

Titan’s southern middle atmosphere has been showing several changes since the start of fall season in 2009. In 2012 a large cloud appeared [1], [2], [3], temperatures became very low and condensation and gas concentration at the South Pole increased [3], [4].In this work we will show the results of gas abundances retrievals in the South Pole and their latitudinal variation changes as the cold season evolved with time.We analyzed several Cassini Composite InfraRed Spectrometer (CIRS [5]) mid-infrared observations of the South Pole acquired during 2013-2014. The data coordinates were converted in order to be centered on the atmospheric pole and refer to the 1 mbar level and not to the surface. We first determine stratospheric temperatures from the same data and latitudes from the n4 band of methane centered around 1300 cm-1. We retrieve the temperature profiles applying a radiative transfer forward model combined with a non-linear optimal estimation inversion method [6]. We then retrieve the main gases abundances and track their variation with latitude using the same method.Latitudinal changes of the main Titan’s gases - HC3N, C4H2, C6H6, C2H2, C2H4, C3H8 and HCN - show different trends in the Southern polar regions over 2014, when winter was getting closer. We observe a ring-shape in some of the gas abundance distributions, with a local maximum peak around -75 deg of latitude. We also observe an increase of abundance of most of the gases toward the south pole, as seen previously in the North during the winter. The observed increase of benzene over the South Pole is definitely evident and strong. References: [1] West, R. A. et al. (2013) BAAS, 45, 305.03. [2] Jennings, D. E. et al. (2012) ApJ, 754, L3. [3] de Kok, R. et al. (2014), Nature, 514, 7520, 65-67. [4] Vinatier S. et al. (2015) Icarus, Volume 250, p. 95-115. [5] Flasar et al. (2004) Space Sci. Rev., 115, 169-297. [6] Irwin, P.G.J. et al. (2008) J. Quant. Spectrosc. Radiat. Trans., 109, 1136-1150.

Sublimation of Ices Containing Organics and/or Minerals and Implications for Icy Bodies Surface Structure and Spectral Properties

NASA Astrophysics Data System (ADS)

Poch, O.; Pommerol, A.; Jost, B.; Yoldi, Z.; Carrasco, N.; Szopa, C.; Thomas, N.

2015-12-01

The surfaces of many objects in the Solar System comprise substantial quantities of water ice either in pure form or mixed with minerals and/or organic molecules. Sublimation is a process responsible for shaping and changing the reflectance properties of these objects. We present laboratory data on the evolution of the structure and the visible and near-infrared spectral reflectance of icy surfaces made of mixtures of water ice and non-volatile components (complex organic matter and silicates), as they undergo sublimation of the water ice under low temperature and pressure conditions (Poch et al., under review). We prepared icy surfaces which are potential analogues of ices found on comets, icy satellites or trans-neptunian objects (TNOs). The experiments were carried out in the SCITEAS simulation setup recently built as part of the Laboratory for Outflow Studies of Sublimating Materials (LOSSy) at the University of Bern (Pommerol et al., 2015a). As the water ice sublimated, we observed in situ the formation of a sublimation lag deposit, or sublimation mantle, made of the non-volatiles at the top of the samples. The texture (porosity, internal cohesiveness etc.), the activity (outbursts and ejection of mantle fragments) and the spectro-photometric properties of this mantle are found to differ strongly depending on the chemical nature of the non-volatiles, the size of their particles, the way they are mixed with the volatile component and the dust/ice mass ratio. The results also indicate how the band depths of the sub-surface water ice evolve during the build-up of the sublimation mantle. These data provide useful references for interpreting remote-sensing observations of Rosetta (see Pommerol et al., 2015b), and also New Horizons. Poch, O., et al., under review in IcarusPommerol, A., et al., 2015a, Planet. Space Sci. 109-110, 106-122. http://dx.doi.org/10.1016/j.pss.2015.02.004Pommerol, A., et al., 2015b, Astronomy and Astrophysics, in press. http://dx.doi.org/10.1051/0004-6361/201525977

Detectability Factors for Earth-based Imaging of the LCROSS Ejecta Plume

NASA Astrophysics Data System (ADS)

Strycker, Paul D.; Schotte, Jonathan M.; Temme, Ruth L.; Chanover, Nancy J.

2017-10-01

NASA’s Lunar Crater Observation and Sensing Satellite (LCROSS) mission delivered a kinetic impactor into Cabeus Crater on 9 October 2009 [1, 2]. Observing campaigns from Earth-based telescopes at multiple facilities attempted to obtain temporally-resolved imaging of the ejecta plume [3], but no Earth-based imaging detections were reported until 2013 after processing images with Principal Component Analysis (PCA) filtering [4]. Subsequently, PCA filtering has revealed plume detections in two additional cameras and also confirmed a non-detection from one telescope [5, 6]. This combination of detection and non-detection data is useful in determining the criteria for detectability in future observations of transient events. The goal of this work is to identify factors contributing to detectability and to establish thresholds applicable to the LCROSS event. We take the data containing detections and then degrade a specific factor in them until the plume is no longer detectable. These derived thresholds for factors (e.g., scattered light, temporal resolution, spatial resolution, field of view, and signal-to-noise of the illuminated foreground of Cabeus) can be compared to the properties of the actual non-detection data to identify problems specific to its observing conditions or observational setup. The percent differences between the thresholds and both the detection data and non-detection data may also reveal the relative importance of these detectability factors. This work was supported by NASA’s Lunar Data Analysis Program through grant number NNX15AP92G. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona.References: [1] Colaprete, A. et al. (2010) Science, 330, 463-468. [2] Schultz, P. H. et al. (2010) Science, 330, 468-472. [3] Heldmann, J. L. et al. (2012) Space Sci. Rev., 167:93-140, doi:10.1007/s11214-011-9759-y. [4] Strycker, P. D. et al. (2013) Nat. Commun., 4:2620, doi:10.1038/ncomms3620. [5] Temme, R. L. et al. (2016) LPS XLVII, Abstract #1166. [6] Schotte, J. M. et al. (2017) LPS XLVIII, Abstract #1503.

Formation Conditions of Basalts at Gale Crater, Mars from ChemCam Analyses

NASA Astrophysics Data System (ADS)

Filiberto, J.; Bridges, J.; Dasgupta, R.; Edwards, P.; Schwenzer, S. P.; Wiens, R. C.

2015-12-01

Surface igneous rocks shed light onto the chemistry, tectonic, and thermal state of planetary interiors. For the purpose of comparative planetology, therefore, it is critical to fully utilize the compositional diversity of igneous rocks for different terrestrial planets. For Mars, igneous float rocks and conglomerate clasts at Gale Crater, as analyzed by ChemCam [1] using a new calibration [2], have a larger range in chemistry than have been analyzed at any other landing site or within the Martian meteorite collection [3, 4]. These rocks may reflect different conditions of melting within the Martian interior than any previously analyzed basalts. Here we present new formation conditions for basaltic and trachybasalt/dioritic rocks at Gale Crater from ChemCam analyses following previous procedures [5, 6]. We then compare these estimates of basalt formation with previous estimates for rocks from the Noachian (Gusev Crater, Meridiani Planum, and a clast in the NWA 7034 meteorite [5, 6]), Hesperian (surface volcanics [7]), and Amazonian (surface volcanics and shergottites [7-8]), to calculate an average mantle potential temperature for different Martian epochs and investigate how the interior of Mars has changed through time. Finally, we will compare Martian mantle potential temperatures with petrologic estimate of cooling for the Earth. Our calculated estimate for the mantle potential temperature (TP) of rocks at Gale Crater is 1450 ± 45 °C which is within error of previous estimates for Noachian aged rocks [5, 6]. The TP estimates for the Hesperian and Amazonian, based on orbital analyses of the crust [7], are lower in temperature than the estimates for the Noachian. Our results are consistent with simple convective cooling of the Martian interior. [1] Wiens R. et al. (2012) Space Sci Rev 170. 167-227. [2] Anderson R. et al. (2015) LPSC. Abstract #7031. [3] Schmidt M.E. et al. (2014) JGRP 2013JE004481. [4] Sautter V. et al. (2014) JGRP 2013JE004472. [5] Filiberto J. and Dasgupta R. (2011) EPSL 304. 527-537. [6] Filiberto J. and Dasgupta R. (2015) JGRP 2014JE004745. [7] Baratoux D. et al. (2011) Nature 472. 338-341. [8] Musselwhite D.S. et al. (2006) MaPS 41. 1271-1290.

Thermal conductivity measurements of proton-heated warm dense aluminum

NASA Astrophysics Data System (ADS)

McKelvey, A.; Kemp, G.; Sterne, P.; Fernandez, A.; Shepherd, R.; Marinak, M.; Link, A.; Collins, G.; Sio, H.; King, J.; Freeman, R.; Hua, R.; McGuffey, C.; Kim, J.; Beg, F.; Ping, Y.

2017-10-01

We present the first thermal conductivity measurements of warm dense aluminum at 0.5-2.7 g/cc and 2-10 eV, using a recently developed platform of differential heating. A temperature gradient is induced in a Au/Al dual-layer target by proton heating, and subsequent heat flow from the hotter Au to the Al rear surface is detected by two simultaneous time-resolved diagnostics. A systematic data set allows for constraining both thermal conductivity and equation-of-state models. Simulations using Purgatorio model or Sesame S27314 for Al thermal conductivity and LEOS for Au/Al release equation-of-state show good agreement with data after 15 ps. Predictions by other models, such Lee-More, Sesame 27311 and 29373, are outside of experimental error bars. Discrepancy still exists at early time 0-15 ps, likely due to non-equilibrium conditions. (Y. Ping et al. Phys. Plasmas, 2015, A. Mckelvey, et al. Sci. Reports 2017). This work was performed under the auspices of the DOE by LLNL under contract DE-AC52-07NA27344 with support from DOE OFES Early Career program and LLNL LDRD program.

The Phobos Atlas and Geo-portal: geodesy and cartography approach for planetary exploration

NASA Astrophysics Data System (ADS)

Karachevtseva, Irina; Kozlova, Natalia; Kokhanov, Alexander; Oberst, Jürgen; Zubarev, Anatoliy; Nadezhdina, Irina; Patraty, Vyacheslav; Konopikhin, Anatoliy; Garov, Andrey

New Phobos mapping. Methods of image processing and modern GIS technologies provide the opportunity for high quality planetary mapping. The new Phobos DTM and global orthomosaic have been used for developing a geodatabase (Karachevtseva et al., 2012) which provides data for various surface spatial analyses: statistics of crater density, as well as studies of gravity field, geomorphology, and photometry. As mapping is the best way to visualize results of research based on spatial context we created the Phobos atlas. The new Phobos atlas includes: control points network which were calculated during photogrammetry processing of SRC images (Zubarev et al., 2012) and fundamental body parameters as a reference basis for Phobos research as well as GIS analyses of surface objects and geomorphologic studies. According to the structure of the atlas we used various scales and projections based on different coordinate system, including three-axial ellipsoid which parameters (a=13.24 km, b=11.49 km, c=9.48 km) derived from new Phobos shape model (Nadezhdina and Zubarev, 2014). The new Phobos atlas includes about 30 thematic original maps that illustrate the surface of the small body based on Mars Express data (Oberst et al., 2008) and illustrates results of various studies of Phobos:, geomorphology parameters of craters (Basilevsky et al., 2014), morphometry studies (Koknanov et al., 2012), statistics of crater size-frequency distributions based on multi-fractal approach (Uchaev Dm. et al., 2012). Phobos Geo-portal. The spatial data products which used for preparing maps for the Phobos atlas are available at the planetary data storage with access via Geo-portal (http://cartsrv.mexlab.ru/geoportal/), based on modern spatial and web-based technologies (Karachevtseva et al., 2013). Now we are developing Geodesy and Cartography node which can integrate various types of information not only for Phobos data, but other planets and their satellites, and it can be used for geo-spatial support of future missions to celestial bodies. Our technological solutions are open-source, which makes it possible to increase the functionality of the system, for example, using 3D-modeling. Phobos Geo-portal provides access to results of calculation of the gravity field parameters (Uchaev Dm. et al., 2013); catalog of craters and calculations of surface roughness (Karachevtseva et al., 2012); surface compositional studies based on HRSC color-channel data (Patsyn et al., 2012). Acknowledgments: The Phobos study was supported by RBRF under grant for “Geodesy, cartography and research satellites Phobos and Deimos” (Helmholtz-Russia Joint Research Group), grant agreement No. 11-05-91323. References: Basilevsky A.T., Lorenz C.A., Shingareva T.V., Head J.W., Ramsley K.R., Zubarev A.E. Surface Geology and Geomorphology of Phobos, 2014, Elsevier, Planetary and Space Science, in press. Karachevtseva I. P., Shingareva K. B., Konopikhin A. A., Mukabenova B. V., Nadezhdina I. E., Zubarev A. E., 2012. GIS mapping of Phobos on the results of data processing of remote sensing satellite Mars Express, Modern problems of remote sensing of the Earth from Space. Space Research Institute, Moscow, 304-311 (in Russian). Karachevtseva I.P., Oberst J., Zubarev A.E., Nadezhdina I.E., Kokhanov A.A., Garov A. S. Uchaev D.V., Uchaev Dm.V., Malinnikov V.A., Klimkin N.D. 2014, The Phobos information system. Elsevier, Planetary and Space Science. http://dx.doi.org/10.1016/j.pss.2013.12.015 Kokhanov A.A., Basilevsky A.T., Karachevtseva I.P., Nadezhdina I.E., Zubarev A.E. Depth/Diameter Ratio and Inner Walls Steepness of Large Phobos Craters. The 44th Lunar and Planetary Science Conference, The Woodlands, Texas, USA, March 18-22, 2013. Abstracts [#2289]. Nadezhdina I.E., Zubarev A.E. Create reference coordinate network as a basis for studying the physical parameters of Phobos. 2014, Solar System Research, Moscow, Nauka, in press. Oberst J., Schwarz, G., Behnke, T., Hoffmann, H., Matz, K.-D., Flohrer, J., Hirsch, H., Roatsch, T., Scholten, F., Hauber, E., Brinkmann, B., Jaumann, R., Williams, D., Kirk, R., Duxbury, T., Leu, C., Neukum, G., 2008. The imaging performance of the SRC on Mars Express. Planet. Space Sci. 56, 473-491. Patsyn V.S, Malinnikov V.A., Grechishev A.V. Research of spectrometric characteristics of the surface of Phobos on the HRSC data from the Mars Express spacecraft // Modern problems of remote the earth sensing from space, Space Research Institute, Moscow, 2012, V. 9, No. 4, pp. 312-318. (in Russian). Uchaev, Dm.V., Malinnikov, V.A., Oberst, J., 2012. Multifractal approach to crater distribution modelling according to their diameters. Izv. Vyssh. Uchevn. Zaved., Geod. Aerofotos"emka 6, 3-8. (in Russian). Uchaev, Dm.V., Uchaev, D. V., Prutov, I., 2013. Multiscale representation of gravitational fields of small celestial bodies. Izv. Vyssh. Uchevn. Zaved., Geod. Aerofotos"emka 4, 3-8. (In Russian). Zubarev, A. E., Nadezhdina, I.E., Konopikhin, A. A., 2012. Problems of processing of remote sensing data for modeling shapes of small bodies in the Solar system, Modern problems of remote sensing of the Earth from Space. Space Research Institute, Moscow, 277-285 (in Russian).

Lightning impact on micro-second long ionospheric variability

NASA Astrophysics Data System (ADS)

Koh, Kuang Liang; Liu, Zhongjian; Fullekrug, Martin

2017-04-01

Lightning discharges cause electron heating and enhanced ionisation in the D region ionosphere which disturb the transmission of VLF communications [Inan et al., 2010]. A disturbance of such nature was measured in a VLF transmission with a sampling rate of 1 MHz, enabling much faster ionospheric variability to be observed when compared to previous studies which typically report results with a time resolution >5-20ms. The disturbance resembles "Long Recovery Early VLF" (LORE) events [Haldoupis et al. 2013, Cotts & Inan 2007]. LOREs exhibit observable ionospheric effects that last longer (>200s) than other lightning related disturbances. It was proposed that the mechanism behind the long-lasting effects of LOREs is different to shorter events [Gordillo-Vázquez et al. 2016]. The ionospheric variability inferred from the transmitted signal is seen to change dramatically after the lightning onset, suggesting that there are fast processes in the ionosphere affected or produced which have not been considered in previous research. The ionospheric variability inferred from the main two frequencies of the transmission is different. A possible explanation is a difference in the propagation paths of the two main frequencies of the transmission [Füllekrug et al., 2015]. References Inan, U.S., Cummer, S.A., Marshall, R.A., 2010. A survey of ELF and VLF research on lightning-ionosphere interactions and causative discharges. J. Geophys. Res. 115, A00E36. doi:10.1029/2009JA014775 Cotts, B.R.T., Inan, U.S., 2007. VLF observation of long ionospheric recovery events. Geophys. Res. Lett. 34, L14809. doi:10.1029/2007GL030094 Haldoupis, C., Cohen, M., Arnone, E., Cotts, B., Dietrich, S., 2013. The VLF fingerprint of elves: Step-like and long-recovery early VLF perturbations caused by powerful ±CG lightning EM pulses. J. Geophys. Res. Space Physics 118, 5392-5402. doi:10.1002/jgra.50489 Gordillo-Vázquez, F.J., Luque, A., Haldoupis, C., 2016. Upper D region chemical kinetic modeling of LORE relaxation times: KINETIC MODEL OF LORE RELAXATION TIMES. Journal of Geophysical Research: Space Physics 121, 3525-3544. doi:10.1002/2015JA021408 Füllekrug, M., Smith, N., Mezentsev, A., Watson, R., Astin, I., Gaffet, S., Evans, A., Rycroft, M., 2015. Multipath propagation of low-frequency radio waves inferred from high-resolution array analysis. Radio Sci. 50, 2015RS005781. doi:10.1002/2015RS005781

In Situ Analysis of Mars Soil and Rocks Sample with the Sam Gcms Instrumentation Onboard Curiosity : Interpretation and Comparison of Measurements Done during the First Martian Year of Curiosity on Mars

NASA Astrophysics Data System (ADS)

Szopa, C.; Coll, P. J.; Cabane, M.; Buch, A.; Coscia, D.; Millan, M.; Francois, P.; Belmahadi, I.; Teinturier, S.; Navarro-Gonzalez, R.; Glavin, D. P.; Freissinet, C.; Steele, A.; Eigenbrode, J. L.; Mahaffy, P. R.

2014-12-01

The characterisation of the chemical and mineralogical composition of solid surface samples collected with the Curiosity rover is a primary objective of the SAM experiment. These data should provide essential clues on the past habitability of Gale crater. Amongst the SAM suite of instruments [1], SAM-GC (Gas Chromatograph) is devoted to identify and quantify volatiles evolved from the thermal (heating up to about 900°C)/chemical (derivatization procedure) treatment of any soil sample collected by the Curiosity rover. With the aim to search for potential organic molecules outgassed from the samples, SAM-GC analytical channels composed of thermal-desorption injector, and a MXT-CLP or a MXT-Q chromatographic column was chosen to achieve all the measurements done up today, with the aim to separate of a wide range of volatile inorganic and organic molecules. Four solid samples have been analyzed with GCMS, one sand sample collected at the Rocknest site, two rock samples (John Klein and Cumberland respectively) collected at the Yellowknife Bay site using the Curiosity driller, and one rock sample collected at the Kimberly site. All the measurements were successful and they produced complex chromatograms with both detectors used for SAM GC, i.e. a thermal conductivity detector and the SAM quandrupole mass spectrometer. Their interpretation already revealed the presence of an oxychlorine phase present in the sample which is at the origin of chlorohydrocarbons clearly identified [2] but this represents only a fraction of the GCMS signal recorded [3,4]. This work presents a systematic comparison of the GCMS measurements done for the different samples collected, supported by reference data obtained in laboratory with different spare models of the gas chromatograph, with the aim to bring new elements of interpretation of the SAM measurements. References: [1] Mahaffy, P. et al. (2012) Space Sci Rev, 170, 401-478. [2] Glavin, D. et al. (2013), JGR. [3] Leshin L. et al. (2013), Science, [4] Ming D. et al. (2013), Science, 32, 64-67. Acknowledgements: SAM-GC team acknowledges support from the French Space Agency (CNES), French National Programme of Planetology (PNP), National French Council (CNRS), Pierre Simon Laplace Institute, Institut Universitaire de France (IUF) and ESEP Labex, and the great MSL team

Global Controlled Mosaic of Mercury from MESSENGER Orbital Images

NASA Astrophysics Data System (ADS)

Becker, K. J.; Weller, L. A.; Edmundson, K. L.; Becker, T. L.; Robinson, M. S.; Solomon, S. C.

2011-12-01

The MESSENGER spacecraft entered orbit around Mercury in March 2011. Since then, the Mercury Dual Imaging System (MDIS) has been steadily acquiring images from the monochrome, narrow-angle camera (NAC) and the multispectral, wide-angle camera (WAC). With these images, the U.S. Geological Survey (USGS) is constructing a global, controlled monochrome base map of the planet using the Integrated Software for Imagers and Spectrometers (ISIS3) [1]. Although the characterization of MESSENGER spacecraft's navigation and attitude data has proven to be reliable to date, an element of uncertainty in these parameters is unavoidable. This leads to registration offsets between images in the base map. To minimize these errors, images are controlled using a least-squares bundle adjustment that provides refined spacecraft attitude and position parameters plus triangulated ground coordinates of image tie points. As a first effort, 4542 images (2781 NAC, 1761 WAC G filter) have been controlled with a root mean squared error of 0.25 pixels in image space [2]. A preliminary digital elevation model (DEM) is also being produced from the large number of ground points (~ 47,000) triangulated in this adjustment. The region defined by these points ranges from 80°S to 86°N latitude and 158°E to 358°E longitude. A symmetric, unimodal distribution and a dynamic range of 10.5 km characterize the hypsometry of this area. Minimum, maximum, and mean elevations are -5.0, 5.5, and -0.2 km relative to the mean radius of Mercury (2440 km) as defined by the mission. The USGS will use the DEM and base map for the construction of a registered color (WAC) map of high spatial integrity essential for reliable scientific interpretation of the color data. Ongoing improvements to the base map will be made as new images from MDIS become available, providing continuity in resolution, illumination, and viewing conditions. Additional bundle adjustments will further improve spacecraft attitude. The results from further bundle adjustments will ultimately be provided to users in the form of a new, smithed (derived) CK SPICE [3] kernel (C-matrix subsystem dealing with orientation of spacecraft and rotating structures on the spacecraft), replacing the original reconstructed kernel (typically provided by the mission navigation team). The determination of updated attitude parameters for every image acquired by MDIS is a primary goal of the USGS. [1] Anderson, J. A., et al. (2004) Modernization of the Integrated Software for Imagers and Spectrometers, Lunar Planet. Sci. 35, abstract 2039. [2] Edmundson, K. L., et al. (2011), Preliminary photogrammetric control of MESSENGER orbital images of Mercury, GSA Annual Meeting, submitted. [3] Acton, C. H. (1966), Ancillary data services of NASA's Navigation and Ancillary Information Facility, Planet. Space Sci. 44, 65-70.

High resolution Ceres HAMO atlas derived from Dawn FC images

NASA Astrophysics Data System (ADS)

Roatsch, Thomas; Kersten, Elke; Matz, Klaus-Dieter; Preusker, Frank; Scholten, Frank; Jaumann, Ralf; Raymond, Carol A.; Russell, Chris T.

2016-04-01

Introduction: NASA's Dawn spacecraft entered the orbit of dwarf planet Ceres in March 2015, and will characterize the geology, elemental and mineralogical composition, topography, shape, and internal structure of Ceres. One of the major goals of the mission is a global mapping of Ceres. Data: The Dawn mission was mapping Ceres in HAMO (High Altitude Mapping Orbit, 1475 km altitude) between August and October 2015. The framing camera took about 2,600 clear filter images with a resolution of about 140 m/pixel during these cycles. The images were taken with different viewing angles and different illumination conditions. We selected images from one cycle (cycle #1) for the mosaicking process to have similar viewing and illumination conditions. Very minor gaps in the coverage were filled with a few images from cycle #2. Data Processing: The first step of the processing chain towards the cartographic products is to ortho-rectify the images to the proper scale and map projec-tion type. This process requires detailed information of the Dawn orbit and attitude data and of the topography of the targets. Both, improved orientation and a high-resolution shape model, are provided by stereo processing (bundle block adjustment) of the HAMO stereo image dataset [3]. Ceres's HAMO shape model was used for the calculation of the ray intersection points while the map projection itself was done onto the reference sphere of Ceres with a radius of 470 km. The final step is the controlled mosaicking) of all images to a global mosaic of Ceres, the so-called basemap. Ceres map tiles: The Ceres atlas was produced in a scale of 1:750,000 and consists of 15 tiles that conform to the quadrangle scheme proposed by Greeley and Batson [4]. A map scale of 1:750,000 guarantees a mapping at the highest available Dawn resolution in HAMO. The individual tiles were extracted from the global mosaic and reprojected. Nomenclature: The Dawn team proposed 81 names for geological features. By international agreement, craters must be named after gods and goddesses of agriculture and vegetation from world mythology, whereas other geological features must be named after agricultural festivals of the world. The nomenclature proposed by the Dawn team was approved by the IAU [http://planetarynames.wr.usgs.gov/] and is shown in Fig. 1. The entire Ceres HAMO atlas will be available to the public through the Dawn GIS web page [http://dawngis.dlr.de/atlas]. References: [1] Russell, C.T. and Raymond, C.A., Space Sci. Rev., 163, DOI 10.1007/s11214-011-9836-2; [2] Sierks, et al., 2011, Space Sci. Rev., 163, DOI 10.1007/s11214-011-9745-4; [3] Preusker, F. et al., this session; [4] Greeley, R. and Batson, G., 1990, Planetary Mapping, Cambridge University Press.

HamSCI: The Ham Radio Science Citizen Investigation

NASA Astrophysics Data System (ADS)

Frissell, N. A.; Moses, M. L.; Earle, G. D.; McGwier, R. W.; Miller, E. S.; Kaeppler, S. R.; Silver, H. W.; Ceglia, F.; Pascoe, D.; Sinanis, N.; Smith, P.; Williams, R.; Shovkoplyas, A.; Gerrard, A. J.

2016-12-01

Amateur (or "ham") radio operators are individuals with a non-pecuniary interest in radio technology, engineering, communications, science, and public service. They are licensed by their national governments to transmit on amateur radio frequencies. In many jurisdictions, there is no age requirement for a ham radio license, and operators from diverse backgrounds participate. There are more than 740,000 hams in the US, and over 3 million (estimated) worldwide. Many amateur communications are conducted using transionospheric links and thus affected by space weather and ionospheric processes. Recent technological advances have enabled the development of automated ham radio observation networks (e.g. the Reverse Beacon Network, www.reversebeacon.net) and specialized operating modes for the study of weak-signal propagation. The data from these networks have been shown to be useful for the study of ionospheric processes. In order to connect professional researchers with the volunteer-based ham radio community, HamSCI (Ham Radio Science Citizen Investigation, www.hamsci.org) has been established. HamSCI is a platform for publicizing and promoting projects that are consistent with the following objectives: (1) Advance scientific research and understanding through amateur radio activities. (2) Encourage the development of new technologies to support this research. (3) Provide educational opportunities for the amateur community and the general public. HamSCI researchers are working with the American Radio Relay League (ARRL, www.arrl.org) to publicize these objectives and recruit interested hams. The ARRL is the US national organization for amateur radio with a membership of over 170,000 and a monthly magazine, QST. HamSCI is currently preparing to support ionospheric research connected to the 21 Aug 2017 Total Solar Eclipse by expanding coverage of the Reverse Beacon Network and organizing a large-scale ham radio operating event ("QSO Party") to generate data during the eclipse.

SciDB versus Spark: A Preliminary Comparison Based on an Earth Science Use Case

NASA Astrophysics Data System (ADS)

Clune, T.; Kuo, K. S.; Doan, K.; Oloso, A.

2015-12-01

We compare two Big Data technologies, SciDB and Spark, for performance, usability, and extensibility, when applied to a representative Earth science use case. SciDB is a new-generation parallel distributed database management system (DBMS) based on the array data model that is capable of handling multidimensional arrays efficiently but requires lengthy data ingest prior to analysis, whereas Spark is a fast and general engine for large scale data processing that can immediately process raw data files and thereby avoid the ingest process. Once data have been ingested, SciDB is very efficient in database operations such as subsetting. Spark, on the other hand, provides greater flexibility by supporting a wide variety of high-level tools including DBMS's. For the performance aspect of this preliminary comparison, we configure Spark to operate directly on text or binary data files and thereby limit the need for additional tools. Arguably, a more appropriate comparison would involve exploring other configurations of Spark which exploit supported high-level tools, but that is beyond our current resources. To make the comparison as "fair" as possible, we export the arrays produced by SciDB into text files (or converting them to binary files) for the intake by Spark and thereby avoid any additional file processing penalties. The Earth science use case selected for this comparison is the identification and tracking of snowstorms in the NASA Modern Era Retrospective-analysis for Research and Applications (MERRA) reanalysis data. The identification portion of the use case is to flag all grid cells of the MERRA high-resolution hourly data that satisfies our criteria for snowstorm, whereas the tracking portion connects flagged cells adjacent in time and space to form a snowstorm episode. We will report the results of our comparisons at this presentation.

SEP-Kr and SEP-Xe in Lunar Ilmenite and the Ar/Kr/Xe Ratio in the Solar Wind

NASA Astrophysics Data System (ADS)

Wieler, R.; Baur, H.; Signer, P.

1992-07-01

We analyzed all five noble gases in an ilmenite sample from lunar soil 71501 by closed system stepped etching (CSSE), thus extending our CSSE studies of solar noble gases (Wieler et al., 1986; Benkert et al., 1988) to Kr and Xe. He, Ne, Ar isotopes: We observe the familiar presence of two solar noble gas components: step 1 shows ^4He/^3He = 2250, ^20Ne/^22Ne = 13.8, and ^36Ar/^38Ar=5.46. The first two ratios are essentially identical to modern solar wind values (SWC; Geiss, 1973), indicating an isotopically unfractionated SW noble gas reservoir in lunar ilmenite. The Ne data-points of later steps fall on a straight line and reach the SEP-Ne point (^20Ne/^22Ne = 11.3). The slope of this line indicates mass dependent fractionation between SW-Ne and SEP-Ne. SEP-He (^4He/^3He = 4650 +-100) and SEP-Ar (^36Ar/^38Ar = 4.89+-0.05) are also observed (latter two numbers slightly revised compared to Wieler et al., 1992). Kr, Xe isotopes: Kr in those two steps that release pure SW-Ne is very slightly lighter than atmospheric Kr (^86Kr/^84Kr = 0.3041; see also Wieler et al., 1992). We interpret this to be SW-Kr in soil 71501. Steps containing (isotopically heavier) SEP-Ne likewise release heavier Kr, interpreted accordingly as SEP-Kr (^86Kr/^84Kr = 0.323). Similarly, a light Xe component is released first (SW-Xe, ^136Xe/^132Xe = 0.3003), followed by heavier SEP-Xe (^136Xe/^132Xe = 0.319). The data are consistent with both Kr and Xe in SW and SEP components to be related by mass fractionation. The relation first proposed by Benkert et al. (1988) between a ratio R(m(sub)2,m(sub)1) of two isotopes with masses m(sub)2>m(sub)1 in SW and SEP now holds for all five noble gases: (R(sub)SW-R(sub)SEP)/R(sub)SW = (2+-0.13)*(m(sub)2- m(sub)1)/m(sub)2. Since m(sub)2~m(sub)1, this relation may also be written as: R(sub)SEP/R(sub)SW ~ (m(sub)1/m(sub)2)^2 (Geiss and Bochsler, 1991). Element ratios: ^4He/^36Ar and ^20Ne/^36Ar rise from values several times below SWC to essentially SWC ratios in the steps releasing nearly pure SEP gases, indicating element fractionation between SW-He/Ne, but essentially unfractionated SEP-He/Ne/Ar in lunar ilmenite. In contrast, Kr/Xe stays virtually constant (^84Kr/^132Xe = 8.4+-0.5), except in the first few steps. If the light three noble gases indeed are not fractionated in the SEP dominated steps, we would also expect no fractionation for Kr/Xe. The measured ^84Kr/^132Xe ratio is, however, about 2.4 times lower than the most recent "solar system" ratio (Anders and Grevesse, 1989), albeit only ~30% lower than the "solar" value preferred by Marti and Suess (1988). Kr/Xe ratios similar to those in ilmenites have been found earlier, e.g. in Peysanoe (Marti, 1969). They are often taken to indicate fractionated loss of solar noble gases. Based on the new CSSE results, we propose, instead, that lunar ilmenites retain a faithful record of ^84Kr/^132Xe in SW and SEP (and also ^36Ar/^84Kr(sub)SW = 1750+- 300). If so, this may indicate noble gas fractionation in the solar corpuscular radiation, perhaps depending on first ionization potential or a related parameter. Work supported by the Swiss National Science Foundation. References: Anders, E. and Grevesse, N. (1989) Geochim. Cosmochim. Acta. 53, 197-214. Benkert, J.-P. et al. (1988) Lunar Planet. Sci. (abstract) 19, 59-60. Geiss, J. (1973) Proc. 13th Int. Cosmic Ray Conf. 3375-3398. Geiss, J. and Bochsler, P. (1991) In The Sun in Time (eds. C. P. Sonett, M. S. Giampapa and M.S. Matthews), pp. 98-117. Univ. Arizona Press, Tucson, Arizona. Marti, K. (1969) Science. 166. 1263-1265. Marti, K. and Suess, H. E. (1988) Astrophys. Space Sci. 144. 507-517. Wieler, R. et al. (1986) Geochim. Cosmochim. Acta. 50. 1997-2017. Wieler, R. et al. (1992) Lunar Planet. Sci. (abstract) 23.

Tower-scale performance of four observation-based evapotranspiration algorithms within the WACMOS-ET project

NASA Astrophysics Data System (ADS)

Michel, Dominik; Miralles, Diego; Jimenez, Carlos; Ershadi, Ali; McCabe, Matthew F.; Hirschi, Martin; Seneviratne, Sonia I.; Jung, Martin; Wood, Eric F.; (Bob) Su, Z.; Timmermans, Joris; Chen, Xuelong; Fisher, Joshua B.; Mu, Quiaozen; Fernandez, Diego

2015-04-01

Research on climate variations and the development of predictive capabilities largely rely on globally available reference data series of the different components of the energy and water cycles. Several efforts have recently aimed at producing large-scale and long-term reference data sets of these components, e.g. based on in situ observations and remote sensing, in order to allow for diagnostic analyses of the drivers of temporal variations in the climate system. Evapotranspiration (ET) is an essential component of the energy and water cycle, which cannot be monitored directly on a global scale by remote sensing techniques. In recent years, several global multi-year ET data sets have been derived from remote sensing-based estimates, observation-driven land surface model simulations or atmospheric reanalyses. The LandFlux-EVAL initiative presented an ensemble-evaluation of these data sets over the time periods 1989-1995 and 1989-2005 (Mueller et al. 2013). The WACMOS-ET project (http://wacmoset.estellus.eu) started in the year 2012 and constitutes an ESA contribution to the GEWEX initiative LandFlux. It focuses on advancing the development of ET estimates at global, regional and tower scales. WACMOS-ET aims at developing a Reference Input Data Set exploiting European Earth Observations assets and deriving ET estimates produced by a set of four ET algorithms covering the period 2005-2007. The algorithms used are the SEBS (Su et al., 2002), Penman-Monteith from MODIS (Mu et al., 2011), the Priestley and Taylor JPL model (Fisher et al., 2008) and GLEAM (Miralles et al., 2011). The algorithms are run with Fluxnet tower observations, reanalysis data (ERA-Interim), and satellite forcings. They are cross-compared and validated against in-situ data. In this presentation the performance of the different ET algorithms with respect to different temporal resolutions, hydrological regimes, land cover types (including grassland, cropland, shrubland, vegetation mosaic, savanna, woody savanna, needleleaf forest, deciduous forest and mixed forest) are evaluated at the tower-scale in 24 pre-selected study regions on three continents (Europe, North America, and Australia). References: Fisher, J. B., Tu, K.P., and Baldocchi, D.D. Global estimates of the land-atmosphere water flux based on monthly AVHRR and ISLSCP-II data, validated at 16 FLUXNET sites, Remote Sens. Environ. 112, 901-919, 2008. Jiménez, C. et al. Global intercomparison of 12 land surface heat flux estimates. J. Geophys. Res. 116, D02102, 2011. 
 Miralles, D.G. et al. Global land-surface evaporation estimated from satellite-based observations. Hydrol. Earth Syst. Sci. 15, 453-469, 2011. 
 Mu, Q., Zhao, M. & Running, S.W. Improvements to a MODIS global terrestrial evapotranspiration algorithm. Remote Sens. Environ. 115, 1781-1800, 2011. 
 Mueller, B., Hirschi, M., Jimenez, C., Ciais, P., Dirmeyer, P. A., Dolman, A. J., Fisher, J. B., Jung, M., Ludwig, F., Maignan, F., Miralles, D. G., McCabe, M. F., Reichstein, M., Sheffield, J., Wang, K., Wood, E. F., Zhang, Y., and Seneviratne, S. I. (2013). Benchmark products for land evapotranspiration: LandFlux-EVAL multi-data set synthesis. Hydrology and Earth System Sciences, 17, 3707-3720. Mueller, B. et al. Benchmark products for land evapotranspiration: LandFlux-EVAL multi-dataset synthesis. Hydrol. Earth Syst. Sci. 17, 3707-3720, 2013. Su, Z. The Surface Energy Balance System (SEBS) for estimation of turbulent heat fluxes. Hydrol. Earth Syst. Sci. 6, 85-99, 2002.

Formation Of Amino Acids And Nucleotide Bases In A Titan Atmosphere Simulation Experiment

NASA Astrophysics Data System (ADS)

Horst, Sarah; Yelle, R. V.; Buch, A.; Carrasco, N.; Cernogora, G.; Dutuit, O.; Quirico, E.; Sciamma-O'Brien, E.; Smith, M. A.; Somogyi, A.; Szopa, C.; Thissen, R.; Vuitton, V.

2010-10-01

Titan has been a subject of astrobiological interest since the Voyager spacecraft first revealed the diversity of the organic chemistry occurring in the atmosphere. However, it was not until the arrival of Cassini-Huygens that the chemical complexity of Titan's atmosphere was fully appreciated. The Cassini Plasma Spectrometer (CAPS) observed negative ions with m/z values up to 10,000 u/q at 950 km [1] and positive ions with m/z up to 400 u/q [2]. CAPS has also observed O+ flowing into Titan's atmosphere [3]. While Titan's atmosphere is relatively oxygen poor compared to terrestrial planets, CO is the fourth most abundant molecule in the atmosphere (˜50 ppm). The fact that the observed O+ flux is deposited in the region now known to contain large organic molecules leads to the exciting possibility that oxygen can be incorporated into these molecules resulting in the production of prebiotic molecules. In this work, Titan aerosol analogues (or "tholins") produced in PAMPRE, a Titan atmosphere simulation experiment, have been analyzed in a very high resolution LTQ Orbitrap mass spectrometer. These PAMPRE tholins were produced by capacitively coupled RF discharge in a mixture of N2, CH4 and CO. The tholins were found to contain 18 molecules with molecular formulae corresponding to biological amino acids and nucleotide bases. GC-MS measurements have confirmed the structure of seven: adenine, cytosine, uracil, thymine, guanine, glycine and alanine. The production of prebiotic molecules under atmospheric conditions presents a new source of prebiotic material and may increase the range of planets where life could begin. [1] Coates AJ, et al. (2007). Geophys. Res. Lett. 34:22103- +. [2] Crary FJ, et al. (2009). Planet. Space Sci. 57:1847- 1856. [3] Hartle RE, et al. (2006). Geophys. Res. Lett. 33:8201-+.

Radiolytic Gas-Driven Cryovolcanism at Europa

NASA Astrophysics Data System (ADS)

Killen, R. M.; Cooper, J. F.; Sarantos, M.; Sittler, E. C., Jr.

2014-12-01

A large apparent plume of water vapor was detected at the south pole of Europa in December 2012 by the Hubble Space Telescope [Roth et al., 2014] when Europa was near maximum radial distance (apojove) in its orbit around Jupiter. The absence thus far of further detections both at apojove and elsewhere may indicate an episodic source. There was reportedly no evident brightening locally or globally of the Europa oxygen neutral atmosphere coincident with the plume water vapor detection. This could be consistent with an O2-driven cryovolcanism model in which bubbles of trapped gases in the ice crust are released from clathrates on thermal contact with rising oceanic water and expand to force upward fluid flows to the surface. It has long been suggested [Chyba, 2000; Cooper et al., 2001] that the Europa ocean could be oxygenated by radiolytic oxygen from surface irradiation, also implying that the overlying ice crust could be saturated in oxygen clathrates [Hand et al., 2006]. That the moon ocean could be a potentially habitable environment by oxygenation or other processes has been a major motivation for missions to Europa. The radiolytic gas source would be far greater at Europa as compared to much lesser source rates for a similar model at Enceladus [Cooper et al., 2009]. Detected plume emissions could arise from both the directly ejected vapor and from sputtering and/or sublimation of chemically-active plume frost in the polar cap region. Europa's surface gravity is much higher than that of Enceladus, so most of the plume vapor would return to the surface as frost. If sputtering or radiolysis were active contributors to polar cap emissions from the frost, then emissions could also maximize at 6.5-hour intervals as Europa passes through the densest part of the jovian magnetospheric plasma sheet as well as at 85-hour apojove intervals of the orbital period. For comparison to available polar cap plume and global atmospheric observations we present ballistic simulations of the resultant neutral gas density distributions for different source models. Chyba, C., Nature, 403, 381, 2000. Cooper, J. F., et al., Icarus, 149, 133-159, 2001. Cooper, J. F., et al., Plan. Sp. Sci., 57, 1607-1620, 2009. Hand, K. P., et al., Astrobiology, 6, 463-482, 2006. Roth, L., et al., Science, 343, 171-174, 2014.

Evidence for Young Lunar Wrinkle Ridges: Ongoing Tectonic Activity on the Surface of the Moon?

NASA Astrophysics Data System (ADS)

Valantinas, A.; Kinch, K. M.

2017-12-01

The conventional understanding of the Moon states that it is a differentiated but currently a geologically `dead' body. Most of the lunar mare volcanism took place 4-3 Ga ago and basin related extensional tectonics ended 3.6 Ga ago [1]. There is evidence for much younger (0.9Ga -1.2 Ga) volcanic units [2,3] and some degree of contractional tectonics up to 1.2 Ga [4]. Other studies, however, identified evidence for ongoing tectonics based on narrow fractures and several young wrinkle ridges crossing the highlands and small craters [5]. In addition, there is evidence for young (<100 Ma) Irregular Mare Patches (IMPs) but their origin is still debated [6,7]. More recently high resolution images provided by NASA's Lunar Reconnaissance Orbiter revealed a number of surface tectonic expressions such as small graben and lobate scarps were found to be < 100 Ma [8,9]. In our work, we analyze several contractional lunar wrinkle ridge systems which are thought to be manifestations of global stress fields along nearside maria edges [10]. Stratigraphic relationships and the lack of large superimposing craters suggests that all wrinkle ridges in our study regions are Copernican. We derive model ages from crater size frequency distributions which result in ages all below 50 Ma. Analyzed lunar wrinkle ridges appear morphologically crisp and include various degrees of pristine rocky outcrops. High abundances of boulders suggest that they could be still tectonically active because meter size rock populations are obliterated by meteorite bombardment in 300 Ma [11,12]. [1] Basaltic Volcanism Study Project, Basaltic volcanism on the terrestrial planets, 948-974, 1981. [2] Schultz, P. H. & Spudis, P. D., Nature, 302, 184-186, 1983. [3] Hiesinger, H. et al., Geological Society of America Special Papers, 477, 2011.[4] Watters, T. R. & Johnson, C. L., Planetary Tectonics, 121-182, 2010. [5] Schultz, P. H., Moon Morphology, 1976. [6] Schultz, P. H. et al., Nature, 444, 184-186, 2006. [7] Braden, S. E. et al., Nature Geosci., 7, 787-791, 2014. [8] Watters, T. R. et al., Nature Geosci, 5, 181-185, 2012. [9] Clark, J. D. et al., LPSC XLVI, #1730, 2015. [10] Yue, Z. et al., J. Geophys. Res. Planets, 120, 978-994, 2015. [11] Basilevsky, A. T. et al., Planet. Space Sci., 89, 118-126, 2013. [12] Ghent, R. R. et al., Geology, 42, 1059-1062, 2014.

Isotopic and Trace Element Compositions of Antarctic Micrometeorites and Comparison with IDPs

NASA Astrophysics Data System (ADS)

Stadermann, F. J.; Olinger, C. T.

1992-07-01

Antarctic micrometeorites (AMMs) show resemblances and differences to both stratospheric interplanetary dust particles (IDPs) and chondritic meteorites, but the exact nature of this relationship has yet to be established. We measured Ne, H, C, and N isotopic compositions, as well as trace element abundances in several AMMs in order to compare the results to similar measurements of IDPs (Stadermann, 1991). AMMs for this study were collected near Cap-Prudhomme (Maurette et al., 1989), and optically selected (Olinger et al., 1990). Noble gases of 23 selected AMMs were extracted through laser vaporization. Nine of these particles contained implanted solar Ne and one showed a clear signature from spallogenic Ne, confirming their extraterrestrial origin. We selected fragments from 6 of these particles, plus 2 containing apparent Ne excess and one with a roughly chondritic bulk chemistry but immeasurably low Ne, for further analyses. Secondary ion mass spectrometry (SIMS) was used to measure the H, C, and N isotopic compositions. These measurements turned out to be difficult, since the concentrations of H and C in the analyzed samples were significantly lower than in IDPs. The low concentration of C also affected the N isotopic measurements because N could only be measured as CN-. We were able to measure H in 9, as well as C and N in 3 AMMs. All measurements yielded isotopically normal results. Previous determinations of the O isotopic compositions of the same samples (Virag, pers. comm.) also gave no indication of isotopic anomalies. These results are significantly different from measurements of IDPs, where isotopic anomalies in H and N were found in roughly 1/2 and 1/3 of the particles, respectively. SIMS was also used to measure the rare earth and trace element abundances in up to 4 different fragments of 6 AMMs. Although most particles had roughly chondritic abundances, anomalous concentrations were found for Ca, Li, Co, Ni, and Ba. Significant Ca depletions up to 0.03 x C1 were observed in 5 out of 6 particles. This effect is well known from IDPs but nonetheless little understood. Enrichments up to 10 x C1 in Li and up to 100 x C1 in Ba were detected in 4 particles each. The Ba enrichment in AMMs has been observed before and can most likely be attributed to terrestrial contamination (Maurette et al., 1992). The origin of the unusual Li enrichment is unknown. Ni was depleted in all analyzed particles and was strongly correlated with Co, whose depletions relative to C1 were always smaller than for Ni. In the particle with the largest Ni-Co depletion, a melted sphere, this effect was accompanied by an Fe depletion. The Fe/Si, Co/Si and Ni/Si ratios relative to C1 were (0.4, 0.06, 0.02). Similar correlated depletions of Fe, Co, and Ni were also found in 2 out of 13 IDPs with otherwise chondritic abundances (Stadermann, 1991). The ratios of their Fe, Co, Ni depletions were (0.2, 0.07, 0.01) and (0.3, 0.03, 0.01), respectively. Interestingly, these 2 IDPs also contained H with isotopically normal composition and C concentrations that were too low for C and N isotopic measurements. One of these particles was a melted spherule. All these similarities suggest that some AMMs and some IDPs may have close relationships, although AMMs and IDPs in general do not represent the same class of extraterrestrial material. Maurette M. et al. (1989) Lunar Planet. Sci. 20, 644-645. Maurette M. et al. (1992) Lunar Planet. Sci. 23, 859-860. Olinger C.T. et al. (1990) Earth Planet. Sci. Lett. 100, 77-93. Stadermann F.J. (1991) Lunar Planet. Sci. 22, 1311-1312.

Advanced Coatings from Natural-Based Polymers for Metals

DTIC Science & Technology

2000-07-01

Polyimide Interfaces," J. surfaces using a simple dipping-withdrawing coating Vac. Sci. Technol., 3,1390 (1985).converted into the solid layers by heat...Tang, C.H., "Interface Reaction During Metalliza- more, the Al metal in the substrate favorably interacted tion of Cured Polyimide : An XPS Study," 1...property together with its biocompatability was the reason why CS is widely used in biomedical applications, for example, a bacteriostatic agent, a

Flaviviruses

DTIC Science & Technology

1990-01-01

R, Paryanonda A. Human immunoglobulin M anti- virus de lots de moustiques adultes males et femelles. Med body in the serodiagnosis of Japanese...Immun 274. Roche JC, Cordellier R, Hervy JP, et al. Isolement de 96 1984;43:429-43 1. souches de virus dengue 2 a partir de moustiques captures en...dengue chez les moustiques . C R Acad Sci Paris persisting virus. Acta Virol (Praha) 1981 ;25:352-360. 1987;304:347-350. 257. Pool WA, Brownlee A, Wilson

Ab initio Quantum Chemical and Experimental Reaction Kinetics Studies in the Combustion of Bipropellants

DTIC Science & Technology

2017-03-24

NUMBER (Include area code) 24 March 2017 Briefing Charts 01 March 2017 - 31 March 2017 Ab initio Quantum Chemical and Experimental Reaction Kinetics...Laboratory AFRL/RQRS 1 Ara Road Edwards AFB, CA 93524 *Email: ghanshyam.vaghjiani@us.af.mil Ab initio Quantum Chemical and Experimental Reaction ...Clearance 17161 Zador et al., Prog. Energ. Combust. Sci., 37 371 (2011) Why Quantum Chemical Reaction Kinetics Studies? DISTRIBUTION A: Approved for

An Implantable Neuroprosthetic Device to Normalize Bladder Function after SCI

DTIC Science & Technology

2014-12-01

intermittent vagal block using an implantable medical device. Surgery for Obesity and Related Diseases 5, 224-230. 8. Frankenhaeuser B (1960...of vagal blockade to induce weight loss in morbid obesity . Obes Surg 2012;22:1771–1782. 15. Waataja JJ, Tweden KS, Honda CN. Effects of high-frequency...and Rosenblueth 1939; Rosenblueth and Reboul 1939). Recently this nerve block method has been applied to treat obesity (Camilleri et al. 2009; Wattaja

An analysis of sponge genomes.

PubMed

Costantini, Maria

2004-11-24

The genome of sponges has only been investigated so far by Bartmann-Lindholm et al. [Progr. Colloid. Polym. Sci. 107 (1997) 122-126] who reported a multimodal CsCl profile which could be resolved into five peaks for Geodia cydonium. This problem was reinvestigated here on both G. cydonium and Suberites domuncula. It was shown that DNAs from both sponges are characterized by unimodal CsCl profiles, additional peaks being due to contaminating prokaryotic and eukaryotic microorganisms.

HgCdTe Surface and Defect Study Program.

DTIC Science & Technology

1983-07-01

RESkSTIVITY. Rm T 10 12 10> 9 i0 1 0 9 I i i i i TI/Au TI AI/Ni Ti/Ni In GATE METAL Figure 8. The Effect of Gate " fetal Type on dc Resistivity of 1500.4...2. J.A. Wilson, V.A. Cotton, J.A. Silkerman, 0. Lacer , W.E. Spicer and P. Morgen, J. Vac. Sci. Tech., Al (1983), 1719. 3. B.K. Janorsek, R.C

Diel Variation in Beaked Whale Diving Behavior

DTIC Science & Technology

2008-01-01

While our results are only from a single study area and our sample size is small, diving patterns of these two species appear very stereotypic ...sharks of the genus Isistius (McSweeney et al. 2007). Cookie-cutter sharks are thought to exhibit diel vertical migrations, spending time near the...Mar. Mamm. Sci. 23: 666-687. 17 Mead, J.G. 1989. Beaked whales of the genus Mesoplodon. Pages 349-430 In S.H. Ridgway and R. Harrison

Role of p53 in Mammary Epithelial Cell Senescence

DTIC Science & Technology

2009-05-01

Cellular Senescence and Skin Aging . In Skin Aging Handbook: Market Perspectives, Pharmacology, Formulation, and Evaluation Techniques, ed., N. Dayan...identifies senescent human cells in culture and in aging skin in vivo. Proc Natl Acad Sci U S A, 1995. 92(20): p. 9363-7. 12. Dimri, G.P., et al...NIH): ZAI1- BDP- I(J2), RFA-AI-08-012 ( Rejuvenating the Aged Immune System) 2009: Online Reviewer USAMRMC BCRP Concept

Evolutionary Dynamics on Protein Bi-stability Landscapes can Potentially Resolve Adaptive Conflicts

PubMed Central

Sikosek, Tobias; Bornberg-Bauer, Erich; Chan, Hue Sun

2012-01-01

Experimental studies have shown that some proteins exist in two alternative native-state conformations. It has been proposed that such bi-stable proteins can potentially function as evolutionary bridges at the interface between two neutral networks of protein sequences that fold uniquely into the two different native conformations. Under adaptive conflict scenarios, bi-stable proteins may be of particular advantage if they simultaneously provide two beneficial biological functions. However, computational models that simulate protein structure evolution do not yet recognize the importance of bi-stability. Here we use a biophysical model to analyze sequence space to identify bi-stable or multi-stable proteins with two or more equally stable native-state structures. The inclusion of such proteins enhances phenotype connectivity between neutral networks in sequence space. Consideration of the sequence space neighborhood of bridge proteins revealed that bi-stability decreases gradually with each mutation that takes the sequence further away from an exactly bi-stable protein. With relaxed selection pressures, we found that bi-stable proteins in our model are highly successful under simulated adaptive conflict. Inspired by these model predictions, we developed a method to identify real proteins in the PDB with bridge-like properties, and have verified a clear bi-stability gradient for a series of mutants studied by Alexander et al. (Proc Nat Acad Sci USA 2009, 106:21149–21154) that connect two sequences that fold uniquely into two different native structures via a bridge-like intermediate mutant sequence. Based on these findings, new testable predictions for future studies on protein bi-stability and evolution are discussed. PMID:23028272

Erratum: Correction to: Water in the Earth's Interior: Distribution and Origin

NASA Astrophysics Data System (ADS)

Peslier, Anne H.; Schönbächler, Maria; Busemann, Henner; Karato, Shun-Ichiro

2017-10-01

Correction to: Space Sci Rev DOI: 10.1007/s11214-017-0387-z This article has been corrected. Figure 3 was initially published with erroneous axis titles in Fig. 3B and 3D where the x axis should be Cpx H2O, instead of Grt H2O.

Capture myopathy in a free-flying greater sandhill crane (Grus canadensis tabida) from Wisconsin

USGS Publications Warehouse

Windingstad, R.M.; Hurley, S.S.; Sileo, L.

1983-01-01

Capture myopathy has been reported Frequently in wild mammals (Bartsch et al., 1977, Vet. Pathol. 14: 314-324). There are, however, fewer reports of this disease in wild birds (Young, 1967, mt. Zoo Yearb. 7: 226-227; Bartsch et al., 1977, op. cit. ; Henschel and Low, 1978, S. Afr. J. Sci. 74: 305-306; Wobeser, 1981, Diseases of Wild Waterfowl, Plenum Press, New York, 300 pp.). We are reporting a case of skeletal muscle necrosis in a greater sandhill crane found dead 5 days after its capture, radio-tagging, and release. We believe this is the first case of capture myopathy to be reported for this species.

Mysteries of R ik = 0: A novel paradigm in Einstein's theory of gravitation

NASA Astrophysics Data System (ADS)

Vishwakarma, Ram Gopal

2014-02-01

Despite a century-long effort, a proper energy-stress tensor of the gravitational field, could not have been discovered. Furthermore, it has been discovered recently that the standard formulation of the energy-stress tensor of matter, suffers from various inconsistencies and paradoxes, concluding that the tensor is not consistent with the geometric formulation of gravitation [Astrophys. Space Sci., 2009, 321: 151; Astrophys. Space Sci., 2012, 340: 373]. This perhaps hints that a consistent theory of gravitation should not have any bearing on the energy-stress tensor. It is shown here that the so-called "vacuum" field equations R ik = 0 do not represent an empty spacetime, and the energy, momenta and angular momenta of the gravitational and the matter fields are revealed through the geometry, without including any formulation thereof in the field equations. Though, this novel discovery appears baffling and orthogonal to the usual understanding, is consistent with the observations at all scales, without requiring the hypothetical dark matter, dark energy or inflation. Moreover, the resulting theory circumvents the long-standing problems of the standard cosmology, besides explaining some unexplained puzzles.

Towards modelling of water inflow into the mantle

NASA Astrophysics Data System (ADS)

Thielmann, M.; Eichheimer, P.; Golabek, G.

2017-12-01

The transport and storage of water in the mantle significantly affects various material properties of mantle rocks and thus water plays a key role in a variety of geodynamical processes (tectonics, magmatism etc.) Geological and seismological observations suggest different inflow mechanisms of water via the subducting slab like slab bending, thermal cracking and serpentinization (Faccenda et al., 2009; Korenaga, 2017). Most of the previous numerical models do not take different dip angles of the subduction slab and subduction velocities into account, while nature provides two different types of subduction regimes i.e. shallow and deep subduction (Li et al., 2011). To which extent both parameters influence the inflow and outflow of water in the mantle still remains unclear. For the investigation of the inflow and outflow of fluids e.g. water in the mantle, we use high resolution 2D finite element simulations, which allow us to resolve subducted sediments and crustal layers. For this purpose the finite element code MVEP2 (Kaus, 2010), is tested against benchmark results (van Keken et al., 2008). In a first step we reproduced the analytical cornerflow model (Batchelor, 1967) used in the benchmark of van Keken et al.(2008) as well as the steady state temperature field. Further steps consist of successively increasing model complexity, such as the incorporation of hydrogen diffusion, water transport and dehydration reactions. ReferencesBatchelor, G. K. An Introduction to Fluid Dynamics. Cambridge University Press, Cambridge, UK (1967) van Keken, P. E., et al. A community benchmark for subduction zone modeling. Phys. Earth Planet. Int. 171, 187-197 (2008). Faccenda, M., T.V. Gerya, and L. Burlini. Deep slab hydration induced by bending-related variations in tectonic pressure. Nat. Geosci. 2, 790-793 (2009). Korenaga, J. On the extent of mantle hydration caused by plate bending. Earth Planet. Sci. Lett. 457, 1-9 (2017). Li, Z. H., Xu, Z. Q., and T.V. Gerya. Flat versus steep subduction: Contrasting modes for the formation and exhumation of high- to ultrahigh-pressure rocks in continental collision zones. Earth Planet. Sci. Lett. 301, 65-77 (2011). Kaus, B. J. P. Factors that control the angle of shear bands in geodynamic numerical models of brittle deformation. Tectonophys. 484, 36-47 (2010). The transport and storage of water in the mantle significantly affects various material properties of mantle rocks and thus water plays a key role in a variety of geodynamical processes (tectonics, magmatism etc.) Geological and seismological observations suggest different inflow mechanisms of water via the subducting slab like slab bending, thermal cracking and serpentinization (Faccenda et al., 2009; Korenaga, 2017). Most of the previous numerical models do not take different dip angles of the subduction slab and subduction velocities into account, while nature provides two different types of subduction regimes i.e. shallow and deep subduction (Li et al., 2011). To which extent both parameters influence the inflow and outflow of water in the mantle still remains unclear. For the investigation of the inflow and outflow of fluids e.g. water in the mantle, we use high resolution 2D finite element simulations, which allow us to resolve subducted sediments and crustal layers. For this purpose the finite element code MVEP2 (Kaus, 2010), is tested against benchmark results (van Keken et al., 2008). In a first step we reproduced the analytical cornerflow model (Batchelor, 1967) used in the benchmark of van Keken et al.(2008) as well as the steady state temperature field.Further steps consist of successively increasing model complexity, such as the incorporation of hydrogen diffusion, water transport and dehydration reactions. Systematic simulations are performed to assess the influence of different model parameters on various target parameters such as dehydration depth, volcanic line position etc., the ultimate goal being the derivation of scaling laws for water transport in the mantleReferencesBatchelor, G. K. An Introduction to Fluid Dynamics. Cambridge University Press, Cambridge, UK (1967)van Keken, P. E., et al. A community benchmark for subduction zone modeling. Phys. Earth Planet. Int. 171, 187-197 (2008). Faccenda, M., T.V. Gerya, and L. Burlini. Deep slab hydration induced by bending-related variations in tectonic pressure. Nat. Geosci. 2, 790-793 (2009). Korenaga, J. On the extent of mantle hydration caused by plate bending. Earth Planet. Sci. Lett. 457, 1-9 (2017). Li, Z. H., Xu, Z. Q., and T.V. Gerya. Flat versus steep subduction: Contrasting modes for the formation and exhumation of high- to ultrahigh-pressure rocks in continental collision zones. Earth Planet. Sci. Lett. 301, 65-77 (2011). Kaus, B. J. P. Factors that control the angle of shear bands in geodynamic numerical models of brittle deformation. Tectonophys. 484, 36-47 (2010).

Variable diffusion rates during exsolution coarsening in the presence of fluids.

NASA Astrophysics Data System (ADS)

Putnis, Andrew; Prent, Alexander

2017-04-01

The scale of exsolution textures in mineral solid solutions has long been used as an indicator of thermal history during cooling. The theory of spinodal decomposition in an anisotropic solid and subsequent coarsening of exsolution textures as a function of temperature and cooling rate is well developed (see Petrishcheva et al., 2009 and Abart et al., 2009 for a review of the Cahn-Hilliard theory). For the case of exsolution in the alkali feldspar solid solution [(Na,K)AlSi3O8] the characteristic texture shows compositional fluctuations in Na,K with a wavelength that depends on the cooling rate. The cooling rate is determined from knowledge of the Na-K interdiffusion coefficient, assuming that the unmixing is simply due to the interdiffusion of Na and K in an otherwise fixed tetrahedral Al,Si framework. Cryptoperthites and mesoperthites with a periodic lamellar microstructure are considered to be the end-result of such a solid-state exsolution process. Later-stage fluid infiltration results in patch perthites that are formed at a sharp replacement front by a dissolution-precipitation mechanism (Parsons et al., 2015). Patch perthites have an easily recognizable texture and are clear indicators of a reaction with an aqueous solution. The distinction is thus drawn between crypto- and meso-perthite showing periodic lamellae, associated with a solid-state exsolution process, and the patch perthite showing irregular domains of Na-rich and K-rich feldspars associated with a fluid mediated reprecipitation process. However, the presence of fluids can also enhance the coarsening of lamellar exsolution textures, retaining an apparently solid-state microstructure but with a length scale that is dependent on local recrystallization driven by fluid infiltration. Examples will be given from alkali feldspars in granitic rocks where it is clearly demonstrable that cooling rates cannot be inferred from such exsolution textures. The variability in Na,K diffusion rates and thus different length scales of exsolution are likely to be due to the efficiency of diffusional transport through a fluid phase, which is influenced by differences in fluid-induced micro- and nano-porosity. Abart R. et al. (2009) Am. J. Sci. 309, 450-475. Petrishcheva E. and Abart R. (2009) Am. J. Sci, 309, 431-449. Parsons I. et al., (2015) Am. Min. 100, 1277-1303.

Characterizing the Nature and Distribution of Phytolith Organic Matter Using Raman Spectroscopy

NASA Astrophysics Data System (ADS)

Gallagher, K. L.; Alfonso-Garcia, A.; Sanchez, J.; Harutyunyan, A.; Santos, G.; Potma, E.

2014-12-01

Many plants, including grasses and some important human food sources, accumulate and precipitate silica in their cells to form opaline phytoliths. These phytoliths contain small amounts of organic matter (OM) that is trapped during the process of silicification and protected from oxidation. If this OM is derived solely from photosynthesis during the life of the plant, it should preserve an isotopic signature of the atmosphere and the type of photosynthetic pathway [1]. However, radiocarbon dating of this OM gives an older age than expected [2], and studies on modern plants indicate a soil contribution to phytolith OM [3,4]. Thus, a better understanding of the role of phytolith OM and the silica precipitation mechanism is needed. Previous work has suggested that plant silica is associated with compounds such as proteins, lipids, lignin and phenol-carbohydrate complexes [5-7]. It is not known whether these compounds are cellular components passively encapsulated as the cell silicified, polymers actively involved in the precipitation process or random compounds assimilated by the plant and discarded into a "glass wastebasket". Here, we used Raman spectroscopy to map individual phytoliths isolated from Sorghum bicolor plants. We showed that OM in phytoliths is heterogeneously distributed and not related to optical features (i.e. dark spots or holes visible in light microscopy) commonly thought to be the repository for phytolith OM (corroborated by nanoSIMS [8]). The Raman spectra showed peaks at 2970-2960, 2945, and 2906 cm-1, indicative of C-H stretching modes, and further peaks at 1600, 1440, 1410, and 1350 cm-1 consistent with lignins and other OM. These peaks exhibited variability of relative intensities both within and between phytoliths. We will discuss these findings in the context of silica biomineralization in plants, mechanistic implications, and isotopic paleo-reconstructions using phytolith OM. 1. Jones, R.L. and A. Beavers, Soil Sci., 1963. 96(6): 375. 2. Santos, G.M., et al., Biogeosci. , 2012. 9(5): 1873. 3. Ryerson, P. et al, in prep. 4. Gallagher, K.L. et al, in prep. 5. Elbaum, R., et al., Quat. Int., 2009. 193:11. 6. Inanaga, S., et al., Soil Sci. and Plant Nut., 1995. 41:111. 7. Zhang, C.C., et al., Plant Soil, 2013. 372(1-2): 137. 8. Alexandre, et al., submitted.

On the Chemical Emergence of Phosphate-Based Biochemistry

NASA Astrophysics Data System (ADS)

Kee, Terence

Contemporary organisms use orthophosphate derivatives (PO43-) in their cell biochemistry,1 yet questions remain as to how Nature was able to accumulate, activate and exploit the or-thophosphate group from geological sources with both poorly solubility and low chemical activ-ity.2 Gulick argued3 a central role for reduced oxidation state phosphorus (P) oxyacids such as H-phosphonates (H2PO3-) and especially H-phosphinates (H2PO2-) in prebiotic chemistry on account of the greater water solubility of their metal salts and, with the presence of P-H bonds, a different reactivity profile to that expected of orthophosphate. The recent demonstration that hydrothermal corrosion of P-rich mineral phases such as schreibersite (Fe,Ni)3P within iron meteorites leads to production of various P-oxyacids including H-phosphonic (H3PO3)4 and H-phosphinic5 acids as well as orthophosphate has reignited interest in reduced oxida-tion state P chemistry in prebiotic environments. We are examining the prebiotic potential of reduced oxidation state P-chemistry through reactions with carbonyl substrates with rea-sonable prebiotic provenance including formaldehyde glycolaldehyde, both intimately involved in the formose reaction for sugar synthesis6 and pyruvic acid,7 a product of glycolysis and feed-stock for the citric acid cycle, a fundamental cellular metablic process whose heritage is considered an ancient one. In this contribution we present some of our latest results on the H-phosphinate-pyruvate system. References: [1] Lodish H et al. (2000) Molecular Cell Biology, 4th Ed., W. H. Freeman Co., New York. [2] Gulick A. (1955) Am. Sci., 43, 479. [3] Gulick A. (1957) Ann. N. Y. Acad. Sci. 69, 309. [4] Pasek M. A. (2008) Proc. Nat. Acad. Sci. USA, 105, 853. [5] Bryant D. E.and Kee T. P. (2006) Chem. Commun. 2344. [6] Weber A. L. (2000) Origins of Life and Evol. Biosph., 30, 33. [7] Cody G. D. et. al. (2000) Science 289, 1337.

Study of the coma of comet 67P/Churyumov-Gerasimenko based on the ROSINA/RTOF instrument onboard Rosetta

NASA Astrophysics Data System (ADS)

Hoang, M.; Garnier, P.; Lasue, J.; Reme, H.; Altwegg, K.; Balsiger, H. R.; Bieler, A. M.; Calmonte, U.; Fiethe, B.; Galli, A.; Gasc, S.; Gombosi, T. I.; Jäckel, A.; Mall, U.; Le Roy, L.; Rubin, M.; Tzou, C. Y.; Waite, J. H., Jr.; Wurz, P.

2015-12-01

The ROSETTA spacecraft of ESA is in the environment of comet 67P/Churyumov-Gerasimenko since August 2014. Among the experiments onboard the spacecraft, the ROSINA experiment (Rosetta Orbiter Spectrometer for Ion and Neutral Analysis) includes two mass spectrometers (DFMS and RTOF) to analyze the composition of neutrals and ions, and a pressure sensor (COPS) to monitor the density and velocity of neutrals in the coma [1]. We will here analyze and discuss the data of the ROSINA/RTOF instrument during the comet escort phase. The Reflectron-type Time-Of-Flight (RTOF) mass spectrometer possesses a wide mass range and a high temporal resolution [1,2]. It was designed to measure cometary neutral gas as well as cometary ions. A detailed description of the main volatiles (H2O, CO2, CO) dynamics and of the heterogeneities of the coma will then be provided. The influence of various parameters on the coma measurements is investigated on a statistical basis, with the parameters being distance to the comet, heliocentric distance, longitude and latitude of nadir point. Our analysis of the northern hemisphere summer season shows the presence of water vapor mostly in the illuminated northern hemisphere near the neck region with cyclic diurnal variations whereas CO2 was confined to the cold southern hemisphere with a more spatially homogeneous composition, in agreement with previous observations of 67P [2] or Hartley 2 [3]. A comparison will also be provided with the COPS total density and DFMS abundance measurements. [1] Balsiger et al., "ROSINA - Rosetta Orbiter Spectrometer for Ion and Neutral Analysis", Space Sci. Rev., 2007. [2] Scherer et al., "A novel principle for an ion mirror design in time-of-flight mass spectrometry," Int. Jou. Mass Spectr., 2006. [3] Hässig et al., "Time variability and heterogeneity in the coma of 67P/Churyumov-Gerasimenko", Science, 2015. [4] A'Hearn et al., "EPOXI at comet Hartley 2", Science, 2011.

ALMA observation of Ceres' Surface Temperature.

NASA Astrophysics Data System (ADS)

Titus, T. N.; Li, J. Y.; Sykes, M. V.; Ip, W. H.; Lai, I.; Moullet, A.

2016-12-01

Ceres, the largest object in the main asteroid belt, has been mapped by the Dawn spacecraft. The mapping includes measuring surface temperatures using the Visible and Infrared (VIR) spectrometer at high spatial resolution. However, the VIR instrument has a long wavelength cutoff at 5 μm, which prevents the accurate measurement of surface temperatures below 180 K. This restricts temperature determinations to low and mid-latitudes at mid-day. Observations from the Atacama Large Millimeter/submillimeter Array (ALMA) [1], while having lower spatial resolution, are sensitive to the full range of surface temperatures that are expected at Ceres. Forty reconstructed images at 75 km/beam resolution were acquired of Ceres that were consistent with a low thermal inertia surface. The diurnal temperature profiles were compared to the KRC thermal model [2, 3], which has been extensively used for Mars [e.g. 4, 5]. Variations in temperature as a function of local time are observed and are compared to predictions from the KRC model. The model temperatures are converted to radiance (Jy/Steradian) and are corrected for near-surface thermal gradients and limb effects for comparison to observations. Initial analysis is consistent with the presence of near-surface water ice in the north polar region. The edge of the ice table is between 50° and 70° North Latitude, consistent with the enhanced detection of hydrogen by the Dawn GRaND instrument [6]. Further analysis will be presented. This work is supported by the NASA Solar System Observations Program. References: [1] Wootten A. et al. (2015) IAU General Assembly, Meeting #29, #2237199 [2] Kieffer, H. H., et al. (1977) JGR, 82, 4249-4291. [3] Kieffer, Hugh H., (2013) Journal of Geophysical Research: Planets, 118(3), 451-470. [4] Titus, T. N., H. H. Kieffer, and P. N. Christensen (2003) Science, 299, 1048-1051. [5] Fergason, R. L. et al. (2012) Space Sci. Rev, 170, 739-773[6] Prettyman, T. et al. (2016) LPSC 47, #2228.

Stratigraphy in the Samarkand Sulci Region of Enceladus

NASA Astrophysics Data System (ADS)

Roatsch, T.; Wagner, R. J.; Schmedemann, N.; Helfenstein, P.; Stephan, K.; Voigt, J.; Jaumann, R.; Giese, B.; Porco, C.

2016-12-01

Saturn's cryovolcanically active moon Enceladus is a primary target for NASA's Cassini Saturn orbiter. In a flyby on Dec. 19, 2015 (orbit 228EN), images with 65 m spatial resolution were taken from the Samarkand Sulci and Anbar Fossae [1] region with the Cassini ISS NAC camera. This study area was geologically mapped, based on the geological context by [2]. Crater counts for age dating were carried out and compared to our previous counts done in a global mosaic at lower resolution [3]. A stereo-derived digital elevation model reveals intense tectonic faulting causing a remarkable height range of up to 1750 meters with respect to the surrounding cratered plains [4]. Relative ages of geologic units can be inferred from mutual crosscutting and/or superposition, but ages from craters counts are comparably uncertain due to low crater frequencies and small areas of measurement. Tectonic features of the study area cut through older densely cratered plains with model ages ranging from 3.9 Gyr to only 500 Ma, depending of impact chronology model [5, and ref's therein] applied to crater frequency measurements. In the units characterized by intense tectonism, larger craters like those found in the cratered plains in parts have survived but smaller much less frequent craters reflect the age of tectonic resurfacing, with model ages ranging from 1.5 Gyr to 15 Myr. Geologic units which show putative small craters (number < 3) at the given resolution have considerably low estimated (maximum) ages on the order of << 10 Myr suggesting intense tectonism has been taking place in the recent past. References: [1] Roatsch, T., et al. (2013), Planet. Space Sci. 77, 118-125. [2] Crow-Willard, E. N., and Pappalardo, R. T. (2015), JGR 120, doi:10.1002/2015JE004818. [3] Jaumann R., et al. (2011), EPSC Abstracts Vol. 6, abstr. No. EPSC-DPS2011-435-1. [4] Giese B., et al. (2016), paper in preparation. [5] Dones, L., et al. (2009), In: Saturn from Cassini-Huygens, Springer Publ., pp. 613-635.

Joint aerosol and water-leaving radiance retrieval from Airborne Multi-angle SpectroPolarimeter Imager

NASA Astrophysics Data System (ADS)

Xu, F.; Dubovik, O.; Zhai, P.; Kalashnikova, O. V.; Diner, D. J.

2015-12-01

The Airborne Multiangle SpectroPolarimetric Imager (AirMSPI) [1] has been flying aboard the NASA ER-2 high altitude aircraft since October 2010. In step-and-stare operation mode, AirMSPI typically acquires observations of a target area at 9 view angles between ±67° off the nadir. Its spectral channels are centered at 355, 380, 445, 470*, 555, 660*, and 865* nm, where the asterisk denotes the polarimetric bands. In order to retrieve information from the AirMSPI observations, we developed a efficient and flexible retrieval code that can jointly retrieve aerosol and water leaving radiance simultaneously. The forward model employs a coupled Markov Chain (MC) [2] and adding/doubling [3] radiative transfer method which is fully linearized and integrated with a multi-patch retrieval algorithm to obtain aerosol and water leaving radiance/Chl-a information. Various constraints are imposed to improve convergence and retrieval stability. We tested the aerosol and water leaving radiance retrievals using the AirMSPI radiance and polarization measurements by comparing to the retrieved aerosol concentration, size distribution, water-leaving radiance, and chlorophyll concentration to the values reported by the USC SeaPRISM AERONET-OC site off the coast of Southern California. In addition, the MC-based retrievals of aerosol properties were compared with GRASP ([4-5]) retrievals for selected cases. The MC-based retrieval approach was then used to systematically explore the benefits of AirMSPI's ultraviolet and polarimetric channels, the use of multiple view angles, and constraints provided by inclusion of bio-optical models of the water-leaving radiance. References [1]. D. J. Diner, et al. Atmos. Meas. Tech. 6, 1717 (2013). [2]. F. Xu et al. Opt. Lett. 36, 2083 (2011). [3]. J. E. Hansen and L.D. Travis. Space Sci. Rev. 16, 527 (1974). [4]. O. Dubovik et al. Atmos. Meas. Tech., 4, 975 (2011). [5]. O. Dubovik et al. SPIE: Newsroom, DOI:10.1117/2.1201408.005558 (2014).

Coupled Retrieval of Aerosol Properties and Surface Reflection Using the Airborne Multi-angle SpectroPolarimetric Imager (AirMSPI)

NASA Astrophysics Data System (ADS)

Xu, F.; van Harten, G.; Kalashnikova, O. V.; Diner, D. J.; Seidel, F. C.; Garay, M. J.; Dubovik, O.

2016-12-01

The Airborne Multi-angle SpectroPolarimetric Imager (AirMSPI) [1] has been flying aboard the NASA ER-2 high altitude aircraft since October 2010. In step-and-stare operation mode, AirMSPI acquires radiance and polarization data at 355, 380, 445, 470*, 555, 660*, 865*, and 935 nm (* denotes polarimetric bands). The imaged area covers about 10 km by 10 km and is observed from 9 view angles between ±67° off of nadir. We have developed an efficient and flexible code that uses the information content of AirMSPI data for a coupled retrieval of aerosol properties and surface reflection. The retrieval was built based on the multi-pixel optimization concept [2], with the use of a hybrid radiative transfer model [3] that combines the Markov Chain [4] and adding/doubling methods [5]. The convergence and robustness of our algorithm is ensured by applying constraints on (a) the spectral variation of the Bidirectional Polarization Distribution Function (BPDF) and angular shape of the Bidirectional Reflectance Distribution Function (BRDF); (b) the spectral variation of aerosol optical properties; and (c) the spatial variation of aerosol parameters across neighboring image pixels. Our retrieval approach has been tested using over 20 AirMSPI datasets having low to moderately high aerosol loadings ( 0.02550-nm< 0.45) and acquired during several field campaigns. Results are compared with AERONET aerosol reference data. We also explore the benefits of AirMSPI's ultraviolet and polarimetric bands as well as the use of multiple view angles. References[1]. D. J. Diner, et al. Atmos. Meas. Tech. 6, 1717 (2013). [2]. O. Dubovik et al. Atmos. Meas. Tech. 4, 975 (2011). [3]. F. Xu et al. Atmos. Meas. Tech. 9, 2877 (2016). [4]. F. Xu et al. Opt. Lett. 36, 2083 (2011). [5]. J. E. Hansen and L.D. Travis. Space Sci. Rev. 16, 527 (1974).

Geologic mapping of the saturnian satellites based on Cassini ISS images: objectives, methods, and results

NASA Astrophysics Data System (ADS)

Wagner, R.; Roatsch, T.; Giese, B.; Wolf, U.; Neukum, G.

Remote Sensing of the Earth and Planets, Freie Universitaet Berlin, Germany Data set and objectives: Since the Cassini Orbiter has been inserted into orbit around Saturn on July 1, 2004, image data of the major saturnian satellites were collected by the Cassini ISS narrow and wide angle cameras (NAC and WAC respectively) at resolutions up to 10 - 20 m/pxl [1]. Up to now, the surface of each one of these satellites was imaged at least once at distances less than 20000 km. The extended image coverage and much higher resolution compared to Voyager images from more than two decades ago help to define (1) the global distribution of geologic units at regional map scale (100 - 300 m/pxl), (2) to identify units of possibly cryovolcanic origin, (3) to map tectonic landforms in detail, and (4) to use the crater size-frequency distributions measured on geologic units for relative and absolute age dating. Also (5), the stratigraphic column for each satellite can be subdivided into time-stratigraphic systems by the combination of stratigraphy and crater frequency measurements. Methods: All geologic maps are produced on image base maps put together from images of various flybys at each satellite [2]. Geologic units are identified by their specific albedo and morphology. In some cases, topographic data and digital elevation models are available. Cratering chronology models are used to derive absolute model ages from crater size-frequency measurements [3]. Important stratigraphic markers (and their associated crater frequencies and ages) which can be used to subdivide the geological history of a specific satellite are (1) volcanic flows, (2) prominent tectonic landforms, (3) large impact features, such as basins, and (4) craters with extended ray systems. Results: In this paper we focus on regional geologic maps of Dione and Rhea, two neighbours in orbit, and of Enceladus. Dione and Rhea, 1124 and 1538 km in diameter, are characterized (a) by densely cratered plains, (b) smooth, less densely cratered plains, and (3) by tectonic features, mostly horst and graben structures [4][5][6]. Cratering model ages of the densely cratered plains are on the order of 4.2 Gyr [6]. The surface of Rhea appears to be more densely cratered and hence older than the one of Dione. Also, Rhea has a higher abundance of large impact features several 100 km in diameter while only one such basin was found on Dione [6][7]. Ray craters are not abundant at crater sizes larger than 20 km except for one feature found on Rhea. Enceladus (502 km in diameter) shows a wide range of geologic units and surface ages. Densely cratered plains with ages on the order of 4 Gyr are cut by tectonic bands of ridges and grooves with various model ages ranging from 1 to more than 3 Gyr [6]. In the south polar terrain, areas almost devoid of craters and with cratering model ages much less than 4 Myr 1 reveal on-going geologic processes which recently were confirmed by the discovery of cryovolcanic activity on this moon [6][8]. References: [1] Porco, C. C. et al., Space Sci. Rev. 115, 363-497, 2004. [2] Roatsch, T. et al., Planet. Space Sci., in press, 2006. [3] Neukum G. et al., 40th ESLAB Symposium, May 8-12, 2006, abstract book, 235, 2006. [4] Plescia, J., Icarus 56, 401-413, 1983. [5] Moore, J., Icarus 59, 205-220, 1984. [6] Wagner, R. et al., LPSC XXXVII, abstr. No. 1805 [CD-Rom], 2006. [7] Stooke, P. J., LPSC XXXIII, abstr. No. 1553 [CD-Rom], 2002. [8] Porco, C. C. et al., Science 311, 1393-1401, 2006. 2