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1

Wavelet Measurement Suggests Cause of Period Instability in Mammalian Circadian  

E-print Network

Wavelet Measurement Suggests Cause of Period Instability in Mammalian Circadian Neurons Kirsten cells as either arrhythmic or circadian, our wavelet analysis reveals that individual cells, when removed from network interac- tions, intermittently express circadian and/or longer infradian periods. We

Petzold, Linda R.

2

Periodic Properties and Inquiry: Student Mental Models Observed during a Periodic Table Puzzle Activity  

ERIC Educational Resources Information Center

The mental models of both novice and advanced chemistry students were observed while the students performed a periodic table activity. The mental model framework seems to be an effective way of analyzing student behavior during learning activities. The analysis suggests that students do not recognize periodic trends through the examination of…

Larson, Kathleen G.; Long, George R.; Briggs, Michael W.

2012-01-01

3

Multispacecraft observations of quasi-periodic emissions  

NASA Astrophysics Data System (ADS)

Quasi-periodic (QP) emissions are VLF electromagnetic waves in the frequency range of about 0.5-5 kHz which exhibit a periodic time modulation of the wave intensity. The modulation period is usually on the order of a few tens of seconds. The generation mechanism of these emissions is still not understood, but at least in some cases it appears to be related to ULF magnetic field pulsations which result in periodic modifications of the resonant conditions in the source region. We use multipoint measurements of QP emissions by the 4 Cluster spacecraft. The observations are obtained close to the equatorial region at radial distances of about 4 Earth radii, i.e. close to a possible generation region. A combined analysis of the high resolution data obtained by the WBD instruments and the ULF magnetic field data obtained by the FGM instruments allows for a detailed case-study analysis of these unique emissions. The presented analysis benefits from the recent close-separation configuration of three of the Cluster spacecraft (?20-100 km) and a related timing analysis, which would be impossible otherwise.

Nemec, Frantisek; Picket, Jolene S.; Santolik, Ondrej

2014-05-01

4

Photometric Observation And Period Study of GO Cygni  

E-print Network

Photometric observations of GO Cyg were performed during the July-October 2002, in B and V bands of Johnson system. Based on Wilson's model, the light curve analysis were carried out to find the photometric elements of the system. The O-C diagram which is based on new observed times of minima suggests a negative rate of period variation (dP/dt<0) for the system.

S. M. Zabihinpoor; A. Dariush; N. Riazi

2005-08-07

5

Cumulative dose on fractional delivery of tomotherapy to periodically moving organ: A phantom QA suggestion  

SciTech Connect

This study was conducted to evaluate the cumulative dosimetric error that occurs in both target and surrounding normal tissues when treating a moving target in multifractional treatment with tomotherapy. An experiment was devised to measure cumulative error in multifractional treatments delivered to a horseshoe-shaped clinical target volume (CTV) surrounding a cylinder shape of organ at risk (OAR). Treatments differed in jaw size (1.05 vs 2.5 cm), pitch (0.287 vs 0.660), and modulation factor (1.5 vs 2.5), and tumor motion characteristics differing in amplitude (1 to 3 cm), period (3 to 5 second), and regularity (sinusoidal vs irregular) were tested. Treatment plans were delivered to a moving phantom up to 5-times exposure. Dose distribution on central coronal plane from 1 to 5 times exposure was measured with GAFCHROMIC EBT film. Dose differences occurring across 1 to 5 times exposure of treatment and between treatment plans were evaluated by analyzing measurements of gamma index, gamma index histogram, histogram changes, and dose at the center of the OAR. The experiment showed dose distortion due to organ motion increased between multiexposure 1 to 3 times but plateaued and remained constant after 3-times exposure. In addition, although larger motion amplitude and a longer period of motion both increased dosimetric error, the dose at the OAR was more significantly affected by motion amplitude rather than motion period. Irregularity of motion did not contribute significantly to dosimetric error when compared with other motion parameters. Restriction of organ motion to have small amplitude and short motion period together with larger jaw size and small modulation factor (with small pitch) is effective in reducing dosimetric error. Pretreatment measurements for 3-times exposure of treatment to a moving phantom with patient-specific tumor motion would provide a good estimation of the delivered dose distribution.

Shin, Eunhyuk [Department of Radiation Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Department of Nuclear Engineering, Hanyang University, Seoul (Korea, Republic of); Han, Youngyih, E-mail: youngyih@skku.edu [Department of Radiation Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Park, Hee-Chul, E-mail: hee.ro.Park@samsung.com [Department of Radiation Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Sung Kim, Jin; Hwan Ahn, Sung; Suk Shin, Jung; Gyu Ju, Sang; Ho Choi, Doo [Department of Radiation Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Lee, Jaiki [Department of Nuclear Engineering, Hanyang University, Seoul (Korea, Republic of)

2013-01-01

6

Observations of low energy interplanetary electrons. [Jovian origin suggested by temporal behavior  

NASA Technical Reports Server (NTRS)

Observations of the temporal behavior of low energy (0.16-6 MeV) at 1 AU are reported. The electron intensity is found to vary by a factor of more than five from one quiet time to another, including short-term enhancements of the type reported at higher electron energies. Over a period of about four months, beginning with the time at which the interplanetary field line first connects earth and Jupiter, the magnitude and frequency of the increases grow abruptly and remain high. The observed longitudinal distribution of Jovian electrons could be the result of the interconnection of the interplanetary field with an extended Jovian magnetotail.

Mewaldt, R. A.; Stone, E. C.; Vogt, R. E.

1975-01-01

7

Optimizing observing sequence design for periodic and non-periodic phenomena : a Bayesian approach  

NASA Technical Reports Server (NTRS)

In this paper we report on our progress on addressing these issues. We have developed an approximate expression for the uniformity of phase coverage that can be used when scheduling to assess candidate sample times. We describe the results obtained using this estimator, and compare them with detailed simulations. We describe our progress and plans for integrating optimizing criteria for both periodic and non-periodic observations into a single observation sequence.

Johnston, Mark D.; Knight, Russell

2005-01-01

8

Some Long-period Variations of BLZ Latitude Observations  

NASA Astrophysics Data System (ADS)

We made a new reduction, in the FK5 reference frame, of the original Belgrade zenith--telescope observations (BLZ) in the period 1949-1985 (37 years). It was a part of the Hipparcos programme. The Commission 19 of the IAU formed WG ERHRF (the Working Group on Earth Rotation in the HIPPARCOS reference frame) to collect the optical astrometric observations and to analyse them in that reference system. Our investigations are in line with it. The formal and external errors of BLZ (new reduction) are less than before. An analysis and some results of the long-period variations of BLZ latitude are presented here.

Damljanovic, G.

9

Observations of long period earthquakes accompanying hydraulic fracturing  

Microsoft Academic Search

Waveforms of most seismic events accompanying hydraulic fracturing have been reported to contain clear P and S waves and have fault plane solutions consistent with shear displacement across a fault. This observation is surprising since classical hydraulic fracturing theory predicts the creation of a tensile opening of a cavity in response to fluid pressure. Very small long period events, similar

Dorthe Bame; Michael Fehler

1986-01-01

10

Phylogeny and oscillating expression of period and cryptochrome in short and long photoperiods suggest a conserved function in Nasonia vitripennis  

PubMed Central

Photoperiodism, the ability to respond to seasonal varying day length with suitable life history changes, is a common trait in organisms that live in temperate regions. In most studied organisms, the circadian system appears to be the basis for photoperiodic time measurement. In insects this is still controversial: while some data indicate that the circadian system is causally involved in photoperiodism, others suggest that it may have a marginal or indirect role. Resonance experiments in the parasitic wasp Nasonia vitripennis have revealed a circadian component in photoperiodic time measurement compatible with a mechanism of internal coincidence where a two components oscillator system obtains information from dawn and dusk, respectively. The identity of this oscillator (or oscillators) is still unclear but possible candidates are the oscillating molecules of the auto-regulatory feedback loops in the heart of the circadian system. Here, we show for the first time the circadian oscillation of period and cryptochrome mRNAs in the heads of Nasonia females kept under short and long photoperiods. Period and cryptochrome mRNA levels display a synchronous oscillation in all conditions tested and persist, albeit with reduced amplitude, during the first day in constant light as well as constant darkness. More importantly, the signal for the period and cryptochrome oscillations is set by the light-on signal. These results, together with phylogenetic analyses, indicate that Nasonia’s period and cryptochrome display characteristics of homologous genes in other hymenopteran species. PMID:24758403

van de Zande, Louis; Beukeboom, Leo W.; Beersma, Domien G. M.

2014-01-01

11

Coronal Field Opens at Lower Height During the Solar Cycles 22 and 23 Minimum Periods: IMF Comparison Suggests the Source Surface Should Be Lowered  

NASA Astrophysics Data System (ADS)

The solar cycle 23 minimum period has been characterized by a weaker solar and interplanetary magnetic field. This provides an ideal time to study how the strength of the photospheric field affects the interplanetary magnetic flux and, in particular, how much the observed interplanetary fields of different cycle minima can be understood simply from differences in the areas of the coronal holes, as opposed to differences in the surface fields within them. In this study, we invoke smaller source surface radii in the potential-field source-surface (PFSS) model to construct a consistent picture of the observed coronal holes and the near-Earth interplanetary field strength as well as polarity measurements for the cycles 23 and 22 minimum periods. Although the source surface value of 2.5 R ? is typically used in PFSS applications, earlier studies have shown that using smaller source surface heights generates results that better match observations during low solar activity periods. We use photospheric field synoptic maps from Mount Wilson Observatory (MWO) and find that the values of ? 1.9 R ? and ? 1.8 R ? for the cycles 22 and 23 minimum periods, respectively, produce the best results. The larger coronal holes obtained for the smaller source surface radius of cycle 23 somewhat offsets the interplanetary consequences of the lower magnetic field at their photospheric footpoints. For comparison, we also use observations from the Michelson Doppler Imager (MDI) and find that the source surface radius of ? 1.5 R ? produces better results for cycle 23, rather than ? 1.8 R ? as suggested from MWO observations. Despite this difference, our results obtained from MWO and MDI observations show a qualitative consistency regarding the origins of the interplanetary field and suggest that users of PFSS models may want to consider using these smaller values for their source surface heights as long as the solar activity is low.

Lee, C. O.; Luhmann, J. G.; Hoeksema, J. T.; Sun, X.; Arge, C. N.; de Pater, I.

2011-04-01

12

The ECMWF reanalysis of the MAP Special Observing Period  

NASA Astrophysics Data System (ADS)

A reanalysis of the Mesoscale Alpine Programme (MAP) Special Observing Period (7 September to 15 November 1999) was performed at the European Centre for Medium-Range Weather Forecasts (ECMWF). Substantial upgrades in the global data assimilation system 4D-Var (T511/159L60, horizontal resolution approximately 40 km) combined with special MAP observations provide a new reference description for studies on mountain-related atmospheric phenomena. The MAP observations used in the MAP reanalysis comprise European windprofilers, high-resolution radiosondes and surface observations. The assimilation of MAP observations results in a slight weakening of the cyclonic flow over central Europe and of the mid-tropospheric westerly wind over the Alpine region. Also, MAP observations lead to moister conditions in the southern Alpine region, southern France and over the Adriatic Sea. The comparison of forecast daily rainfall from the MAP reanalysis with observed precipitation totals averaged over the Po catchment shows good agreement in timing and rain amount. Investigations of some Intensive Observation Periods (IOPs) illustrate specific aspects of the MAP reanalysis. Different precipitation patterns characteristic of different flow regimes are well captured (IOP2b and IOP8). The assimilation of windprofilers rectifies the divergent wind field, but changes can erroneously feed back on the humidity field (IOP2a) because of the way the humidity analysis is performed (a modified humidity analysis was introduced at ECMWF in 2003). Validation with model-independent Global Positioning System (GPS) derived integrated water-vapour contents shows that the humidity field describes well the inter-diurnal humidity variations at southern Alpine GPS stations. However, the reanalysis appears to be slightly too dry compared with GPS measurements.

Keil, Christian; Cardinali, Carla

2004-10-01

13

The Changing Surface of Saturn's Titan: Cassini Observations Suggest Active Cryovolcanism  

NASA Astrophysics Data System (ADS)

R. M. Nelson(1), L. Kamp(1), R. M. C. Lopes(1), D. L. Matson(1), S. D. Wall(1), R. L. Kirk(2), K. L Mitchell(1), G. Mitri(1), B. W. Hapke(3), M. D. Boryta(4), F. E. Leader(1) , W. D. Smythe(1), K. H. Baines(1), R. Jauman(5), C. Sotin(1), R. N. Clark(6), D. P. Cruikshank(7) , P. Drossart(9), B. J. Buratti(1) , J.Lunine(8), M. Combes(9), G. Bellucci(10), J.-P. Bibring(11), F. Capaccioni(10), P. Cerroni(10), A. Coradini(10), V. Formisano(10), G Filacchione(10), R. Y. Langevin(11), T. B. McCord(12), V. Mennella(13), P. D. Nicholson(14) , B. Sicardy(8) 1-JPL, 4800 Oak Grove Drive, Pasadena CA 91109, 2-USGS, Flagstaff, 3-U Pittsburgh, 4-Mt. Sac Col, 5- DLR, Berlin, 6-USGS Denver, 7-NASA AMES, 8-U Paris-Meudon, 9-Obs de Paris, 10-ISFI-CNR Rome, 11-U Paris -Sud. Orsay, 12-Bear Flt Cntr Winthrop WA, 13-Obs Capodimonte Naples, 14-Cornell U. Several Instruments on the Cassini Saturn Orbiter have been observing the surface of Saturn's moon Titan since mid 2004. The Visual and Infrared Mapping Spectrometer (VIMS) reports that regions near 26oS, 78oW (region 1) and 7oS, 138oW (region 2) exhibit photometric changes consistent with on-going surface activity. These regions are photometrically variable with time(1). Cassini Synthetic Aperture Rader (SAR) has investigated these regions and reports that both of these regions exhibit morphologies consistent with cryovolcanism (2). VIMS observed region 1 eight times and reported that on two occasions the region brightened two-fold and then decreased again on timescales of several weeks. Region 2 was observed on four occasions (Tb-Dec13/2004 ,T8-Oct27/2005, T10-Jan15/2006, T12-Mar18/2006) and exhibited a pronounced change in I/F betweenT8 and T10. Our photometric analysis finds that both regions do not exhibit photometric properties consistent with atmospheric phenomena such as tropospheric clouds. These changes must be at or very near the surface. Radar images of these regions reveal morphology that is consistent with cryovolcanoes. We conclude that the VIMS instrument has found two instances in which selected regions on Titan's surface became unusually reflective and remained reflective on time scales of days to months. In both cases the area of reflectance variability is large (~100000 sq km), larger than either Loki or the Big Island of Hawaii. This is a strong evidence for currently active surface processes on Titan. Pre-Cassini, Titan was thought of as a pre-biotic earth that was frozen in time. Cassini VIMS and SAR observations combined suggest that Titan is the present day is not frozen solid, and is instead an episodically changing or evolving world. References: [1] Nelson R. M. et al, LPSC 2007 , Europlanets 2007, AGU 2007, EGU 2008, Accepted in Icarus 2008. [2] Lopes et al (this meeting), Stofan et al. Icarus 185, 443-456, 2007. Lopes et al. Icarus 186, 395- 412, 2007. Kirk et al., DPS 2007. Acknowledgement: This work done at JPL under contract with NASA

Nelson, R. M.

2008-12-01

14

Countergradient heat flux observations during the evening transition period  

NASA Astrophysics Data System (ADS)

Gradient-based turbulence models generally assume that the buoyancy flux ceases to introduce heat into the surface layer of the atmospheric boundary layer in temporal consonance with the gradient of the local virtual potential temperature. Here, we hypothesize that during the evening transition a delay exists between the instant when the buoyancy flux goes to zero and the time when the local gradient of the virtual potential temperature indicates a sign change. This phenomenon is studied using a range of data collected over several intensive observational periods (IOPs) during the Boundary Layer Late Afternoon and Sunset Turbulence field campaign conducted in Lannemezan, France. The focus is mainly on the lower part of the surface layer using a tower instrumented with high-speed temperature and velocity sensors. The results from this work confirm and quantify a flux-gradient delay. Specifically, the observed values of the delay are ~ 30-80 min. The existence of the delay and its duration can be explained by considering the convective timescale and the competition of forces associated with the classical Rayleigh-Bénard problem. This combined theory predicts that the last eddy formed while the sensible heat flux changes sign during the evening transition should produce a delay. It appears that this last eddy is decelerated through the action of turbulent momentum and thermal diffusivities, and that the delay is related to the convective turnover timescale. Observations indicate that as horizontal shear becomes more important, the delay time apparently increases to values greater than the convective turnover timescale.

Blay-Carreras, E.; Pardyjak, E. R.; Pino, D.; Alexander, D. C.; Lohou, F.; Lothon, M.

2014-09-01

15

''Very Carefully Managed'': Advice and Suggestions in Post-Observation Meetings  

ERIC Educational Resources Information Center

This study examined the discourse of teacher supervision/mentoring, specifically within the context of the post-observation meeting. The analysis of six transcripts of post-observation meetings from one semester in a small university Intensive English Program revealed a variety of politeness strategies employed by supervisors in the delivery of…

Vasquez, Camilla

2004-01-01

16

Countergradient heat flux observations during the evening transition period  

NASA Astrophysics Data System (ADS)

Gradient-based turbulence models generally assume that the buoyancy flux ceases to introduce heat into the surface layer of the atmospheric boundary layer in temporal consonance with the gradient of the local virtual potential temperature. Here, we hypothesize that during the evening transition a delay exists between the instant when the buoyancy flux goes to zero and the time when the local gradient of the virtual potential temperature indicates a sign change. This phenomenon is studied using a range of data collected over several Intensive Observational Periods (IOPs) during the Boundary Layer Late Afternoon and Sunset Turbulence field campaign conducted in Lannemezan, France. The focus is mainly on the lower part of the surface layer using a tower instrumented with high-speed temperature and velocity sensors. The results from this work confirm and quantify a flux-gradient delay. Specifically, the observed values of the delay are ~30-80 min. The existence of the delay and its duration can be explained by considering the convective time scale and the competition of forces associated with the classical Rayleigh-Bénard problem. This combined theory predicts that the last eddy formed while the sensible heat flux changes sign during the evening transition should produce a delay. It appears that this last eddy is decelerated through the action of turbulent momentum and thermal diffusivities, and that the delay is related to the convective turn - over time - scale. Observations indicate that as horizontal shear becomes more important, the delay time apparently increases to values greater than the convective turnover time-scale.

Blay-Carreras, E.; Pardyjak, E. R.; Pino, D.; Alexander, D. C.; Lohou, F.; Lothon, M.

2014-03-01

17

Are Dietary Restraint Scales Valid Measures of Acute Dietary Restriction? Unobtrusive Observational Data Suggest Not  

ERIC Educational Resources Information Center

The finding that dietary restraint scales predict onset of bulimic pathology has been interpreted as suggesting that dieting causes this eating disturbance, despite the dearth of evidence that these scales are valid measures of dietary restriction. The authors conducted 4 studies that tested whether dietary restraint scales were inversely…

Stice, Eric; Fisher, Melissa; Lowe, Michael R.

2004-01-01

18

Are Dietary Restraint Scales Valid Measures of Acute Dietary Restriction? Unobtrusive Observational Data Suggest Not  

Microsoft Academic Search

The finding that dietary restraint scales predict onset of bulimic pathology has been interpreted as suggesting that dieting causes this eating disturbance, despite the dearth of evidence that these scales are valid measures of dietary restriction. The authors conducted 4 studies that tested whether dietary restraint scales were inversely correlated with unobtrusively measured caloric intake. These studies, which varied in

Eric Stice; Melissa Fisher; Michael R. Lowe

2004-01-01

19

Quasi-Periodic Pulsations with Varying Period in Multi-Wavelength Observations of an X-class Flare  

NASA Astrophysics Data System (ADS)

This work presents an interesting phenomenon of the period variation in quasi-periodic pulsations (QPPs) observed during the impulsive phase of a coronal mass ejection-related X1.1 class flare on 2012 July 6. The period of QPPs was changed from 21 s at soft X-rays (SXR) to 22-23 s at microwaves, to ~24 s at extreme ultraviolet emissions (EUV), and to 27-32 s at metric-decimetric waves. The microwave, EUV, and SXR QPPs, emitted from flare loops of different heights, were oscillating in phase. Fast kink mode oscillations were proposed to be the modulation mechanism, which may exist in a wide region in the solar atmosphere from the chromosphere to the upper corona or even to the interplanetary space. Changed parameters of flare loops through the solar atmosphere could result in the varying period of QPPs at different wavelengths. The first appearing microwave QPPs and quasi-periodic metric-decimetric type III bursts were generated by energetic electrons. This may imply that particle acceleration or magnetic reconnection were located between these two non-thermal emission sources. Thermal QPPs (in SXR and EUV emissions) occurred later than the nonthermal ones, which would suggest a some time for plasma heating or energy dissipation in flare loops during burst processes. At the beginning of flare, a sudden collapse and expansion of two separated flare loop structures occurred simultaneously with the multi-wavelength QPPs. An implosion in the corona, including both collapse and expansion of flare loops, could be a trigger of loop oscillations in a very large region in the solar atmosphere.

Huang, Jing; Tan, Baolin; Zhang, Yin; Karlický, Marian; Mészárosová, Hana

2014-08-01

20

Periodic magnetopause oscillations observed with the GOES satellites on March 24, 1991  

NASA Technical Reports Server (NTRS)

The GOES 6 and 7 satellites were in the dayside magnetosphere late on March 24, 1991, when the magnetopause moved in to geosynchronous orbit. Observations on GOES 6 near 1030 local time (LT) indicated six inward and outward periodic movements of the magnetopause past the satellite over a 30-min interval. Later the magnetopause moved farther in, placing GOES 6 (1100 LT) in the magnetosheath and then moving in past GOES 7, near 1245 LT. The periodic oscillations of the magnetopause at GOES 6 suggest surface waves propagating toward the dawn flank of the magnetopause.

Cahill, L. J., Jr.; Winckler, J. R.

1992-01-01

21

Cybersemiotics: A suggestion for a transdisciplinary framework for description of observing, anticipatory and meaning producing systems  

Microsoft Academic Search

The ability of systems to be anticipatory seems to be intricate connected with the ability to observe and to cognate by reducing complexity through signification. The semantic capacity of living systems, the cognitive ability to assign meaning to differences perturbating the system's self-organization, seems to be the prerequisite for the phenomenon of communication, language and consciousness. In cybernetics Bateson developed

Soren Brier

1998-01-01

22

Non-linear dynamic of singular long-period volcanic tremors observed at Mt. Asama  

Microsoft Academic Search

On September 1, 2004, a middle-scale eruption occurred at Mt.Asama. Before the eruption, we observed three long-period tremors with singular waveforms, which occurred at 4:25, 11:30, and 20:30 on June 24, 2004. The common characteristic of these tremors is that the tip of the waveform is sharp. This sharp-pointed waveform may suggest a non-linear dynamics of the source process. In

M. Takeo

2007-01-01

23

Examining Periodic Solar-Wind Density Structures Observed in the SECCHI Heliospheric Imagers  

NASA Technical Reports Server (NTRS)

We present an analysis of small-scale, periodic, solar-wind density enhancements (length scales as small as approximately equals 1000 Mm) observed in images from the Heliospheric Imager (HI) aboard STEREO-A. We discuss their possible relationship to periodic fluctuations of the proton density that have been identified at 1 AU using in-situ plasma measurements. Specifically, Viall, Kepko, and Spence examined 11 years of in-situ solar-wind density measurements at 1 AU and demonstrated that not only turbulent structures, but also nonturbulent, periodic density structures exist in the solar wind with scale sizes of hundreds to one thousand Mm. In a subsequent paper, Viall, Spence, and Kasper analyzed the alpha-to-proton solar-wind abundance ratio measured during one such event of periodic density structures, demonstrating that the plasma behavior was highly suggestive that either temporally or spatially varying coronal source plasma created those density structures. Large periodic density structures observed at 1 AU, which were generated in the corona, can be observable in coronal and heliospheric white-light images if they possess sufficiently high density contrast. Indeed, we identify such periodic density structures as they enter the HI field of view and follow them as they advect with the solar wind through the images. The smaller, periodic density structures that we identify in the images are comparable in size to the larger structures analyzed in-situ at 1 AU, yielding further evidence that periodic density enhancements are a consequence of coronal activity as the solar wind is formed.

Viall, Nicholeen M.; Spence, Harlan E.; Vourlidas, Angelos; Howard, Russell

2010-01-01

24

Spectroscopic observations of evolving flare ribbon substructure suggesting origin in current sheet waves  

NASA Astrophysics Data System (ADS)

A flare ribbon is the chromospheric image of reconnection at a coronal current sheet. The dynamics and structure of the ribbon can thus reveal properties of the current sheet, including motion of the reconnecting flare loops. We present imaging and spectroscopic observations from the Interface Region Imaging Spectrograph (IRIS) of the evolution of a flare ribbon at high spatial resolution and time cadence. These reveal small-scale substructure in the ribbon, which manifest as oscillations in both position and Doppler velocities. We consider various alternative explanations for these oscillations, including modulation of chromospheric evaporation flows. Among these we find the best support for some form of elliptical wave localized to the coronal current sheet, such as a tearing mode or Kelvin-Helmholtz instability.IRIS is a NASA Small Explorer mission developed and operated by Lockheed Martin Solar and Astrophysics Laboratory. This work is supported by contract 8100002702 from Lockheed Martin to Montana State University, a Montana Space Grant Consortium fellowship, and by NASA through HSR.

Brannon, Sean R.; Longcope, Dana; Qiu, Jiong

2015-04-01

25

Recurrence times and periodicities in 4U 1608-52 as observed by Vela 5B  

NASA Technical Reports Server (NTRS)

We report on the Vela 5B 10 year history of the soft X-ray transient 4U 1608-52, and on the characteristics of its soft X-ray outbursts. The Vela 5B satellite observed the four known outbursts in 1975, 1977, and 1979, and four new outbursts in 1970 and 1971, altering the recurrence pattern of outbursts from this source. One of the 1970 outbursts is symmetric in its intensity profile, while the two outbursts in 1971 have short exponential profiles separated by 80 days. Despite suggestive recurrence periods of approximately 85 and approximately 150 days evident in the time intervals between the outbursts, there is no single statistically significant recurrence time on which the outbursts recur consistently. In the 1970 symmetric event, there is evidence for a period of either 4.10 or 5.19 days. Drawing upon the analogy with SU Ursa Majoris dwarf novae, we suggest that the short period is orbital and any longer period would be associated with a precession period of the accretion disk.

Lochner, James C.; Roussel-Dupre, Diane

1994-01-01

26

Cybersemiotics: A suggestion for a transdisciplinary framework for description of observing, anticipatory and meaning producing systems  

NASA Astrophysics Data System (ADS)

The ability of systems to be anticipatory seems to be intricate connected with the ability to observe and to cognate by reducing complexity through signification. The semantic capacity of living systems, the cognitive ability to assign meaning to differences perturbating the system's self-organization, seems to be the prerequisite for the phenomenon of communication, language and consciousness. In cybernetics Bateson developed the idea that information is a difference that makes a difference and second order cybernetics developed the concept of organisms as self-organized and self-produced systems (autopoietic) as the prerequisite of life and cognition. The cognitive ability seems to be qualitative different from what so far is computable on any known machine although parts of different aspects of the process can be partly simulated in AI, neutral network and AL. In semiotics the fundamental process of cognition and communication is called semiosis or signification and C. S. Peirce created a special triadic, objective idealistic, pragmatic and evolutionary philosophy to be able to give a fruitful description of the process and its relation to logic and the concept of natural law. Both second order cybernetics and semiotics sees information and meaning as something produced by individual organisms through structural couplings to the environments or other individuals through historical drift and further developed in social communication. Luhmann points out that social communication also only functions through structural couplings which he calls generalized media such as science, art, power, love and money. Peirce talks of the semiotic net as a triadic view of meanings developing through history and in animals through evolution. In accordance with this Wittgenstein points out that signification is created in language games developed in specific life forms. Life forms are the things we do in society such as seducing, commanding and explaining. As animals do not have language in the true sense I have extended his concept into ethology and bio-semiotics by talking of sign games related to specific motivations and innate response mechanisms. Life as such seems to be an anticipatory function generating expectations through evolution through open genetic programs as Konrad Lorenz pointed out. The phenomenon of imprinting in ducks for instance is a standard example of programmed anticipation. Expectations are expectations of meaning and order (information) related to the semiosphere the organism constructs as its individual world view and live in. (The Umwelt of von Uexküll). On this basis events that perpetuates the semiosphere are reduced to meaning, i.e. something related to the survival and procreation of the individual living system, it conatus, to use one of Spinoza's terms. The framework of cybersemiotics, uniting second order cybernetics, semiotics and language game theory, is created to make transdisciplinary concepts and models that can handle the process of cognition, information and communication across the domains of the sciences, the arts and social sciences in a non-reductionistic way. It is seen as an alternative based on biological and semiotic thinking (biosemiotics) to the functionalistic information processing paradigm of cognitive science that is build on the computer as paradigm and based on classical logic and mechanistic physics—and therefore has severe problems of dealing with semantics and signification.

Brier, Soren

1998-07-01

27

Exclusion of linkage between hypokalemic periodic paralysis and a candidate region in 1q31-32 suggests genetic heterogeneity  

SciTech Connect

Familial hypokalemic periodic paralysis (HOKPP) is an autosomal dominant disease with attacks of paralysis of varying severity. The attacks occur at intervals of days to years in otherwise healthy people combined with hypokalemia during attacks. The paralysis attacks are precipitated by a number of different factors, like carbohydrate-rich meals, cold, exercise and mental stress. Recently linkage for HOKPP was shown for chromosome 1q31-32 and the disease was mapped between D1S413 and D1S249. The gene for the calcium channel alfa1-subunit (CACNL 1A3) maps to this interval and in two families no recombination was found between a polymorphism in the CACNL 1A3 gene and the disease. This gene is therefore considered to be a candidate for HOKPP. The analysis of a large Danish family excludes linkage to this region and to the CACNL 1A3 gene. In each direction from D1S413, 18.8 cM could be excluded and for D1S249, 14.9 cM. The present study clearly excludes the possibility that the gene causing HOKPP in a large Danish family is located in the region 1q31-32. This result shows that HOKPP is a heterogenous disease, with only one mapped gene so far.

Sillen, A.; Wadelius, C.; Gustabson, K.H. [University Hospital, Uppsala (Sweden)] [and others

1994-09-01

28

Conjugate observations of quasi-periodic emissions by Cluster and DEMETER spacecraft  

NASA Astrophysics Data System (ADS)

Abstract<p label="1">Quasi-<span class="hlt">periodic</span> (QP) emissions are electromagnetic emissions at frequencies of about 0.5-4 kHz that are characterized by a <span class="hlt">periodic</span> time modulation of the wave intensity. Typical <span class="hlt">periods</span> of this modulation are on the order of minutes. We present a case study of a large-scale long-lasting QP event <span class="hlt">observed</span> simultaneously on board the DEMETER (Detection of Electro-Magnetic Emissions Transmitted from Earthquake Regions) and the Cluster spacecraft. The measurements by the Wide-Band Data instrument on board the Cluster spacecraft enabled us to obtain high-resolution frequency-time spectrograms of the event close to the equatorial region over a large range of radial distances, while the measurements by the STAFF-SA instrument allowed us to perform a detailed wave analysis. Conjugate <span class="hlt">observations</span> by the DEMETER spacecraft have been used to estimate the spatial and temporal extent of the emissions. The analyzed QP event lasted as long as 5 h and it spanned over the L-shells from about 1.5 to 5.5. Simultaneous <span class="hlt">observations</span> of the same event by DEMETER and Cluster show that the same QP modulation of the wave intensity is <span class="hlt">observed</span> at the same time at very different locations in the inner magnetosphere. ULF magnetic field fluctuations with a <span class="hlt">period</span> roughly comparable to, but somewhat larger than the <span class="hlt">period</span> of the QP modulation were detected by the fluxgate magnetometers instrument on board the Cluster spacecraft near the equatorial region, <span class="hlt">suggesting</span> these are likely to be related to the QP generation. Results of a detailed wave analysis show that the QP emissions detected by Cluster propagate unducted, with oblique wave normal angles at higher geomagnetic latitudes.</p> <div class="credits"> <p class="dwt_author">N?Mec, F.; SantolíK, O.; Parrot, M.; Pickett, J. S.; Hayosh, M.; Cornilleau-Wehrlin, N.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">29</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/21578297"> <span id="translatedtitle">SPITZER <span class="hlt">OBSERVATIONS</span> OF GX17+2: CONFIRMATION OF A <span class="hlt">PERIODIC</span> SYNCHROTRON SOURCE</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">GX17+2 is a low-mass X-ray binary (LMXB) that is also a member of a small family of LMXBs known as 'Z-sources' that are believed to have persistent X-ray luminosities that are very close to the Eddington limit. GX17+2 is highly variable at both radio and X-ray frequencies, a feature common to Z-sources. What sets GX17+2 apart is its dramatic variability in the near-infrared, where it changes by {Delta}K {approx} 3 mag. Previous investigations have shown that these brightenings are <span class="hlt">periodic</span>, recurring every 3.01 days. Given its high extinction (A{sub V} {>=} 9 mag), it has not been possible to ascertain the nature of these events with ground-based <span class="hlt">observations</span>. We report mid-infrared Spitzer <span class="hlt">observations</span> of GX17+2 which indicate a synchrotron spectrum for the infrared brightenings. In addition, GX17+2 is highly variable in the mid-infrared during these events. The combination of the large-scale outbursts, the presence of a synchrotron spectrum, and the dramatic variability in the mid-infrared <span class="hlt">suggest</span> that the infrared brightening events are due to the <span class="hlt">periodic</span> transit of a synchrotron jet across our line of sight. An analysis of both new, and archival, infrared <span class="hlt">observations</span> has led us to revise the <span class="hlt">period</span> for these events to 3.0367 days. We also present new Rossi X-Ray Timing Explorer (RXTE) data for GX17+2 obtained during two predicted infrared brightening events. Analysis of these new data, and data from the RXTE archive, indicates that there is no correlation between the X-ray behavior of this source and the <span class="hlt">observed</span> infrared brightenings. We examine various scenarios that might produce <span class="hlt">periodic</span> jet emission.</p> <div class="credits"> <p class="dwt_author">Harrison, Thomas E.; McNamara, Bernard J.; Bornak, Jillian [Department of Astronomy, New Mexico State University, Las Cruces, NM 88003-8001 (United States); Gelino, Dawn M. [NASA Exoplanet Science Institute, California Institute of Technology, Pasadena, CA 91125 (United States); Wachter, Stefanie [Spitzer Science Center, Caltech M/S 220-6, Pasadena, CA 91125 (United States); Rupen, Michael P. [National Radio Astronomy Observatory, Socorro, NM 87801 (United States); Gelino, Christopher R., E-mail: tharriso@nmsu.edu, E-mail: bmcnamar@nmsu.edu, E-mail: jbornak@nmsu.edu, E-mail: dawn@ipac.caltech.edu, E-mail: wachter@ipac.caltech.edu, E-mail: mrupen@aoc.nrao.edu, E-mail: cgelino@ipac.caltech.edu [Infrared Processing and Analysis Center, Caltech M/S 220-6, Pasadena, CA 91125 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-07-20</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">30</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/1167617"> <span id="translatedtitle">Evaluation of and <span class="hlt">Suggested</span> Improvements to the WSM6 Microphysics in WRF- ARW Using Synthetic and <span class="hlt">Observed</span> GOES-13 Imagery</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Synthetic satellite imagery can be employed to evaluate simulated cloud fields. Past studies have revealed that the Weather Research and Forecasting (WRF) WRF Single-Moment 6-class (WSM6) microphysics in WRF-ARW produces less upper level ice clouds within synthetic images compared to <span class="hlt">observations</span>. Synthetic Geostationary Operational Environmental Satellite (GOES)-13 imagery at 10.7 ?m of simulated cloud fields from the 4 km National Severe Storms Laboratory (NSSL) WRF-ARW is compared to <span class="hlt">observed</span> GOES-13 imagery. Histograms <span class="hlt">suggest</span> that too few points contain upper level simulated ice clouds. In particular, side-by-side examples are shown of synthetic and <span class="hlt">observed</span> convective anvils. Such images illustrate the lack of anvil cloud associated with convection produced by the NSSL WRF-ARW. A vertical profile of simulated hydrometeors <span class="hlt">suggests</span> that too much cloud water mass may be converted into graupel mass, effectively reducing the main source of ice mass in a simulated anvil. Further, excessive accretion of ice by snow removes ice from an anvil by precipitation settling. Idealized sensitivity tests reveal that a 50% reduction of the conversion of cloud water mass to graupel and a 50% reduction of the accretion rate of ice by snow results in a significant increase in anvil ice of a simulated storm. Such results provide guidance as to which conversions could be reformulated, in a more physical manner, to increase simulated ice mass in the upper troposphere.</p> <div class="credits"> <p class="dwt_author">Grasso, Lewis; Lindsey, Daniel T.; Lim, Kyo-Sun; Clark, Adam; Bikos, Dan; Dembek, Scott R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-10-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">31</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/1998A%26A...332..904D"> <span id="translatedtitle">BeppoSAX <span class="hlt">observations</span> of the long <span class="hlt">period</span> polar system V1309Ori</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We present BeppoSAX <span class="hlt">observations</span> of the peculiar long <span class="hlt">period</span> polar system V1309Ori (RXJ0515.6+0105). The source was detected simultaneously at soft and, for the first time, at hard X-rays with the LECS and the MECS detectors. Both, the LECS and the MECS light curves are irregular with a bursting/flaring type behaviour indicating inhomogeneous accretion onto the white dwarf. This peculiar variability, together with an extreme high soft-to-hard X-ray luminosity ratio, indicates that in V1309Ori accretion occurs predominantly in highly compressed chunks or ``blobs'' of matter. From coordinated ESO optical spectroscopy, we find indications that the magnetic field strength of the white dwarf is < 70MG, not expected either from the 8hr orbital <span class="hlt">period</span> synchronism or from the strong soft-to-hard X-ray ratio <span class="hlt">suggesting</span> alternative solutions for sustaining synchronism in this system. Also based on <span class="hlt">observations</span> collected at the European Southern Observatory, La Silla, Chile</p> <div class="credits"> <p class="dwt_author">de Martino, D.; Barcaroli, R.; Matt, G.; Mouchet, M.; Belloni, T.; Beuermann, K.; Chiappetti, L.; Done, C.; Gänsicke, B. T.; La Franca, F.; Mukai, K.</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">32</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015AnGeo..33..333P"> <span id="translatedtitle">Outflow of low-energy O+ ion beams <span class="hlt">observed</span> during <span class="hlt">periods</span> without substorms</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Numerous <span class="hlt">observations</span> have shown that ions flow out of the ionosphere during substorms with more fluxes leaving as the substorm intensity increases (Wilson et al., 2004). In this article we show <span class="hlt">observations</span> of low-energy (few tens of electron volts) ionospheric ions flowing out <span class="hlt">periods</span> without substorms, determined using the Wideband Imaging Camera (WIC) and Auroral Electrojet (AE) indices. We use Cluster ion composition data and show the outflowing ions are field-aligned H+, He+ and O+ beams accelerated to energies of ~40-80 eV, after correcting for spacecraft potential. The estimated fluxes of the low-energy O+ ions measured at ~20 000 km altitude are >103-105 cm-2 s. Assuming the auroral oval is the source of the escaping ions, the measured fluxes correspond to a flow rate of ~1019-1021 ions s-1 leaving the ionosphere. However, <span class="hlt">periods</span> without substorms can persist for hours <span class="hlt">suggesting</span> the low-energy ions flowing out during these times could be a major source of the heavy ion population in the plasma sheet and lobe.</p> <div class="credits"> <p class="dwt_author">Parks, G. K.; Lee, E.; Fu, S. Y.; Fillingim, M.; Dandouras, I.; Cui, Y. B.; Hong, J.; Rème, H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-03-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">33</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3438871"> <span id="translatedtitle"><span class="hlt">Periodization</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Background: Clinicians are constantly faced with the challenge of designing training programs for injured and noninjured athletes that maximize healing and optimize performance. <span class="hlt">Periodization</span> is a concept of systematic progression—that is, resistance training programs that follow predictable patterns of change in training variables. The strength training literature is abundant with studies comparing <span class="hlt">periodization</span> schemes on uninjured, trained, and untrained athletes. The rehabilitation literature, however, is scarce with information about how to optimally design resistance training programs based on <span class="hlt">periodization</span> principles for injured athletes. The purpose of this review is to discuss relevant training variables and methods of <span class="hlt">periodization</span>, as well as <span class="hlt">periodization</span> program outcomes. A secondary purpose is to provide an anecdotal framework regarding implementation of <span class="hlt">periodization</span> principles into rehabilitation programs. Evidence Acquisition: A Medline search from 1979 to 2009 was implemented with the keywords <span class="hlt">periodization</span>, strength training, rehabilitation, endurance, power, hypertrophy, and resistance training with the Boolean term AND in all possible combinations in the English language. Each author also undertook independent hand searching of article references used in this review. Results: Based on the studies researched, <span class="hlt">periodized</span> strength training regimens demonstrate improved outcomes as compared to nonperiodized programs. Conclusions: Despite the evidence in the strength training literature supporting <span class="hlt">periodization</span> programs, there is a considerable lack of data in the rehabilitation literature about program design and successful implementation of <span class="hlt">periodization</span> into rehabilitation programs. PMID:23015982</p> <div class="credits"> <p class="dwt_author">Lorenz, Daniel S.; Reiman, Michael P.; Walker, John C.</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">34</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://learningcenter.nsta.org/product_detail.aspx?id=10.2505/9780873552394.3"> <span id="translatedtitle"><span class="hlt">Periodicity</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">In thinking about a title for this chapter, the word <span class="hlt">periodicity</span> came to mind. I was sure this had some kind of pop culture reference. After discussing this with my wife, we figured I was thinking of synchronicity, which is a reference to music by the band, The Police. Looking the word <span class="hlt">Periodicity</span> up on the internet, I found that I was, in fact, a science geek and had not made a hip reference. <span class="hlt">Periodicity</span> refers mainly to the <span class="hlt">Periodic</span> Table, which is a focus of this chapter. No music, just science.</p> <div class="credits"> <p class="dwt_author">William C. Robertson, Ph.D.</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">35</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3000892"> <span id="translatedtitle">Validation of a 6-hour <span class="hlt">observation</span> <span class="hlt">period</span> for cocaine body stuffers</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Often, patients are brought in to the emergency room after ingesting large amounts of cocaine in an attempt to conceal it. This act is known as “body stuffing.” The <span class="hlt">observation</span> <span class="hlt">period</span> required to recognize potential toxic side effects in these patients is not well described in the literature. We sought to validate a treatment algorithm for asymptomatic cocaine body stuffers utilizing a 6-hour <span class="hlt">observation</span> <span class="hlt">period</span> by <span class="hlt">observing</span> the clinical course of cocaine body stuffers over a 24-hour <span class="hlt">period</span>. A retrospective chart review was performed on all patients evaluated for witnessed or suspected stuffing over two years utilizing a standardized protocol. 106 patients met final inclusion criteria as adult cocaine stuffers. No patients developed life-threatening symptoms and no patients died during <span class="hlt">observation</span>. In our medical setting, stuffers could be discharged after a 6- hour <span class="hlt">observation</span> <span class="hlt">period</span> if there was either complete resolution or absence of clinical symptoms. PMID:20825819</p> <div class="credits"> <p class="dwt_author">Moreira, Maria; Buchanan, Jennie; Heard, Kennon</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">36</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/19229771"> <span id="translatedtitle">Experimental <span class="hlt">Observation</span> of a <span class="hlt">Periodically</span> Oscillating Plasma Sphere in a Gridded Inertial Electrostatic Confinement Device</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The <span class="hlt">periodically</span> oscillating plasma sphere (POPS) [D. C. Barnes and R. A. Nebel, Phys. Plasmas 5, 2498 (1998).] oscillation has been <span class="hlt">observed</span> in a gridded inertial electrostatic confinement device. In these experiments, ions in the virtual cathode exhibit resonant behavior when driven at the POPS frequency. Excellent agreement between the <span class="hlt">observed</span> POPS resonance frequency and theoretical predictions has been <span class="hlt">observed</span></p> <div class="credits"> <p class="dwt_author">R. A. Nebel; S. Stange; S. Krupakar Murali</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">37</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/52788850"> <span id="translatedtitle">VRc <span class="hlt">observations</span> of LMC long-<span class="hlt">period</span> red variables (Noda+, 2002)</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">146 long-<span class="hlt">period</span> red variable stars in the Large Magellanic Cloud (LMC) from the three-year Microlensing <span class="hlt">Observations</span> in Astrophysics (MOA) project data base were analysed. A careful <span class="hlt">periodic</span> analysis was performed on these stars and a catalogue of their magnitudes, colours, <span class="hlt">periods</span> and amplitudes is presented. We convert our blue and red magnitudes to K-band values using 19 oxygen-rich stars. A</p> <div class="credits"> <p class="dwt_author">S. Noda; M. Takeuti; F. Abe; I. A. Bond; R. J. Dodd; J. B. Hearnshaw; M. Honda; M. Honma; J. Jugaku; S. Kabe; Y. Kan-Ya; Y. Kato; P. M. Kilmartin; Y. Matsubara; K. Masuda; Y. Muraki; T. Nakamura; G. R. Nankivell; C. Noguchi; K. Ohnishi; M. Reid; N. J. Rattenbury; T. Saito; H. Sato; M. Sekiguchi; J. Skuljan; D. J. Sullivan; T. Sumi; Y. Watase; S. Wilkinson; R. Yamada; T. Yanagisawa; P. C. M. Yock; M. Yoshizawa</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">38</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.cru.uea.ac.uk/cru/pubs/crurp/CRU_RP6a.pdf"> <span id="translatedtitle">Weather <span class="hlt">Observations</span> and a Tentative Meteorological Analysis of the <span class="hlt">Period</span> May</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">Weather <span class="hlt">Observations</span> and a Tentative Meteorological Analysis of the <span class="hlt">Period</span> May to July 1588 K. CRU RP6 (1978) Douglas KS, Lamb HH & Loader C A meteorological study of July to October 1588 Meteorological Analysis of the <span class="hlt">Period</span> May to July 1588. CRU RP7 (1980) Perry AH & Fearnside T Northern Hemisphere</p> <div class="credits"> <p class="dwt_author">Feigon, Brooke</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">39</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/18522171"> <span id="translatedtitle"><span class="hlt">Observation</span> and removal of daily quasi-<span class="hlt">periodic</span> components in soil radon data</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">We report (quasi) <span class="hlt">periodic</span> oscillations <span class="hlt">observed</span> in soil radon emanation data especially during summer <span class="hlt">period</span>. Soil radon has been continuously monitored in the Marmara region of Turkey over the past nine years to reveal possible relationships between soil radon and seismic activities. This long term monitoring has clearly demonstrated that soil radon concentrations are affected by various parameters such as</p> <div class="credits"> <p class="dwt_author">S. Baykut; T. Akgül; S. ?nan; C. Seyis</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">40</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19860013037&hterms=eric+pino&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Deric%2Bpino"> <span id="translatedtitle">Archive of <span class="hlt">observations</span> of <span class="hlt">periodic</span> comet Crommelin made during its 1983-84 apparition</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">This is an archive of 680 reduced <span class="hlt">observations</span> of <span class="hlt">Periodic</span> Comet Crommelin made during its 1984 apparition. The archive integrates reports by members of the eight networks of the International Halley Watch (IHW) and presents the results of a trial run designed to test the preparedness of the IHW organization for the current apparition of <span class="hlt">Periodic</span> Comet Halley.</p> <div class="credits"> <p class="dwt_author">Sekanina, Z. (editor); Aronsson, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">1985-01-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_1");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a style="font-weight: bold;">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' 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Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">41</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://users.camk.edu.pl/alex/papers/multih.pdf"> <span id="translatedtitle">FAST AND STATISTICALLY OPTIMAL <span class="hlt">PERIOD</span> SEARCH IN UNEVEN SAMPLED <span class="hlt">OBSERVATIONS</span> A. SCHWARZENBERG-CZERNY</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">) based power spectrum in <span class="hlt">period</span> analysis stems from its simplicity, clear interpretation for the nonsinusoidal signals. Second, it is less well known that in practical applications neither power spectrum norFAST AND STATISTICALLY OPTIMAL <span class="hlt">PERIOD</span> SEARCH IN UNEVEN SAMPLED <span class="hlt">OBSERVATIONS</span> A. SCHWARZENBERG</p> <div class="credits"> <p class="dwt_author">Schwarzenberg-Czerny, Alex</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">42</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://pubs.er.usgs.gov/publication/70026155"> <span id="translatedtitle"><span class="hlt">Observations</span> of deep long-<span class="hlt">period</span> (DLP) seismic events beneath Aleutian arc volcanoes; 1989-2002</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p class="result-summary">Between October 12, 1989 and December 31, 2002, the Alaska Volcano Observatory (AVO) located 162 deep long-<span class="hlt">period</span> (DLP) events beneath 11 volcanic centers in the Aleutian arc. These events generally occur at mid- to lower-crustal depths (10-45 km) and are characterized by emergent phases, extended codas, and a strong spectral peak between 1.0 and 3.0 Hz. <span class="hlt">Observed</span> wave velocities and particle motions indicate that the dominant phases are P- and S-waves. DLP epicenters often extend over broad areas (5-20 km) surrounding the active volcanoes. The average reduced displacement of Aleutian DLPs is 26.5 cm2 and the largest event has a reduced displacement of 589 cm2 (or ML 2.5). Aleutian DLP events occur both as solitary events and as sequences of events with several occurring over a <span class="hlt">period</span> of 1-30 min. Within the sequences, individual DLPs are often separated by lower-amplitude volcanic tremor with a similar spectral character. Occasionally, volcano-tectonic earthquakes that locate at similar depths are contained within the DLP sequences. At most, Aleutian volcanoes DLPs appear to loosely surround the main volcanic vent and occur as part of background seismicity. A likely explanation is that they reflect a relatively steady-state process of magma ascent over broad areas in the lower and middle portions of the crust. At Mount Spurr, DLP seismicity was initiated by the 1992 eruptions and then slowly declined until 1997. At Shishaldin Volcano, a short-lived increase in DLP seismicity occurred about 10 months prior to the April 19, 1999 eruption. These <span class="hlt">observations</span> <span class="hlt">suggest</span> a link between eruptive activity and magma flux in the mid- to lower-crust and uppermost mantle.</p> <div class="credits"> <p class="dwt_author">Power, J.A.; Stihler, S.D.; White, R.A.; Moran, S.C.</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">43</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://cds.cern.ch/record/539470/files/0202441.pdf"> <span id="translatedtitle">Dwarf Nova Oscillations and Quasi-<span class="hlt">Periodic</span> Oscillations in Cataclysmic Variables I. <span class="hlt">Observations</span> of VW Hyi</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">From archived and recent high speed photometry of VW Hyi we find Dwarf Nova Oscillations (DNOs) occasionally present throughout outburst, evolving from 14.06 s <span class="hlt">period</span> at maximum to > 40 s near the end of outburst. A relatively slow increase of <span class="hlt">period</span> is followed by rapid increase and subsequent decrease. Quasi-<span class="hlt">periodic</span> Oscillations (QPOs) are seen at <span class="hlt">periods</span> of hundreds of seconds. For the first time, an evolution of QPO <span class="hlt">period</span> is seen, steadily increasing during the final decline of an outburst. The occasional presence of two DNOs, separated in frequency by the QPO frequency, <span class="hlt">suggests</span> reprocessing of the rotating DNO beam by a `wall' rotating progradely in the disc at the QPO <span class="hlt">period</span>.</p> <div class="credits"> <p class="dwt_author">Woudt, P A; Woudt, Patrick A.; Warner, Brian</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">44</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://dspace.mit.edu/handle/1721.1/32909"> <span id="translatedtitle">X-ray <span class="hlt">periodicities</span> in sources <span class="hlt">observed</span> by the RXTE ASM</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">The X-ray intensities measured from 230 X-ray sources <span class="hlt">observed</span> by the RXTE All-Sky Monitor (ASM) were analyzed for <span class="hlt">periodic</span> behavior. The ASM has been <span class="hlt">observing</span> sources for nine years in the 1.5-12 keV energy range. In ...</p> <div class="credits"> <p class="dwt_author">Shivamoggi, Vasudha B</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">45</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19960021447&hterms=szabo&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3Dszabo"> <span id="translatedtitle">Solar wind plasma <span class="hlt">periodicities</span> <span class="hlt">observed</span> at 1 AU by IMP 8</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The IMP 8 spacecraft has been in Earth orbit since 1973, gathering plasma data over one complete 22-year solar cycle. These data are being examined to look for <span class="hlt">periodicities</span> at time scales ranging from several hours to the entire span of the data set. A 1.3-year <span class="hlt">periodicity</span> in the radial speed <span class="hlt">observed</span> by IMP 8 and Voyager 2 has already been reported for the years from 1987 to 1993. The periodogram method, useful for unevenly sampled data such as the IMP 8 plasma data, has been used to search for other <span class="hlt">periods</span>. It is interesting to note that the 13-year <span class="hlt">period</span> is not present in the out-of-the-ecliptic component of the velocity (Vz), although a 1-year <span class="hlt">period</span> is very obvious both visually and on the periodogram. Both components show a very strong peak associated with the 11-year solar cycle variation. This work will be extended to the thermal speed (a measure of the wind's temperature) and density, although the frequent correlations between these parameters and the velocity are expected to cause similar results. Additionally, the fine resolution data will be examined for shorter time <span class="hlt">periods</span> than are visible using the hourly average data which are appropriate for longer <span class="hlt">periods</span>. A comparison with <span class="hlt">periods</span> <span class="hlt">observed</span> at other spacecraft may also be made.</p> <div class="credits"> <p class="dwt_author">Paularena, K. I.; Szabo, A.; Lazarus, A. J.</p> <p class="dwt_publisher"></p> <p class="publishDate">1995-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">46</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/52229583"> <span id="translatedtitle">Latitudinal variation of perturbation electric fields during magnetically disturbed <span class="hlt">periods</span> - 1986 Sundial <span class="hlt">observations</span> and model results</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">F-region incoherent scatter radar drift <span class="hlt">observations</span> from Millstone Hill and Jicamarca, h-prime F <span class="hlt">observations</span> from Huancayo, and high latitude ground-magnetometer measurements taken during the Sundial 1986 campaign are used to study the relationship between plasmaspheric electric field perturbations and high latitude currents during disturbed <span class="hlt">periods</span>. The <span class="hlt">observations</span> are in good agreement with numerical results from a Rice Covection Model run</p> <div class="credits"> <p class="dwt_author">B. G. Fejer; R. W. Spiro; R. A. Wolf; J. C. Foster</p> <p class="dwt_publisher"></p> <p class="publishDate">1990-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">47</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/19436246"> <span id="translatedtitle"><span class="hlt">Observation</span> of spin-wave envelope solitons in <span class="hlt">periodic</span> magnetic film structures</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The formation and propagation of light and dark microwave spin-wave envelope solitons in a <span class="hlt">periodic</span> magnetic film structure\\u000a have been <span class="hlt">observed</span>. The <span class="hlt">periodic</span> structure was manufactured on the basis of the single-crystal film of iron-yttrium garnet\\u000a and a lattice of copper strips placed on the surface of the film perpendicularly to the propagation direction of carrying\\u000a spin waves. The solitons</p> <div class="credits"> <p class="dwt_author">A. B. Ustinov; N. Yu. Grigor’eva; B. A. Kalinikos</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">48</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014SoPh..289.1983E"> <span id="translatedtitle">Long-<span class="hlt">Period</span> Oscillations of Sunspots <span class="hlt">Observed</span> by SOHO/MDI</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We processed magnetograms that were obtained with the Michaelson Doppler Imager onboard the Solar and Heliospheric Observatory (SOHO/MDI). The results confirm the basic properties of long-<span class="hlt">period</span> oscillations of sunspots that have previously been established and also reveal new properties. We show that the limiting (lowest) eigenmode of low-frequency oscillations of a sunspot as a whole is the mode with a <span class="hlt">period</span> of 10 - 12 up to 32 - 35 hours (depending on the sunspot's magnetic-field strength). This mode is <span class="hlt">observed</span> consistently throughout an <span class="hlt">observation</span> <span class="hlt">period</span> of 5 - 7 days, but its amplitude is subject to quasi-cyclic changes, which are separated by about 1.5 - 2 days. As a result, the lower mode with a <span class="hlt">period</span> of about 35 - 48 hours appears in the power spectrum of sunspot oscillations. But this lowest mode is apparently not an eigenmode of a sunspot because its <span class="hlt">period</span> does not depend on the magnetic field of the sunspot. Perhaps the mode reflects the quasi-<span class="hlt">periodic</span> sunspot perturbations caused by supergranulation cells that surround it. We also analyzed SOHO/MDI artifacts, which may affect the low-frequency power spectra of sunspots.</p> <div class="credits"> <p class="dwt_author">Efremov, V. I.; Parfinenko, L. D.; Solov'ev, A. A.; Kirichek, E. A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">49</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/45898161"> <span id="translatedtitle"><span class="hlt">Observational</span> evidence of coupling between quasi-<span class="hlt">periodic</span> echoes and medium scale traveling ionospheric disturbances</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">We have found that quasi-<span class="hlt">periodic</span> (QP) echoes in the E region were well defined when medium scale traveling ionospheric disturbances (MSTIDs) in the F region were present. The appearance and disappearance of the MSTIDs <span class="hlt">observed</span> with the dense GPS receiver network are well correlated with the development and decay of QP echoes <span class="hlt">observed</span> with the Middle-and-Upper atmosphere (MU) radar. Interferometric</p> <div class="credits"> <p class="dwt_author">S. Saito; M. Yamamoto; H. Hashiguchi; A. Maegawa; A. Saito</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">50</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/52200273"> <span id="translatedtitle">Experimental <span class="hlt">Observation</span> of a <span class="hlt">Periodically</span> Oscillating Plasma Sphere in a Gridded Inertial Electrostatic Confinement Device</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The <span class="hlt">periodically</span> oscillating plasma sphere (POPS) [D. C. Barnes and R. A. Nebel, Phys. Plasmas 5, 2498 (1998)., PHPAEN, 1070-664X, 10.1063\\/1.872933] oscillation has been <span class="hlt">observed</span> in a gridded inertial electrostatic confinement device. In these experiments, ions in the virtual cathode exhibit resonant behavior when driven at the POPS frequency. Excellent agreement between the <span class="hlt">observed</span> POPS resonance frequency and theoretical predictions</p> <div class="credits"> <p class="dwt_author">R. A. Nebel; S. Stange; S. Krupakar Murali</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">51</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/1501.05043.pdf"> <span id="translatedtitle">Ultrashort-<span class="hlt">period</span> MS eclipsing systems. New <span class="hlt">observations</span> and light curve solutions of six NSVS binaries</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We carried out photometric and low-resolution spectral <span class="hlt">observations</span> of six eclipsing ultrashort-<span class="hlt">period</span> binaries with MS components. The light curve solutions of the Rozhen <span class="hlt">observations</span> show that all targets are overcontact systems. We found well-defined empirical relation "<span class="hlt">period</span> -- semi-major axis" for the short-<span class="hlt">period</span> binaries and used it for estimation of the global parameters of the targets. Our results revealed that NSVS 925605 is quite interesting target: (a) it is one of a few contact binaries with M components; (b) it exhibits high activity (emission in H$\\alpha$ line, X-ray emission, large cool spots, non-Planck energy distribution); (c) its components differ in temperature by 700 K. All appearances of high magnetic activity and huge fillout factor (0.7) of NSVS 925605 might be assumed as a precursor of the predicted merging of close magnetic binaries. Another unusual binary is NSVS 2700153 which reveals considerable long-term variability.</p> <div class="credits"> <p class="dwt_author">Dimitrov, Dinko</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">52</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://sprg.ssl.berkeley.edu/adminstuff/webpubs/2003_jgr_1411.pdf"> <span id="translatedtitle"><span class="hlt">Periodic</span> magnetospheric substorms: Multiple space-based and ground-based instrumental <span class="hlt">observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary"><span class="hlt">Periodic</span> magnetospheric substorms: Multiple space-based and ground-based instrumental <span class="hlt">observations</span> represent particle injections from the tail to the inner magnetosphere, whether the sawtooth variations-based and ground-based instruments in the magnetosphere and ionosphere during two magnetic storms. The Geotail</p> <div class="credits"> <p class="dwt_author">California at Berkeley, University of</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">53</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012EGUGA..14.4375S"> <span id="translatedtitle"><span class="hlt">Observed</span> temporal evolution of global mean age of stratospheric air for the 2002 to 2010 <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">An extensive <span class="hlt">observational</span> data set from MIPAS measurements, consisting of more than one million SF6 vertical profiles distributed globally has been condensed into monthly zonal means of mean age of air for the <span class="hlt">period</span> September 2002 to January 2010, binned at 10° latitude and 1-2 km altitude. The data were analysed with respect to their temporal variation by fitting a regression model consisting of: a constant and a linear increase term, 2 proxies for the QBO variation, sinusoidal terms for the seasonal and semi-annual variation and overtones for the correction of the shapes to the <span class="hlt">observed</span> data set. The impact of subsidence of mesospheric SF6-depleted air and in-mixing into non-polar latitudes on mid-latitudinal age of air and its linear increase was assessed and found to be small. The linear increase of mean age of stratospheric air was found to be positive and partly larger than the trend derived by Engel et al. (2009) for most of the Northern mid-latitudes, the middle stratosphere in the tropics, and parts of the Southern mid-latitudes, as well as for the Southern polar upper stratosphere. Multi-year decrease of age of air was found for the lowermost and the upper stratospheric tropics, for parts of Southern mid-latitudes, and for the Northern polar regions. Analyses of the amplitudes and phases of the seasonal variation shed light on the coupling between different stratospheric regions. In particular, the Northern mid-latitude stratosphere is well coupled to the tropics, while the Northern lowermost mid-latitudinal stratosphere is decoupled, confirming the separation of the shallow branch of the Brewer-Dobson circulation from the deep branch. We <span class="hlt">suggest</span> an overall increased tropical upwelling, together with a weakening of mixing barriers, especially in the Northern hemisphere, as possible explanations for the <span class="hlt">observed</span> patterns. Reference: Engel, A., Möbius, T., Bönisch, H., Schmidt, U., Heinz, R., Levin, I., Atlas, E., Aoki, S., Nakazawa, T., Sugawara, S., Moore, F., Hurst, D., Elkins, J., Schauffler, S., Andrews, A., and Boering, K.: Age of stratospheric air unchanged within uncertainties over the past 30 years, Nature Geosci., 2, 28-31, doi:10.1038/ngeo388, 2009.</p> <div class="credits"> <p class="dwt_author">Stiller, G. P.; von Clarmann, T.; Haenel, F.; Funke, B.; Glatthor, N.; Grabowski, U.; Kellmann, S.; Kiefer, M.; Linden, A.; Lossow, S.; López-Puertas, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">54</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/20696429"> <span id="translatedtitle">Experimental <span class="hlt">Observation</span> of a <span class="hlt">Periodically</span> Oscillating Plasma Sphere in a Gridded Inertial Electrostatic Confinement Device</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The <span class="hlt">periodically</span> oscillating plasma sphere (POPS) [D. C. Barnes and R. A. Nebel, Phys. Plasmas 5, 2498 (1998).] oscillation has been <span class="hlt">observed</span> in a gridded inertial electrostatic confinement device. In these experiments, ions in the virtual cathode exhibit resonant behavior when driven at the POPS frequency. Excellent agreement between the <span class="hlt">observed</span> POPS resonance frequency and theoretical predictions has been <span class="hlt">observed</span> for a wide range of potential well depths and for three different ion species. The results provide the first experimental validation of the POPS concept proposed by Barnes and Nebel [R. A. Nebel and D. C. Barnes, Fusion Technol. 34, 28 (1998).].</p> <div class="credits"> <p class="dwt_author">Park, J.; Nebel, R.A.; Stange, S.; Murali, S. Krupakar [Los Alamos National Laboratory, Los Alamos, New Mexico 87544 (United States); University of Wisconsin, Madison, Wisconsin 53706 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-07-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">55</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/16090625"> <span id="translatedtitle">Experimental <span class="hlt">observation</span> of a <span class="hlt">periodically</span> oscillating plasma sphere in a gridded inertial electrostatic confinement device.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The <span class="hlt">periodically</span> oscillating plasma sphere (POPS) [D. C. Barnes and R. A. Nebel, Phys. Plasmas 5, 2498 (1998).] oscillation has been <span class="hlt">observed</span> in a gridded inertial electrostatic confinement device. In these experiments, ions in the virtual cathode exhibit resonant behavior when driven at the POPS frequency. Excellent agreement between the <span class="hlt">observed</span> POPS resonance frequency and theoretical predictions has been <span class="hlt">observed</span> for a wide range of potential well depths and for three different ion species. The results provide the first experimental validation of the POPS concept proposed by Barnes and Nebel [R. A. Nebel and D. C. Barnes, Fusion Technol. 34, 28 (1998).]. PMID:16090625</p> <div class="credits"> <p class="dwt_author">Park, J; Nebel, R A; Stange, S; Murali, S Krupakar</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">56</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22086236"> <span id="translatedtitle">EVOLUTIONARY TRACKS OF TRAPPED, ACCRETING PROTOPLANETS: THE ORIGIN OF THE <span class="hlt">OBSERVED</span> MASS-<span class="hlt">PERIOD</span> RELATION</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The large number of <span class="hlt">observed</span> exoplanets ({approx}>700) provides important constraints on their origin as deduced from the mass-<span class="hlt">period</span> diagram of planets. The most surprising features in the diagram are (1) the (apparent) pileup of gas giants at a <span class="hlt">period</span> of {approx}500 days ({approx}1 AU) and (2) the so-called mass-<span class="hlt">period</span> relation, which indicates that planetary mass is an increasing function of orbital <span class="hlt">period</span>. We construct the evolutionary tracks of growing planets at planet traps in evolving protoplanetary disks and show that they provide a good physical understanding of how these <span class="hlt">observational</span> properties arise. The fundamental feature of our model is that inhomogeneities in protoplanetary disks give rise to multiple (up to 3) trapping sites for rapid (type I) planetary migration of planetary cores. The viscous evolution of disks results in the slow radial movement of the traps and their cores from large to small orbital <span class="hlt">periods</span>. In our model, the slow inward motion of planet traps is coupled with the standard core accretion scenario for planetary growth. As planets grow, type II migration takes over. Planet growth and radial movement are ultimately stalled by the dispersal of gas disks via photoevaporation. Our model makes a number of important predictions: that distinct sub-populations of planets that reflect the properties of planet traps where they have grown result in the mass-<span class="hlt">period</span> relation, that the presence of these sub-populations naturally explains a pileup of planets at {approx}1 AU, and that evolutionary tracks from the ice line do put planets at short <span class="hlt">periods</span> and fill an earlier claimed {sup p}lanet desert{sup -}a sparse population of planets in the mass-semimajor axis diagram.</p> <div class="credits"> <p class="dwt_author">Hasegawa, Yasuhiro [Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1 (Canada); Pudritz, Ralph E., E-mail: hasegay@physics.mcmaster.ca, E-mail: pudritz@physics.mcmaster.ca [Origins Institute, McMaster University, Hamilton, ON L8S 4M1 (Canada)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">57</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/1502.00397v1"> <span id="translatedtitle">Revolution of S-stars and oscillation of solar and terrestrial <span class="hlt">observables</span>: nonrandom coincidence of <span class="hlt">periods</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">A striking coincidence of revolution <span class="hlt">periods</span> of S-stars orbiting a supermassive black hole at the Galactic Center of the Milky Way and oscillation <span class="hlt">periods</span> of such solar and terrestrial <span class="hlt">observables</span> as the sunspot number, the geomagnetic field Y-component and the global temperature is established on basis of the corresponding experimental data. Rejecting randomness of this discovered coincidence, we put forward a hypothesis that modulation of dark matter flows in the Milky Way by the S-stars is responsible for such a frequency transfer from the Galactic Center to the Solar System.</p> <div class="credits"> <p class="dwt_author">V. D. Rusov; V. P. Smolyar; M. V. Eingorn</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-02-02</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">58</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/1502.00397.pdf"> <span id="translatedtitle">Revolution of S-stars and oscillation of solar and terrestrial <span class="hlt">observables</span>: nonrandom coincidence of <span class="hlt">periods</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">A striking coincidence of revolution <span class="hlt">periods</span> of S-stars orbiting a supermassive black hole at the Galactic Center of the Milky Way and oscillation <span class="hlt">periods</span> of such solar and terrestrial <span class="hlt">observables</span> as the sunspot number, the geomagnetic field Y-component and the global temperature is established on basis of the corresponding experimental data. Rejecting randomness of this discovered coincidence, we put forward a hypothesis that modulation of dark matter flows in the Milky Way by the S-stars is responsible for such a frequency transfer from the Galactic Center to the Solar System.</p> <div class="credits"> <p class="dwt_author">Rusov, V D; Eingorn, M V</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">59</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014HESS...18.1953F"> <span id="translatedtitle">Overview of the first HyMeX Special <span class="hlt">Observation</span> <span class="hlt">Period</span> over Italy: <span class="hlt">observations</span> and model results</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The Special <span class="hlt">Observation</span> <span class="hlt">Period</span> (SOP1), part of the HyMeX campaign (Hydrological cycle in the Mediterranean Experiments, 5 September-6 November 2012), was dedicated to heavy precipitation events and flash floods in the western Mediterranean, and three Italian hydro-meteorological monitoring sites were identified: Liguria-Tuscany, northeastern Italy and central Italy. The extraordinary deployment of advanced instrumentation, including instrumented aircrafts, and the use of several different operational weather forecast models, including hydrological models and marine models, allowed an unprecedented monitoring and analysis of high-impact weather events around the Italian hydro-meteorological sites. This activity has seen strong collaboration between the Italian scientific and operational communities. In this paper an overview of the Italian organization during SOP1 is provided, and selected Intensive <span class="hlt">Observation</span> <span class="hlt">Periods</span> (IOPs) are described. A significant event for each Italian target area is chosen for this analysis: IOP2 (12-13 September 2012) in northeastern Italy, IOP13 (15-16 October 2012) in central Italy and IOP19 (3-5 November 2012) in Liguria and Tuscany. For each IOP the meteorological characteristics, together with special <span class="hlt">observations</span> and weather forecasts, are analyzed with the aim of highlighting strengths and weaknesses of the forecast modeling systems, including the hydrological impacts. The usefulness of having different weather forecast operational chains characterized by different numerical weather prediction models and/or different model set up or initial conditions is finally shown for one of the events (IOP19).</p> <div class="credits"> <p class="dwt_author">Ferretti, R.; Pichelli, E.; Gentile, S.; Maiello, I.; Cimini, D.; Davolio, S.; Miglietta, M. M.; Panegrossi, G.; Baldini, L.; Pasi, F.; Marzano, F. S.; Zinzi, A.; Mariani, S.; Casaioli, M.; Bartolini, G.; Loglisci, N.; Montani, A.; Marsigli, C.; Manzato, A.; Pucillo, A.; Ferrario, M. E.; Colaiuda, V.; Rotunno, R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-05-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">60</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2008APS..MARV40014D"> <span id="translatedtitle"><span class="hlt">Observations</span> of simple RNA suboptimal structures including pseudoknots <span class="hlt">suggests</span> that the folding landscape is often funnel shaped</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Many RNA structure are known to fold up into complex function structures such as ribosomal RNA, transfer RNA (tRNA), riboswitches, etc. We are currently developing a novel theoretical approach for predicting the base pairing topology of folded RNA structures [1,2], a term known as RNA secondary structure. A good prediction of this base pairing can significantly speed up computation of the full 3D structure of these complex molecules. In recent work, we reported a pseudoknot prediction application using this model [3]. We have now upgraded this application to also predict suboptimal structures. The results of this model <span class="hlt">suggest</span> that structures like tRNA often have a folding landscape of suboptimal structures that is essentially funnel shaped; similar to what is known to be the case for many simple proteins. This model has also been applied to simple protein structure topology prediction in a similar fashion. [1] Dawson, et al. (2001). J Theor Biol. 213, 359-386 and 387-412. [2] Dawson, et al. (2006). Nucleosides, Nucleotides, and Nucleic Acids 25, 171-189. [3]Dawson, et al. (2007). PLoS One, 2, 905.</p> <div class="credits"> <p class="dwt_author">Dawson, Wayne; Kawai, Gota</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-03-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_2");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a 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onClick='return showDiv("page_11");' href="#">11</a> <a onClick='return showDiv("page_12");' href="#">12</a> <a onClick='return showDiv("page_13");' href="#">13</a> <a onClick='return showDiv("page_14");' href="#">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a onClick='return showDiv("page_16");' href="#">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a onClick='return showDiv("page_21");' href="#">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_5");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">61</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/astro-ph/0605421v1"> <span id="translatedtitle">Optimal placement of a limited number of <span class="hlt">observations</span> for <span class="hlt">period</span> searches</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">Robotic telescopes present the opportunity for the sparse temporal placement of <span class="hlt">observations</span> when <span class="hlt">period</span> searching. We address the best way to place a limited number of <span class="hlt">observations</span> to cover the dynamic range of frequencies required by an <span class="hlt">observer</span>. We show that an <span class="hlt">observation</span> distribution geometrically spaced in time can minimise aliasing effects arising from sparse sampling, substantially improving signal detection quality. The base of the geometric series is however a critical factor in the overall success of this strategy. Further, we show that for such an optimal distribution <span class="hlt">observations</span> may be reordered, as long as the distribution of spacings is preserved, with almost no loss of quality. This implies that optimal <span class="hlt">observing</span> strategies can retain significant flexibility in the face of scheduling constraints, by providing scope for on-the-fly adaptation. Finally, we present optimal geometric samplings for a wide range of common <span class="hlt">observing</span> scenarios, with an emphasis on practical application by the <span class="hlt">observer</span> at the telescope. Such a sampling represents the best practical empirical solution to the undersampling problem that we are aware of. The technique has applications to robotic telescope and satellite <span class="hlt">observing</span> strategies, where target acquisition overheads mean that a greater total target exposure time (and hence signal-to-noise) can often in practice be achieved by limiting the number of <span class="hlt">observations</span>.</p> <div class="credits"> <p class="dwt_author">Eric S. Saunders; Tim Naylor; Alasdair Allan</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-05-17</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">62</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014AAS...22315412G"> <span id="translatedtitle">Optical <span class="hlt">Observations</span> of the Cataclysmic Variable FL Ceti, Evidence for a Decrease in Orbital <span class="hlt">Period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">FL Ceti is a short <span class="hlt">period</span> cataclysmic variable star belonging to the highly magnetic subclass of polars. Our one second time resolution light curves show dramatic eclipses, as well as a well defined ingress and egress features. We collected 35 hours of broad band optical photometry on FL Ceti at the 82" reflector in the McDonald Observatory. We <span class="hlt">observed</span> 23 eclipses of the system in 2011. Combining timings of these eclipses with previously publish data we obtain preliminary evidence which indicate that the orbital <span class="hlt">period</span> of the system is decreasing. We discuss the implications for the derived <span class="hlt">period</span> derivative and mass transfer rate. This research is supported in part by NSF grant 0958783.</p> <div class="credits"> <p class="dwt_author">Gomez, Sebastian; Mason, P. A.; Robinson, E. L.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">63</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24319226"> <span id="translatedtitle">Key clinical <span class="hlt">observations</span> after 5-azacytidine and decitabine treatment of myelodysplastic syndromes <span class="hlt">suggest</span> practical solutions for better outcomes.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Clinical experience with 5-azacytidine and decitabine treatment of myelodysplastic syndromes (MDS), complemented by biological and pharmacological studies, has revealed compelling mechanism of action differences compared with traditional myeloid cancer treatment mainstays such as cytarabine. For example, 5-azacytidine and decitabine produce remissions and better overall survival in MDS with high-risk chromosome abnormalities at a surprisingly high rate, consistent with experimental <span class="hlt">observations</span> that noncytotoxic DNA methyltransferase depletion by 5-azacytidine/decitabine can trigger cell cycle exit independently of p53, thus circumventing a basis for resistance to apoptosis-based DNA-damaging therapy. That responses cut across the chaotic genomic landscape of MDS highlights common threads in disease, such as high expression in myeloblasts of differentiation-driving transcription factors yet paradoxical epigenetic suppression of proliferation-terminating late-differentiation genes. Less toxic regimens (lower dosages but more frequent administration) of 5-azacytidine/decitabine have been more successful, underscoring the importance of preserving functionally normal stem cells, which are rendered more precious by attrition from age, previous cytotoxic treatments, and the disease process and are needed to relieve cytopenias, the cause of morbidity and mortality. Also emphasized is that there can be no therapeutic benefit, regardless of mutation or cytogenetic subtype, if DNA methyltransferase is not depleted by sufficient overlap between intracellular drug half-lives and S-phase entries of malignant cells. Improved understanding of mechanism-of-action differences demands new approaches, from historic (but not scientific) more-is-better and one-size-fits-all empiricism to pharmacodynamic-based designs and combinations directed not solely at suppressing malignant clones, but at improving therapeutic indices. PMID:24319226</p> <div class="credits"> <p class="dwt_author">Saunthararajah, Yogen</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">64</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20140010418&hterms=Cummings&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3DCummings"> <span id="translatedtitle">Elemental GCR <span class="hlt">Observations</span> during the 2009-2010 Solar Minimum <span class="hlt">Period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Using <span class="hlt">observations</span> from the Cosmic Ray Isotope Spectrometer (CRIS) onboard the Advanced Composition Explorer (ACE), we present new measurements of the galactic cosmic ray (GCR) elemental composition and energy spectra for the species B through Ni in the energy range approx. 50-550 MeV/nucleon during the record setting 2009-2010 solar minimum <span class="hlt">period</span>. These data are compared with our <span class="hlt">observations</span> from the 1997-1998 solar minimum <span class="hlt">period</span>, when solar modulation in the heliosphere was somewhat higher. For these species, we find that the intensities during the 2009-2010 solar minimum were approx. 20% higher than those in the previous solar minimum, and in fact were the highest GCR intensities recorded during the space age. Relative abundances for these species during the two solar minimum <span class="hlt">periods</span> differed by small but statistically significant amounts, which are attributed to the combination of spectral shape differences between primary and secondary GCRs in the interstellar medium and differences between the levels of solar modulation in the two solar minima. We also present the secondary-to-primary ratios B/C and (Sc+Ti+V)/Fe for both solar minimum <span class="hlt">periods</span>, and demonstrate that these ratios are reasonably well fit by a simple "leaky-box" galactic transport model that is combined with a spherically symmetric solar modulation model.</p> <div class="credits"> <p class="dwt_author">Lave, K. A.; Israel, M. H.; Binns, W. R.; Christian, E. R.; Cummings, A. C.; Davis, A. J.; deNolfo, G. A.; Leske, R. A.; Mewaldt, R. A.; Stone, E. C.; vonRosenvinge, T. T.; Wiedenbeck, M. E.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">65</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2005APS..MAR.K1104Y"> <span id="translatedtitle"><span class="hlt">Period</span> doubling <span class="hlt">observed</span> in the circadian photosynthetic rhythm of the prokaryotic cyanobacterium Cyanothece RF-1</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The circadian rhythm is an endogenous biological clock that governs biochemical phenomena or behavior in organisms. The Cyanothece RF-1 is the first prokaryote shown to exhibit circadian nitrogen-fixing rhythm. The <span class="hlt">observation</span> of the circadian photosynthetic rhythm of this strain was recently reported by the authors. In this work, the dissolved-oxygen variation in the culture of Cyanothece RF-1 was recorded, which would reveal the photosynthetic activity of the strain. For a culture of about 1x10^8 cells/ml in concentration, a <span class="hlt">period</span>-doubling pattern was clearly displayed in the circadian photosynthetic rhythm signals. The mechanism corresponding to this nonlinear effect will be discussed. These results represent the first <span class="hlt">observation</span> of the <span class="hlt">period</span> doubling in the circadian rhythm of a prokaryotic cyanobacterium.</p> <div class="credits"> <p class="dwt_author">Yen, Tsu-Chiang; Cheng, Da-Long</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">66</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011ASPC..451...39Y"> <span id="translatedtitle"><span class="hlt">Observation</span> and Study of the Short-<span class="hlt">Period</span> Algol-Type Binaries</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The Algol-type binaries with EA- or EB-type light curves, are semi-detached interacting binary systems. The more massive component with spectral type from textrm{B} to textrm{A} is a main sequence star, while the less massive secondary component is a giant or subgiant with spectral type of textrm{F} or later-textrm{G}. Many special phenomena and physical processes make Alogls interesting objects. Based on 434 identified Algols, the orbital <span class="hlt">periods</span> for one-third of sample stars are less than 1fd5, which is considered as a principle for selecting the short-<span class="hlt">period</span> Algol-type binaries. Nine sample binaries have been studied. Based on 312 eclipsing times, the <span class="hlt">period</span> variations of AO Ser were analyzed and photometric solution of GW Gem are deduced from new BVR <span class="hlt">observations</span>. Combining with the characteristics of orbital <span class="hlt">period</span> changes, the short-<span class="hlt">period</span> Algols with P<1fd5 may evolve from the semidetached configuration into the contact configuration by three possible evolutionary scenarios.</p> <div class="credits"> <p class="dwt_author">Yang, Y.; Wei, J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">67</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/41983155"> <span id="translatedtitle">Viking magnetic and electric field <span class="hlt">observations</span> of <span class="hlt">periodic</span> Pc 1 waves: Pearl pulsations</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Pearl pulsations, with an average repetition <span class="hlt">period</span> of 60 s, were recorded using the magnetic and electric field experiments on the polar-orbiting Viking satellite. The wave event occurred on September 30, 1986, during Viking orbit 1212 at 1030 MLT, from L=3.6 to L=4.1, and at an altitude of 13,500 km. Electron density <span class="hlt">observations</span> obtained from Viking show that the waves</p> <div class="credits"> <p class="dwt_author">R. E. Erlandson; B. J. Anderson; L. J. Zanetti</p> <p class="dwt_publisher"></p> <p class="publishDate">1992-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">68</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011AGUFM.A31D0114S"> <span id="translatedtitle"><span class="hlt">Observed</span> Temporal Evolution of Global Mean Age of Stratospheric Air for the 2002 to 2010 <span class="hlt">Period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">According to model calculations, the meridional circulation is expected to intensify as a result of climate change, and mean age of stratospheric air is expected to decrease. However, an <span class="hlt">observational</span> data set presented recently (Engel et al., 2009) and consisting of 27 balloon samples of the age of air tracers carbon dioxide and sulfur hexafluoride covering the years 1975 to 2005 did not confirm the model predictions. As a contribution to the ongoing discussion, an extensive <span class="hlt">observational</span> data set, consisting of more than 1 Million SF6 vertical profiles distributed globally is presented here. It has been derived from the MIPAS instrument covering the <span class="hlt">period</span> 2002 to 2010 and has been converted into mean age of stratospheric air by referring to a combined data set of in-situ and flask global mean tropospheric SF6 measurements provided by NOAA/ESRL. During conversion into age of air, the non-linearity of tropospheric SF6 increase has been corrected for by convolution with the age spectrum within an iterative approach. Monthly zonal means of mean age of air, binned at 10 deg latitude and 1-2 km altitude, were analyzed with respect to their temporal variation by fitting a regression model consisting of a constant and a linear increase term, 2 proxies for the QBO variation, sinusoidal terms for the seasonal and semi-annual variation and overtones for the correction of the shapes to the <span class="hlt">observed</span> data set. The impact of subsidence of mesospheric SF6-depleted air and in-mixing into non-polar latitudes on mid-latitudinal absolute age of air and the age-of-air linear increase was assessed and found to be small. The linear increase of mean age of stratospheric air was found to be positive and partly larger than the trend derived by Engel et al. (2009) for most of the Northern mid-latitudes, the middle stratosphere in the tropics, and parts of the Southern mid-latitudes, as well as for the Southern polar upper stratosphere. Multi-year decrease of age of air was found for the lowermost and the upper stratospheric tropics, for parts of Southern mid-latitudes, and for the Northern polar regions. Analysis of the amplitudes and phases of the seasonal variation shed light on the coupling of stratospheric regions to each other. In particular, the Northern mid-latitude stratosphere is well coupled to the tropics, while the Northern lowermost mid-latitudinal stratosphere is decoupled, confirming the separation of the shallow branch of the Brewer-Dobson circulation from the deep branch. We <span class="hlt">suggest</span> an overall increased tropical upwelling, together with weakening of mixing barriers, especially in the Northern hemisphere, as a hypothetical model to explain the <span class="hlt">observed</span> pattern of linear multi-year increase/decrease, and amplitudes and phase shifts of the seasonal variation. Reference: Engel, A., Möbius, T., Bönisch, H., Schmidt, U., Heinz, R., Levin, I., Atlas, E., Aoki, S., Nakazawa, T., Sugawara, S., Moore, F., Hurst, D., Elkins, J., Schauffler, S., Andrews, A., and Boering, K.: Age of stratospheric air unchanged within uncertainties over the past 30 years, Nature Geosci., 2, 28--31, doi:10.1038/ngeo388, 2009.</p> <div class="credits"> <p class="dwt_author">Stiller, G. P.; von Clarmann, T.; Haenel, F.; Funke, B.; Glatthor, N.; Grabowski, U.; Kellmann, S.; Kiefer, M.; Linden, A.; Lossow, S.; Lopez-Puertas, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">69</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010AGUFMSM32A..04M"> <span id="translatedtitle">Saturn's Ionospheric Clock(s): A Concept for Generating and Maintaining Saturn's <span class="hlt">Observed</span> Magnetospheric <span class="hlt">Periodicities</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Saturn’s 10.X hour <span class="hlt">periodicity</span>, <span class="hlt">observed</span> throughout the magnetosphere, remains a mystery. It has been <span class="hlt">observed</span> in many regions, modulating many phenomena. During the Cassini mission most <span class="hlt">observations</span> have shown a <span class="hlt">period</span> at about 10.8 hours, expressed in Saturn kilometric radiation from the high latitude auroral zone, in magnetic field components (both equatorial and high latitude) from 3 to 12 Rs, in current sheet encounters in the outer magnetosphere and magnetotail, in energetic neutral atom emission from the equatorial magnetosphere, and in plasma and energetic particles throughout the magnetosphere. More recently, various authors have shown at least two dominant <span class="hlt">periods</span> expressed (in SKR and in magnetic field components), with slightly different values in the southern and northern hemispheres. The cause of this behavior is still not accounted for. Although loosely associated with Saturn’s rotation, the variability in the <span class="hlt">period</span> precludes a direct connection with Saturn’s interior (e.g., a magnetic anomaly). Other candidates that have been discussed by others are an ionospheric source (conductivity anomaly), a perturbation in the cold plasma circulation pattern, a magnetospheric cam, asymmetric ring current particle pressure, and/or a natural frequency of the magnetosphere (cavity mode or traveling wave front of some sort). In this paper we present a concept that derives its energy from the subcorotating cold, dense plasma (which exhibits a rotation <span class="hlt">period</span> on the order of 13 to 14 hours throughout L-shells between ~3 and 20), but is triggered by a process linked with the ionosphere. Key components of the model include significant slippage between the ionosphere and the magnetosphere (with the ionosphere rotating at the expressed <span class="hlt">period</span> in each hemisphere, only slightly more slowly than the planet interior), subcorotating cold dense plasma with a source in the inner magnetosphere, predominantly radial transport of the cold dense plasma in the rotational frame of the cold plasma, and the episodic release of plasma, primarily from the night side outer magnetosphere, when a critical loading criterion has been reached. For one dominant ionospheric driver, the cartoon in the figure describes the behavior of the cold plasma.</p> <div class="credits"> <p class="dwt_author">Mitchell, D. G.; Brandt, P. C.; Ukhorskiy, A. Y.</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">70</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4350878"> <span id="translatedtitle">Management of Toxoplasmic Retinochoroiditis during Pregnancy, Postpartum <span class="hlt">Period</span> and Lactation: Clinical <span class="hlt">Observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Background During pregnancy and labor, the immune response is physiologically impaired and women are more susceptible to infections. Since many drugs may have potentially adverse effects on the fetus and newborn, less aggressive treatment regimens should be considered in pregnant and lactating patients. The aim of our study was to present the management of toxoplasmic retinochoroiditis during pregnancy, postpartum <span class="hlt">period</span>, and lactation. Material/Methods A retrospective study was undertaken of the clinical records of 24 women during pregnancy, postpartum <span class="hlt">period</span>, and lactation who were referred in the years 1994–2014 to the Department of Zoonoses and Tropical Diseases or the Department of Ophthalmology, Medical University of Warsaw for toxoplasmic retinochoroiditis. The diagnosis was based on the typical ophthalmoscopic picture, confirmed by serological testing using an ELISA method. Results A total of 28 attacks of toxoplasmic retinochoroiditis were <span class="hlt">observed</span> in 24 patients during pregnancy, postpartum <span class="hlt">period</span>, and lactation. The choice of treatment was guided by the character and location of the inflammatory lesion and the gestational age. Topical (steroidal/nonsteroidal eye drops) and systemic treatments with spiramycin or azithromycin, Fansidar (pyrimethamine 25 mg/sulfadoxine 500 mg), and prednisone were used. Conclusions Management of toxoplasmic retinochoroiditis during pregnancy, postpartum <span class="hlt">period</span>, or lactation must be individualized and guided by the gestational age and location of the active lesion. Women of childbearing age with toxoplasma ocular lesions should be informed by their doctors about possible active recurrences during pregnancy and followed carefully by an ophthalmologist when pregnant. PMID:25711713</p> <div class="credits"> <p class="dwt_author">Brydak-Godowska, Joanna; Moneta-Wielgo?, Joanna; K?cik, Dariusz; Borkowski, Piotr Karol</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">71</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011ApJ...728...16H"> <span id="translatedtitle">Infrared Spectroscopic <span class="hlt">Observations</span> of the Secondary Stars of Short-<span class="hlt">period</span> Sub-gap Cataclysmic Variables</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We present K-band spectroscopy of short-<span class="hlt">period</span>, "sub-gap" cataclysmic variable (CV) systems obtained using ISAAC on the Very Large Telescope. We show the infrared (IR) spectra for nine systems below the 2-3 hr <span class="hlt">period</span> gap: V2051 Oph, V436 Cen, EX Hya, VW Hyi, Z Cha, WX Hyi, V893 Sco, RZ Leo, and TY PsA. We are able to clearly detect the secondary star in all but WX Hyi, V893 Sco, and TY PsA. We present the first direct detection of the secondary stars of V2051 Oph, V436 Cen, and determine new spectral classifications for EX Hya, VW Hyi, Z Cha, and RZ Leo. We find that the CO band strengths of all but Z Cha appear normal for their spectral types, in contrast to their longer <span class="hlt">period</span> cousins above the <span class="hlt">period</span> gap. This brings the total number of CVs and pre-CVs with moderate resolution (R >~ 1500) IR spectroscopy to 61 systems: 19 pre-CVs, 31 non-magnetic systems, and 11 magnetic or partially magnetic systems. We discuss the trends seen in the IR abundance patterns thus far and highlight a potential link between anomalous abundances seen in the IR with the C IV/N V anomaly seen in the ultraviolet. We present a compilation of all systems with sufficient resolution IR <span class="hlt">observations</span> to assess the CO band strengths and, by proxy, obtain an estimate on the C abundance on the secondary star.</p> <div class="credits"> <p class="dwt_author">Hamilton, Ryan T.; Harrison, Thomas E.; Tappert, Claus; Howell, Steve B.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-02-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">72</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25711713"> <span id="translatedtitle">Management of Toxoplasmic Retinochoroiditis during Pregnancy, Postpartum <span class="hlt">Period</span> and Lactation: Clinical <span class="hlt">Observations</span>.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Background During pregnancy and labor, the immune response is physiologically impaired and women are more susceptible to infections. Since many drugs may have potentially adverse effects on the fetus and newborn, less aggressive treatment regimens should be considered in pregnant and lactating patients. The aim of our study was to present the management of toxoplasmic retinochoroiditis during pregnancy, postpartum <span class="hlt">period</span>, and lactation. Material and Methods A retrospective study was undertaken of the clinical records of 24 women during pregnancy, postpartum <span class="hlt">period</span>, and lactation who were referred in the years 1994-2014 to the Department of Zoonoses and Tropical Diseases or the Department of Ophthalmology, Medical University of Warsaw for toxoplasmic retinochoroiditis. The diagnosis was based on the typical ophthalmoscopic picture, confirmed by serological testing using an ELISA method. Results A total of 28 attacks of toxoplasmic retinochoroiditis were <span class="hlt">observed</span> in 24 patients during pregnancy, postpartum <span class="hlt">period</span>, and lactation. The choice of treatment was guided by the character and location of the inflammatory lesion and the gestational age. Topical (steroidal/nonsteroidal eye drops) and systemic treatments with spiramycin or azithromycin, Fansidar (pyrimethamine 25 mg/sulfadoxine 500 mg), and prednisone were used. Conclusions Management of toxoplasmic retinochoroiditis during pregnancy, postpartum <span class="hlt">period</span>, or lactation must be individualized and guided by the gestational age and location of the active lesion. Women of childbearing age with toxoplasma ocular lesions should be informed by their doctors about possible active recurrences during pregnancy and followed carefully by an ophthalmologist when pregnant. PMID:25711713</p> <div class="credits"> <p class="dwt_author">Brydak-Godowska, Joanna; Moneta-Wielgo?, Joanna; K?cik, Dariusz; Borkowski, Piotr Karol</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">73</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012cosp...39.1272E"> <span id="translatedtitle">Confrontation Between a Quantized <span class="hlt">Periods</span> of Some Exo-planetary Systems and <span class="hlt">Observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Confrontation Between a Quantized <span class="hlt">Periods</span> of Some Exo-planetary Systems and <span class="hlt">Observations</span> A.B. Morcos Corot and Kepler were designed to detect Earth-like extra solar planets. The orbital elements and <span class="hlt">periods</span> of these planets will contain some uncertainties. Many theoretical treatments depend on the idea of quantization were done aiming to find orbital elements of these exoplenets. In the present work, as an extension of previous works, the <span class="hlt">periods</span> of some extoplanetary systems are calculated by using a simple derived formula. The orbital velocities of some of them are predicted . A comparison between the calculated and <span class="hlt">observed</span> data is done References 1-J.M. Barnothy , the stability of the Solar System and of small Stellar Systems . (Y.Kazai edn,IAU,1974). 2-L.Nottale,Fractal Space-Time and Microphysics,Towards a Theory of Scale Relativity,( World Scientific, London,1994). 3-L. Nottale, A&A Lett. 315, L9 (1996). 4-L. Nottale, G. Schumacher and J. Gay, A&A , 322, 1018 , (1997). 5-L. Nottale, A&A , 361, 379 (2000). 6-A.G. Agnese and R.Festa, arXiv:astro-ph/9807186v1, (1998). 7-A.G. Agnese and R.Festa, arXiv:astro-ph/9910534v2. (1999). 8- A.B.Morcos, MG 12 , France (2009). 9- A.B.Morcs, Cospar 38 , Bremen , Germany (2010)</p> <div class="credits"> <p class="dwt_author">El Fady Morcos, Abd</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">74</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011jsrs.conf..137G"> <span id="translatedtitle"><span class="hlt">Observing</span> and modeling long-<span class="hlt">period</span> tidal variations in polar motion</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">By exchanging angular momentum with the solid Earth, ocean tides cause the Earth's rotation to change. While hydrodynamic tide models have been used to study the effect of ocean tides on polar motion, it is shown here that none of the published models can fully account for the <span class="hlt">observed</span> variations. An empirical ocean tide model is therefore determined by fitting <span class="hlt">periodic</span> terms at the tidal frequencies to polar motion excitation <span class="hlt">observations</span> spanning 1980.0-2010.4 from which atmospheric and non-tidal oceanic effects were removed. While the empirical ocean tide model does fully account for all of the <span class="hlt">observed</span> tidal power, tests indicate that the model may not have completely converged. So better models of the effects of ocean tides on polar motion are still needed, both dynamical and empirical.</p> <div class="credits"> <p class="dwt_author">Gross, R. S.; Dickman, S. R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-10-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">75</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20110020642&hterms=Tidal+Power&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3DTidal%2BPower"> <span id="translatedtitle"><span class="hlt">Observing</span> and Modeling Long-<span class="hlt">Period</span> Tidal Variations in Polar Motion</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">By exchanging angular momentum with the solid Earth, ocean tides cause the Earth's rotation to change. While hydrodynamic tide models have been used to study the effect of ocean tides on polar motion, it is shown here that none of the published models can fully account for the <span class="hlt">observed</span> variations. An empirical ocean tide model is therefore determined by fitting <span class="hlt">periodic</span> terms at the tidal frequencies to polar motion excitation <span class="hlt">observations</span>, from which atmospheric and non-tidal oceanic effects were removed. While the empirical ocean tide model does fully account for allof the <span class="hlt">observed</span> tidal power, tests indicate that the model may not have completely converged. So better models of the effects of ocean tides on polar motion are still needed, both dynamical and empirical.</p> <div class="credits"> <p class="dwt_author">Gross, Richard S.; Dickman, S. R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">76</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20060009467&hterms=gsm&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dgsm"> <span id="translatedtitle">Cluster <span class="hlt">observations</span> of quasi-<span class="hlt">periodic</span> impulsive signatures in the dayside northern lobe: High-latitude flux transfer events?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">We report on a series of quasi-<span class="hlt">periodic</span> reversals in GSM B(sub Z) <span class="hlt">observed</span> by the four Cluster spacecraft in the northern dayside lobe poleward of the cusp on 23 February 2001. During an interval of about 35 min, multiple reversals (negative to positive) in B(sub Z) of approximately 1-min duration with an approximate 8-min recurrence time were <span class="hlt">observed</span>. The individual structures do not resemble low-latitude flux transfer events (FTE) [Russell and Elphic, 1979] but the 8-min recurrence frequency <span class="hlt">suggests</span> that intermittent reconnection may be occurring .Measurements (appropriately lagged) of the solar wind at ACE show that the IMF was southward-oriented with a strong B(sub X) and that a modest dynamic pressure increased as the events started. The multi-point <span class="hlt">observations</span> afforded by the Cluster spacecraft were used to infer the motion (direction and speed) of the <span class="hlt">observed</span> magnetic field reversals. The associated currents were also calculated and they are consistent with the spatial confinement of the <span class="hlt">observed</span> magnetic field reversals. We propose that the <span class="hlt">observed</span> reversals are due to flux tubes reconnecting with closed field lines on the dayside. Ancillary data from the Cluster Ion Spectrometry (CIS) and Plasma Electron And Current Experiment (PEACE) instruments were used to develop a physical picture of the reversals.</p> <div class="credits"> <p class="dwt_author">Thompson, S. M.; Kivelson, M. G.; Khurana, K. K.; Balogh, A.; Reme, H.; Fazakerley, A. N.; Kistler, L. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">77</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/1993P%26SS...41.1079R"> <span id="translatedtitle"><span class="hlt">Periodicities</span> of Jovian broad-band kilometric radiation <span class="hlt">observed</span> by Ulysses</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary"><span class="hlt">Observations</span> of the Unified Radio and Plasma Wave (URAP) instrument onboard the Ulysses spacecraft have been used to analyze <span class="hlt">periods</span> inherent in the Jovian broad-banded kilometric radio emission (bKOM) between 29 and 47 kHz. It is demonstrated, by using power spectrum analysis and linear prediction time filtering that the long-term fluctuations of the bKOM signal are triggered by the solar wind, particularly by the solar wind density, while no association was found with the solar wind velocity. In addition, there seem to be some inherent <span class="hlt">periodicities</span> in the bKOM events which cannot be fully attributed to the influence of solar wind plasma quantities by these techniques.</p> <div class="credits"> <p class="dwt_author">Rabl, G. K. F.</p> <p class="dwt_publisher"></p> <p class="publishDate">1993-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">78</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19890050304&hterms=Ocean+wave+power&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3D%2528%2528Ocean%2Bwave%2529%2Bpower%2529"> <span id="translatedtitle"><span class="hlt">Observations</span> of 20-day <span class="hlt">period</span> meridional current oscillations in the upper ocean along the Pacific Equator</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Prominent oscillations of the meridional current, with a mean <span class="hlt">period</span> of approximately 20 days, is <span class="hlt">observed</span> in the upper ocean from May 1979 to October 1985 using moored current measurements along the Pacific equator at 95, 110, 124, 140, and 152 deg W, as well as off (but near) the equator at 110 and 140 deg W. The fluctuations are relatively narrowband in frequency. A 95 percent statistically significant peak in the power spectra of the meridional current occurs at 110, 124, and 140 deg W, but not at 95 and 152 deg W where the spectral peaks are smaller. The dominant wave <span class="hlt">period</span> decreases by about 4 percent from 110 to 140 deg W. The wave amplitude decreases with depth, and the wave is essentially confined to the upper 80 m. The penetration depth of the oscillation is greatest at 110 deg W and least at 140 deg W.</p> <div class="credits"> <p class="dwt_author">Halpern, David; Knox, Robert A.; Luther, Douglas S.</p> <p class="dwt_publisher"></p> <p class="publishDate">1988-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">79</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/21583171"> <span id="translatedtitle">SOHO/SWAN <span class="hlt">OBSERVATIONS</span> OF SHORT-<span class="hlt">PERIOD</span> SPACECRAFT TARGET COMETS</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">SWAN, the Solar Wind ANisotropies all-sky hydrogen Ly{alpha} camera on the Solar and Heliospheric Observatory spacecraft that makes all-sky images of interplanetary neutral hydrogen, has an ongoing campaign to make special <span class="hlt">observations</span> of comets, both short- and long-<span class="hlt">period</span> ones, in addition to the serendipitous <span class="hlt">observations</span> of comets as part of the all-sky monitoring program. We report here on a study of several short-<span class="hlt">period</span> comets that were detected by SWAN: 21P/Giacobini-Zinner (1998 and 2005 apparitions), 19P/Borrelly (2001 apparition), 81P/Wild 2 (1997 apparition), and 103P/Hartley 2 (1997 apparition). SWAN <span class="hlt">observes</span> comets over long continuous stretches of their visible apparitions and therefore provides excellent temporal coverage of the water production. For some of the <span class="hlt">observations</span> we are also able to analyze an entire sequence of images over many days to several weeks/months using our time-resolved model and extract daily average water production rates over continuous <span class="hlt">periods</span> of several days to months. The short-term (outburst) and long-term behavior can be correlated with other <span class="hlt">observations</span>. The overall long-term variation is examined in light of seasonal effects seen in the pre- to post-perihelion differences. For 21P/Giacobini-Zinner and 81P/Wild 2 the activity variations over each apparition were more continuously monitored but nonetheless consistent with previous <span class="hlt">observations</span>. For 19P/Borrelly we found a very steep variation of water production rates, again consistent with some previous <span class="hlt">observations</span>, and a variation over six months around perihelion that was reasonably consistent with the spin-axis model of Schleicher et al. and the illumination of the main active areas. During the 1997-1998 apparition of 103P/Hartley 2, the target comet of the EPOXI mission (the Deep Impact extended mission), we found a variation with heliocentric distance ({approx}r{sup -3.6}) that was almost as steep as 19P/Borrelly and, given the small measured radius near aphelion, this places a number of possible constraints on the size, shape, and/or distribution active of areas on the surface.</p> <div class="credits"> <p class="dwt_author">Combi, M. R.; Lee, Y.; Patel, T. S. [Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109-2143 (United States); Maekinen, J. T. T. [Finnish Meteorological Institute, P.O. Box 503, SF-00101 Helsinki (Finland); Bertaux, J.-L.; Quemerais, E., E-mail: mcombi@umich.edu [LATMOS, CNRS/INSU, Universite de Versailles Saint-Quentin, 11 Bd d'Alembert, 78280 Guyancourt (France)</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-04-15</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">80</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010AGUFM.S53F..07I"> <span id="translatedtitle"><span class="hlt">Observations</span> of Long-<span class="hlt">Period</span> Rotational Ground Motions: From Ambient Noise to Earth's Free Oscillations</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">After some technical improvements to the ring laser system measuring the vertical component of rotation rate at Wettzell, Germany, in 2009 a marked improvement of the signal-to-noise ratio for the broad-band frequency range of seismic <span class="hlt">observations</span> could be achieved. This led to the first direct <span class="hlt">observation</span> of rotational ground motions induced by toroidal free oscillations of the Earth, following the Mw=8.1 Samoa earthquake on September 29, 2009 and the Mw=8.8 Chile earthquake on February 27, 2010. <span class="hlt">Observations</span> are compared with synthetic seismograms computed by summing normal modes. Amplitude spectra of real and synthetic data are analyzed to interpret the <span class="hlt">observations</span>. We show that several toroidal modes can be detected in the ring laser data and that our <span class="hlt">observations</span> are in reasonable agreement with the synthetic spectra. This indicates that long-<span class="hlt">period</span> seismology can benefit from measurements of rotational ground motion measurements using ring lasers in the future. In addition, analysis of earthquake-free time windows of the ring laser records leads us to the conclusion that we consistently <span class="hlt">observe</span> Love waves generated in the two ocean-generated microseismic frequency bands and that the azimuth of the source areas can be estimated from joint analysis with translation records from a collocated broadband seismometer.</p> <div class="credits"> <p class="dwt_author">Igel, H.; Kurrle, D.; Ferreira, A. M.; Wassermann, J. M.; Gaebler, P.; Schreiber, K. U.</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-12-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_3");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a style="font-weight: bold;">4</a> <a 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href="#">12</a> <a onClick='return showDiv("page_13");' href="#">13</a> <a onClick='return showDiv("page_14");' href="#">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a onClick='return showDiv("page_16");' href="#">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a onClick='return showDiv("page_21");' href="#">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_6");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">81</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015JHyd..520...52M"> <span id="translatedtitle">Solute transport in <span class="hlt">periodical</span> heterogeneous porous media: Importance of <span class="hlt">observation</span> scale and experimental sampling</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This paper focuses on the effects of the <span class="hlt">observation</span> scale and sampling on the dispersion of tracers in <span class="hlt">periodical</span> heterogeneous porous media. A Model Heterogeneous Porous Medium (MHPM) with a high degree of heterogeneity was built. It consists of a preferential flow path surrounded by glass beads. 44 tracer experiments were carried out on several series of <span class="hlt">periodic</span> MHPM to investigate the effect of the <span class="hlt">observation</span> scale on solute dispersion. Each series was replicated several times, allowing for a statistical description of the unit transfer function of the MHPM. No significant trend was found for the dispersion coefficient as a function of the size of the MHPM. However, given the variability of the breakthrough curves from one experiment replicate to another, under-sampling might easily lead to conclude that the dispersion coefficient is variable with distance. Depending on the samples used, it would be as easy to (wrongly) detect an increasing trend as to detect a decreasing one. A confidence interval analysis of the experimental breakthrough curves in the Laplace space shows that (i) there exists a model with scale independent parameters that can describe the experimental breakthrough curves within the limits of experimental uncertainty, (ii) this model is not the advection-dispersion (AD) model, (iii) the modelling error of the AD model decreases with the number of <span class="hlt">periods</span>, (iv) the size of the Reference Elementary Volume for the dispersion coefficient is between 10 and 20 <span class="hlt">periods</span>. The effects of sampling prove to override those of scaling. This, with the invalidity of the AD model, leads to question attempts to calibrate and/or identify trends in the dispersion coefficient at intermediate scales from a limited number of experiment replicates.</p> <div class="credits"> <p class="dwt_author">Majdalani, S.; Chazarin, J. P.; Delenne, C.; Guinot, V.</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">82</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013SoPh..285..141C"> <span id="translatedtitle">Results of IPS <span class="hlt">Observations</span> in the <span class="hlt">Period</span> Near Solar Activity Minimum</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">IPS <span class="hlt">observations</span> with the Big Scanning Array of Lebedev Physical Institute (BSA LPI) radio telescope at the frequency 111 MHz have been monitored since 2006. All the sources, about several hundred daily, with a scintillating flux greater than 0.2 Jy are recorded for 24 hours in the 16 beams of the radio telescope covering a sky strip of 8? declination width. We present some results of IPS <span class="hlt">observations</span> for the recent <span class="hlt">period</span> of low solar activity considering a statistical ensemble of scintillating radio sources. The dependences of the averaged over ensemble scintillation index on heliocentric distance are considerably weaker than the dependence expected for a spherically symmetric geometry. The difference is especially pronounced in the year 2008 during the very deep solar activity minimum <span class="hlt">period</span>. These features are explained by the influence of the heliospheric current sheet that is seen as a strong concentration of turbulent solar wind plasma aligned with the solar equatorial plane. A local maximum of the scintillation index is found in the anti-solar direction. Future prospects of IPS <span class="hlt">observations</span> using BSA LPI are briefly discussed.</p> <div class="credits"> <p class="dwt_author">Chashei, I. V.; Shishov, V. I.; Tyul'bashev, S. A.; Subaev, I. A.; Oreshko, V. V.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-07-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">83</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011AGUFMSA41B1863M"> <span id="translatedtitle">Time <span class="hlt">Periods</span> of Unusual Density Behavior <span class="hlt">Observed</span> by GRACE and CHAMP</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Time <span class="hlt">periods</span> of low cross correlation between precision orbit ephemeris (POE) derived density and accelerometer density for CHAMP and GRACE are examined. In particular, the cross correlation for GRACE dropped from typical values near 0.9 to much lower values and then returned to typical over the time <span class="hlt">period</span> of late October to late December of 2005. This time <span class="hlt">period</span> includes a maneuver where GRACE-A and GRACE-B swapped positions. However, the drop in cross correlation begins and reaches its low point before the maneuvers begin. In addition, the densities were found using GRACE-A, but GRACE-B did most of the maneuvering. The time <span class="hlt">period</span> is characterized by high frequency variations in accelerometer density of the same magnitude as the daylight to eclipse variations over the course of an orbit. However, the daylight to eclipse variations are particularly small during this time <span class="hlt">period</span> because the orbit plane is near the terminator. Additionally, the difference between the accelerometer and POE derived densities are not unusually large during this time <span class="hlt">period</span>. This implies the variations are not unusual, just more significant when the orbit plane is near terminator. Cyclical variations in correlation of the POE derived densities with accelerometer derived densities are seen for both GRACE and CHAMP, but the magnitude of the variations are much larger for GRACE, possibly because of the higher altitude of GRACE. The cycles seem to be phased so that low correlations occur with low beta angle when the orbit plane is near the terminator. The low correlation is possibly caused by the lower amplitude of the daylight to eclipse signal making higher frequency variations relatively more important. However, another possible explanation is terminator waves in density that propagate to the thermosphere from lower in the atmosphere. These waves have been <span class="hlt">observed</span> in CHAMP accelerometer data and global circulation model simulations. Further investigation is needed to see if the variations correspond to terminator waves or if they represent typical high frequency signal from another source that is more apparent when the orbit plane is near the terminator. 1. C. A. McLaughlin, E. Fattig, D. Mysore Krishna, and P. M. Mehta, "Time <span class="hlt">Periods</span> of Anomalous Density for GRACE and CHAMP," AAS/AIAA Astrodynamics Specialists Conference, AAS 11-613, Girdwood, AK, August 2011. 2. C. A. McLaughlin, A. Hiatt, and T. Lechtenberg, "Calibrating Precision Orbit Derived Total Density," Journal of Spacecraft and Rockets, Vol. 48, No. 1, January-February 2011, pp. 166-174.</p> <div class="credits"> <p class="dwt_author">McLaughlin, C. A.; Fattig, E.; Mysore Krishna, D.; Locke, T.; Mehta, P. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">84</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19810029928&hterms=x-ray+mini&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dx-ray%2Bmini"> <span id="translatedtitle">The continuous spectrum of Markarian 421 during <span class="hlt">periods</span> of X-ray satellite <span class="hlt">observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">New UBVRI photometry of Mrk 421 obtained during <span class="hlt">periods</span> of X-ray satellite <span class="hlt">observations</span> are presented. An X-ray light curve for 1977 November from the HEAO A-1 experiment is also given. The decomposition of the UBVR fluxes into a compact nonthermal component and an extended galactic component shows that there are coordinated variations in the optical nonthermal and X-ray emission. The data are consistent with the hypothesis that the mini-BL Lac object is emitting by the synchrontron-self-Compton process. The host galaxy of this composite source has properties like those of a giant elliptical.</p> <div class="credits"> <p class="dwt_author">Mufson, S. L.; Wood, K.; Mcnutt, D. P.; Yentis, D. J.; Meekins, J. F.; Byram, E. T.; Chubb, T. A.; Friedman, H.; Wisniewski, W. Z.</p> <p class="dwt_publisher"></p> <p class="publishDate">1980-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">85</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/60463440"> <span id="translatedtitle"><span class="hlt">Observations</span> and modelling of winds and waves during the surface wave dynamics experiment. Report 2. Intensive <span class="hlt">observation</span> <span class="hlt">period</span> IOP3, 25 February9 March 1991. Technical report</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">This report describes the compilation of <span class="hlt">observed</span> and modelled wind, wave and current parameters during the third intensive <span class="hlt">observation</span> <span class="hlt">period</span> (IOP-3) from February 25 to March 9, 1991, of the Surface Wave Dynamics Experiment. The measurements include wind speed and direction, wave heights and <span class="hlt">periods</span>, air and sea temperatures, and atmospheric pressures from four directional wave buoys, two meteorological buoys,</p> <div class="credits"> <p class="dwt_author">M. J. Caruso; H. C. Graber; R. E. Jensen; M. A. Donelan</p> <p class="dwt_publisher"></p> <p class="publishDate">1994-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">86</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/1983PhRvL..51..562H"> <span id="translatedtitle"><span class="hlt">Observation</span> of <span class="hlt">period</span> doubling in an all-optical resonator containing NH3 gas</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">It is pointed out that systems exhibiting <span class="hlt">period</span>-doubling cascades to chaotic behavior while governed by deterministic equations have attracted great interest. Ikeda (1979) showed that an optically bistable ring resonator containing a two-level system can show a <span class="hlt">period</span>-doubling cascade, a sufficiently strong CW input beam yielding an output oscillating at twice the resonator round-trip time t(R). On further increase of the input field the output <span class="hlt">period</span> doubles to chaos. The present investigation is concerned with <span class="hlt">observations</span> of 2t(R) oscillation, with some indications of 4t(R), in an all-optical system very similar to Ikeda's original proposal. A passive ring resonator was pumped by a transversely excited atmosphere (TEA) CO2 laser pulse. The employed line lies 1.23 GHz above the aR(11) transition of the NH3 gas contained in a 1-m intracacity cell at pressures of 9-15 Torr, where it acts as a homogeneously broadened two-level system. The obtained results show that molecular gases pumped by CO2 lasers are extremely promising media for the study of chaos in all-optical systems.</p> <div class="credits"> <p class="dwt_author">Harrison, R. G.; Firth, W. J.; Emshary, C. A.; Al-Saidi, I. A.</p> <p class="dwt_publisher"></p> <p class="publishDate">1983-08-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">87</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19760026034&hterms=gamma+emitting+natural&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dgamma%2Bemitting%2Bnatural"> <span id="translatedtitle"><span class="hlt">Observation</span> of gamma rays with a 4.8 hour <span class="hlt">periodicity</span> from CYG X-3</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Energetic (E35 MeV) Gamma rays were <span class="hlt">observed</span> from Cyg X-3 with the SAS-2 Gamma ray telescope. They are modulated at the 4.8 sup h <span class="hlt">period</span> <span class="hlt">observed</span> in the X-ray and infrared regions, and within the statistical error are in phase with this emission. The flux above 100 MeV has an average value of (4.4 + or - 1.1)x 10 to the -6 power/sq cm/sec. If the distance to Cyg X-3 is 10 kpcs, this flux implies a luminosity of more than 10 to the 37th power ergs/s if the radiation is isotropic and about 10 to the 36th power ergs/s if the radiation is restricted to a cone of one steradian, as it might be in a pulsar.</p> <div class="credits"> <p class="dwt_author">Lamb, R. C.; Fichtel, C. E.; Hartman, R. C.; Kniffen, D. A.; Thompson, D. J.</p> <p class="dwt_publisher"></p> <p class="publishDate">1976-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">88</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/1985iue..prop.2211R"> <span id="translatedtitle">Coordinated <span class="hlt">Observations</span> of Rotational Modulation in Long <span class="hlt">Period</span> RS CVn Systems</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This proposal requests IUE time to obtain SWP low dispersion spectra during 10 US2 shifts during the Fall of 1985. The targets are all late G or early K giants in long <span class="hlt">period</span> active chromosphere RS Canum Venaticorum binary systems. The research goal is to discern the spatial relationship and extent of the surface active regions in both the horizontal and vertical directions. Ground based <span class="hlt">observations</span> will be obtained contemporaneously over the fall season. We will use the C IV line as the primary activity indicator in the stellar transition region, whereas ground based <span class="hlt">observations</span> will supply information on the chromosphere and photosphere. We will particularly be seeking information on the relative shape and phase lead or lag of the transition region emission relative to the chromospheric and photospheric rotational phase behavior.</p> <div class="credits"> <p class="dwt_author">Ramsey, Lawrence</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">89</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/44484987"> <span id="translatedtitle">The Global Hydrologic and Energy Cycles: <span class="hlt">Suggestions</span> for Studies in the Pre-Global Energy and Water Cycle Experiment (GEWEX) <span class="hlt">Period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Given the importance of a quantitative understanding of the way in which water and energy are moved from place to place and from component to component of the earth's climate system, it is necessary to obtain reliable estimates of the hydrologic and energy cycles in the global atmosphere. While a number of <span class="hlt">observing</span> platforms designed to address this problem are</p> <div class="credits"> <p class="dwt_author">J. L. Kinter; J. Shukla</p> <p class="dwt_publisher"></p> <p class="publishDate">1990-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">90</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20030053372&hterms=APRIL&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3DAPRIL"> <span id="translatedtitle">RHESSI <span class="hlt">Observations</span> of Flares During the Storms <span class="hlt">Period</span> from 14 to 24 April 2002</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) <span class="hlt">observes</span> X-rays and gamma rays from solar flares in the energy range from 3 keV to 17 MeV with a duty cycle of about 50%. The RHESSI <span class="hlt">observations</span> of the flares during the Storms Workshop <span class="hlt">period</span> from 14 to 24 April, 2002, will be reviewed. Many Geostationary Operational Environmental Satellites (GOES) C- and M-class flares were <span class="hlt">observed</span> including the M2.6 flare on 17 April that was followed by a Coronal Mass Ejection (CME). The X1.5 flare on 21 April was particularly well <span class="hlt">observed</span> with RHESSI in X-rays from its start at 00:40 UT until 01:33 UT on the first orbit, just before the soft X-ray peak. Footpoint emission was detected to energies as high as 200 keV, and a spatially-separated coronal source was identified at energies below about 30 keV. The coronal X-ray source was followed for over 12 more hours on subsequent orbits as it gradually rose to over 130,000 km above the limb. The X-ray images and spectra of this flare will be presented in relation to the Transitional Region and Coronal Explorer (TRACE) images in the 195-angstrom band and the Large Angle and Spectrometric Coronagraph Experiment (LASCO) images of the associated CME.</p> <div class="credits"> <p class="dwt_author">Rabin, Douglas (Technical Monitor); Dennis, Brian R.; Gallagher, Peter T.</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">91</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://cds.cern.ch/record/707834/files/0401498.pdf"> <span id="translatedtitle">XMM-Newton EPIC & OM <span class="hlt">observations</span> of Her X-1 over the 35 day beat <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We present the results of a series of XMM-Newton EPIC and OM <span class="hlt">observations</span> of Her X-1, spread over a wide range of the 35 day precession <span class="hlt">period</span>. We confirm that the spin modulation of the neutron star is weak or absent in the low state - in marked contrast to the main or short-on states. During the states of higher intensity, we <span class="hlt">observe</span> a substructure in the broad soft X-ray modulation below ~1keV, revealing the presence of separate peaks which reflect the structure seen at higher energies. The strong fluorescence emission line at ~6.4keV is detected in all <span class="hlt">observations</span> (apart from one taken in the middle of eclipse), with higher line energy, width and normalisation during the main-on state. In addition, we report the detection of a second line near 7keV in 10 of the 15 <span class="hlt">observations</span> taken during the low-intensity states of the system. This feature is rather weak and not significantly detected during the main-on state, when the strong continuum emission dominates the X-ray spectrum. Spin resolved spectroscopy j...</p> <div class="credits"> <p class="dwt_author">Zane, S; Jiménez-Garate, M A; Den Herder, J W A; Hailey, C J; Zane, Silvia; Ramsay, Gavin; Jimenez-Garate, Mario A.; Herder, Jan Willem den; Hailey, Charles J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">92</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012EGUGA..14.8306F"> <span id="translatedtitle">The French component of the FENNEC Saharan Climate project 2011 Special <span class="hlt">Observing</span> <span class="hlt">Period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The central Sahara has one of the most extreme climates on Earth. During the northern summer months, a large low pressure system caused by intense solar heating develops over a huge, largely uninhabited expanse of northern Mali, southern Algeria and eastern Mauritania. This Saharan heat low plays a pivotal role in the West African Monsoon. Based on this, the interested French, British and German communities have decided to propose the FENNEC project which aims at (i) characterizing the Saharan atmospheric boundary layer, (ii) evaluating its representation in regional and global models, and (iii) improving "aerosol" products issued from space-borne <span class="hlt">observations</span>. A key element of this programme was the organization of an international field campaign in June 2011 over the Saharan heat low region, which will include both ground-based and airborne detachments. The Special <span class="hlt">Observing</span> <span class="hlt">Period</span> component of FENNEC-France included the implementation of the SAFIRE Falcon 20 to conduct research on the atmospheric boundary layer and the dust cycle of the Sahara, the installation of a remote sensing station in southern Spain, equipped with a backscatter lidar and a sunphotometer, to study the transport of desert dust to Europe, as well as a couple of GPS stations installed in southern Morocco to investigate the moisture inflow from the Atlantic Ocean into the Sahara. For the first time, the ALADIN and AROME models (5 and 24 km grid spacing, respectively) have been implemented operationally to provide forecasts of dust events over the Sahara and parts of the Sahel in June 2011 to assist in planning for airborne operations. This effort was complemented by the forecasts made with the Meso-NH model (5 and 20 km resolution). During the SOP <span class="hlt">period</span>, the ground-based, airborne and space-borne <span class="hlt">observations</span> have documented the evolution of dynamic properties of thermodynamic and the atmospheric boundary layer Saharan Africa (Mauritania and Mali) during the installation phase of the Saharan heat low west of the continent as well as the increase in aerosol loading associated with the phase shift of the heat low from east to west. During this <span class="hlt">period</span>, episodes of intense uplift of desert aerosols associated with various dynamic phenomena (fronts, "Mediterannean surges", "Atlantic inflow" of low-level jets, etc ...) have also been documented as well as the export of dust over the Atlantic Ocean. An overview of implementation plan and of the first <span class="hlt">observational</span> and modelling results acquired during the time of the SOP will be presented.</p> <div class="credits"> <p class="dwt_author">Flamant, C.; Chaboureau, J.-P.; Kocha, C.; Lavaysse, C.; Schepanski, K.; Chazette, P.; Bock, O.; Marticorena, B.; Tulet, P.; Pelon, J.; Marnas, F.; Mokhtari, M.; Lafore, J.-P.; Roehrig, R.; Koulali Idrissi, A.; Tsamalis, C.; Chedin, A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">93</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24040024"> <span id="translatedtitle">mtDNA from the early Bronze Age to the Roman <span class="hlt">period</span> <span class="hlt">suggests</span> a genetic link between the Indian subcontinent and Mesopotamian cradle of civilization.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Ancient DNA methodology was applied to analyse sequences extracted from freshly unearthed remains (teeth) of 4 individuals deeply deposited in slightly alkaline soil of the Tell Ashara (ancient Terqa) and Tell Masaikh (ancient Kar-Assurnasirpal) Syrian archaeological sites, both in the middle Euphrates valley. Dated to the <span class="hlt">period</span> between 2.5 Kyrs BC and 0.5 Kyrs AD the studied individuals carried mtDNA haplotypes corresponding to the M4b1, M49 and/or M61 haplogroups, which are believed to have arisen in the area of the Indian subcontinent during the Upper Paleolithic and are absent in people living today in Syria. However, they are present in people inhabiting today's Tibet, Himalayas, India and Pakistan. We anticipate that the analysed remains from Mesopotamia belonged to people with genetic affinity to the Indian subcontinent since the distribution of identified ancient haplotypes indicates solid link with populations from the region of South Asia-Tibet (Trans-Himalaya). They may have been descendants of migrants from much earlier times, spreading the clades of the macrohaplogroup M throughout Eurasia and founding regional Mesopotamian groups like that of Terqa or just merchants moving along trade routes passing near or through the region. None of the successfully identified nuclear alleles turned out to be ?F508 CFTR, LCT-13910T or ?32 CCR5. PMID:24040024</p> <div class="credits"> <p class="dwt_author">Witas, Henryk W; Tomczyk, Jacek; J?drychowska-Da?ska, Krystyna; Chaubey, Gyaneshwer; P?oszaj, Tomasz</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">94</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3770703"> <span id="translatedtitle">mtDNA from the Early Bronze Age to the Roman <span class="hlt">Period</span> <span class="hlt">Suggests</span> a Genetic Link between the Indian Subcontinent and Mesopotamian Cradle of Civilization</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Ancient DNA methodology was applied to analyse sequences extracted from freshly unearthed remains (teeth) of 4 individuals deeply deposited in slightly alkaline soil of the Tell Ashara (ancient Terqa) and Tell Masaikh (ancient Kar-Assurnasirpal) Syrian archaeological sites, both in the middle Euphrates valley. Dated to the <span class="hlt">period</span> between 2.5 Kyrs BC and 0.5 Kyrs AD the studied individuals carried mtDNA haplotypes corresponding to the M4b1, M49 and/or M61 haplogroups, which are believed to have arisen in the area of the Indian subcontinent during the Upper Paleolithic and are absent in people living today in Syria. However, they are present in people inhabiting today’s Tibet, Himalayas, India and Pakistan. We anticipate that the analysed remains from Mesopotamia belonged to people with genetic affinity to the Indian subcontinent since the distribution of identified ancient haplotypes indicates solid link with populations from the region of South Asia-Tibet (Trans-Himalaya). They may have been descendants of migrants from much earlier times, spreading the clades of the macrohaplogroup M throughout Eurasia and founding regional Mesopotamian groups like that of Terqa or just merchants moving along trade routes passing near or through the region. None of the successfully identified nuclear alleles turned out to be ?F508 CFTR, LCT-13910T or ?32 CCR5. PMID:24040024</p> <div class="credits"> <p class="dwt_author">Witas, Henryk W.; Tomczyk, Jacek; J?drychowska-Da?ska, Krystyna; Chaubey, Gyaneshwer; P?oszaj, Tomasz</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">95</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015AAS...22534520A"> <span id="translatedtitle">A Bayesian Estimation for Spica's Apsidal <span class="hlt">Period</span> from 111 years of Spectroscopic <span class="hlt">Observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Toward the goal of constraining the short <span class="hlt">period</span> (P = 4.01 d) massive binary star Spica's apsidal constant, which in turn constrains the internal structure of the primary star (B1.5 IV), we have modified the Bayesian Markov Chain Monte Carlo code EXOFAST (Eastman et al. 2013) to fit six radial velocity (RV) data sets obtained between 1889 to 2000. The code was modified to take radial velocity input from two stars rather than a single exoplanet host star. In addition the apsidal <span class="hlt">period</span> (U) and the RV amplitude of the secondary star (K2) have been added as fit parameters, and the longitude of periastron is now a function of time. Measurements from Vogel (1889), Baker (1910), Struve & Ebigghausen (1934), Struve et al. (1958), Shobbrook et al. (1972) and Riddle (2000) provide 338 and 239 RV measurements for the primary and secondary stars respectively.Preliminary results yield: (1) a median apsidal <span class="hlt">period</span> (U) of 118.9±1.3 years with 68% confidence consistent with the value of Herbison-Evans et al. (1971), 124±11 years. The ratio of the orbital <span class="hlt">period</span> to the apsidal <span class="hlt">period</span> (P/U), one of three parameters needed for <span class="hlt">observationally</span> determined apsidal-motion constant k2obs (Claret & Willems 2002), is now tentatively constrained to 1%, P/U = 9.24±0.01x10-5. (2) The eccentricity is constrained in our solution with an uncertainty of 9%, down from an uncertainly of 20% found by Riddle (2000). (3) The uncertainty in k2obs is dominated by the uncertainty of the ratio of the primary star radius, R1,to the semi-major axis, a, since k2obs is proportional to (R1/a)5. The semi-major axis can be found from a?sini which is constrained with an uncertainty of 3%, similar to previous work. The influence of the prior values on the posterior distributions will be described. The next step is to constrain the inclination from the light curve and long-baseline near-IR interferometry.</p> <div class="credits"> <p class="dwt_author">Aufdenberg, Jason P.; Robinette, Timothy M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">96</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2003A%26A...400..623K"> <span id="translatedtitle">Spectroscopic and photometric <span class="hlt">observations</span> of the short-<span class="hlt">period</span> RS CVn-type star CG Cyg</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Spectroscopic <span class="hlt">observations</span> around the Halpha line and BVR photometry of the eclipsing short-<span class="hlt">period</span> RS CVn-star CG Cyg are presented. The solutions of the radial velocity curves and the light curves yielded the following masses and radii of the star components: M1=0.97 Msun, M2=0.80 Msun, R1=1.00 Rsun, R2=0.83 Rsun. The measured rotational broadenings of the <span class="hlt">observed</span> lines correspond to equatorial velocities V1=80 km s-1 and V2=66 km s-1. The distortions of our multicolor light curve were reproduced by two cool spots on the primary star. The strong absorption feature between the spectral lines of the two stars was explained by extended structure around the mass center of the system. The Halpha emission line of the secondary star in the August spectra was attributed to a prolonged flare of this star. Based on spectral <span class="hlt">observations</span> at the 2-m Rozhen telescope, operated by the National Astronomical Observatory; the research was supported in part by grants of project No. 1/2002 of Shoumen University.</p> <div class="credits"> <p class="dwt_author">Kjurkchieva, D. P.; Marchev, D. V.; Ogloza, W.</p> <p class="dwt_publisher"></p> <p class="publishDate">2003-03-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">97</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19900064186&hterms=sundial&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dsundial"> <span id="translatedtitle">Latitudinal variation of perturbation electric fields during magnetically disturbed <span class="hlt">periods</span> - 1986 Sundial <span class="hlt">observations</span> and model results</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">F-region incoherent scatter radar drift <span class="hlt">observations</span> from Millstone Hill and Jicamarca, h-prime F <span class="hlt">observations</span> from Huancayo, and high latitude ground-magnetometer measurements taken during the Sundial 1986 campaign are used to study the relationship between plasmaspheric electric field perturbations and high latitude currents during disturbed <span class="hlt">periods</span>. The <span class="hlt">observations</span> are in good agreement with numerical results from a Rice Covection Model run that involved a sharp increase in the polar cap potential drop followed by a subsequent decrease. The zonal disturbance electric field pattern is latitude independent, and the corresponding amplitudes change approximately as L exp n (where n is about 1.5). The meridional electric field patterns and amplitudes have larger latitudinal variations. The mid-, low, and equatorial electric fields from the Rice Convection Model are in good agreement with previous results from the semianalytic, Senior-Blanc (1987) model. Also discussed are three physical mechanisms (over-shielding, fossil winds, and magnetic reconfiguration) that contribute to the long lasting (1-2 h) equatorial zonal electric field perturbations associated with a sudden northward turning of the IMF. It is predicted that the penetration of high latitude electric fields to low latitudes should, in general, be closely related to the rate of motion of the shielding layer and the equatorward edge of the diffuse aurora.</p> <div class="credits"> <p class="dwt_author">Fejer, B. G.; Spiro, R. W.; Wolf, R. A.; Foster, J. C.</p> <p class="dwt_publisher"></p> <p class="publishDate">1990-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">98</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19890006111&hterms=burnett&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D90%26Ntt%3Dburnett"> <span id="translatedtitle"><span class="hlt">Periodic</span> behaviors in the <span class="hlt">observed</span> vertical column abundances of atmospheric hydroxyl</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The data base for the vertical column abundance of atmospheric hydroxyl (OH) for Fritz Peak Observatory, Colorado (40 N, 105 W), now extends from 1976 through 1988 and is composed of 8849 independent data sets, averaging about 15 percent uncertainty and 20-minute time resolution each. The dominant solar zenith angle (chi) dependence of the OH abundance is characterized by an empirical curve, N(88), which has been updated from N(82) to include all valid data from 1980 through 1988. The chi-dependence of the OH abundance has been, to a first order, removed from the data base by a normalization procedure in which each data point is divided by the N(88,AM) value for the corresponding solar zenith angle. The resulting normalized OH values may then be examined for other systematic effects, particularly for <span class="hlt">periodic</span> variations. <span class="hlt">Observations</span> have also been made at Boca Raton, Florida (26 N, 80 W) and at Truk, Federated States of Micronesia (7 N, 152 E). These data bases are much less extensive and, as such, are less amenable to analysis for <span class="hlt">periodic</span> behaviors. Some comparisons with the Colorado data may be made, however.</p> <div class="credits"> <p class="dwt_author">Burnett, Elizabeth Beaver; Burnett, Clyde R.; Minschwaner, Kenneth R.</p> <p class="dwt_publisher"></p> <p class="publishDate">1989-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">99</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/0803.2104v1"> <span id="translatedtitle">Estimating the birth <span class="hlt">period</span> of pulsars through GLAST/LAT <span class="hlt">observations</span> of their wind nebulae</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">In this paper we show that the high energy $\\gamma$-ray flux in the GeV domain from mature pulsar wind nebulae (PWN) scales as the change in rotational kinetic energy $I(\\Omega_0^2-\\Omega^2)/2$ since birth, rather than the present day spindown power $I\\Omega\\dot{\\Omega}$. This finding holds as long as the lifetime of inverse Compton emitting electrons exceeds the age of the system. For a typical $\\gamma^{-2}$ electron spectrum, the predicted flux depends mostly on the pulsar birth <span class="hlt">period</span>, conversion efficiency of spindown power to relativistic electrons and distance to the PWN, so that first order estimates of the birth <span class="hlt">period</span> can be assessed from {\\it GLAST/LAT} <span class="hlt">observations</span> of PWN. For this purpose we derive an analytical expression. The associated (``uncooled'') photon spectral index in the GeV domain is expected to cluster around $\\sim 1.5$, which is bounded at low energies by an intrinsic spectral break, and at higher energies by a second spectral break where the photon index steepens to $\\sim 2$ due to radiation losses. Mature PWN are expected to have expanded to sizes larger than currently known PWN, resulting in relatively low magnetic energy densities and hence survival of GeV inverse Compton emitting electrons. Whereas such a PWN may be radio and X-ray quiet in synchrotron radiation, it may still be detectable as a {\\it GLAST/LAT} source as a result of the relic electrons in the PWN.</p> <div class="credits"> <p class="dwt_author">O. C. de Jager</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-03-14</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">100</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013AnGeo..31.1279D"> <span id="translatedtitle">Quasi-16-day <span class="hlt">period</span> oscillations <span class="hlt">observed</span> in middle atmospheric ozone and temperature in Antarctica</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Nightly averaged mesospheric temperature derived from the hydroxyl nightglow at Rothera station (67°34' S, 68°08' W) and nightly midnight measurements of ozone mixing ratio obtained from Troll station (72°01' S, 2°32' E) in Antarctica have been used to investigate the presence and vertical profile of the quasi-16-day planetary wave in the stratosphere and mesosphere during the Antarctic winter of 2009. The variations caused by planetary waves on the ozone mixing ratio and temperature are discussed, and spectral and cross-correlation analyses are performed to extract the wave amplitudes and to examine the vertical structure of the wave from 34 to 80 km. The results show that while planetary-wave signatures with <span class="hlt">periods</span> 3-12 days are strong below the stratopause, the oscillations associated with the 16-day wave are the strongest and present in both the mesosphere and stratosphere. The <span class="hlt">period</span> of the wave is found to increase below 42 km due to the Doppler shifting by the strong eastward zonal wind. The 16-day oscillation in the temperature is found to be correlated and phase coherent with the corresponding oscillation <span class="hlt">observed</span> in O3 volume mixing ratio at all levels, and the wave is found to have vertical phase fronts consistent with a normal mode structure.</p> <div class="credits"> <p class="dwt_author">Demissie, T. D.; Kleinknecht, N. H.; Hibbins, R. E.; Espy, P. J.; Straub, C.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-07-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_4");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' 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src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_5");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' href="#">4</a> <a onClick='return showDiv("page_5");' href="#">5</a> <a style="font-weight: bold;">6</a> <a onClick='return showDiv("page_7");' href="#">7</a> <a onClick='return showDiv("page_8");' href="#">8</a> <a onClick='return showDiv("page_9");' href="#">9</a> <a onClick='return showDiv("page_10");' href="#">10</a> <a onClick='return showDiv("page_11");' href="#">11</a> <a onClick='return showDiv("page_12");' href="#">12</a> <a onClick='return showDiv("page_13");' href="#">13</a> <a onClick='return showDiv("page_14");' href="#">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a onClick='return showDiv("page_16");' href="#">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a onClick='return showDiv("page_21");' href="#">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_7");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">101</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011ECSS...95..307D"> <span id="translatedtitle">Short <span class="hlt">period</span> sea level oscillations at Strait of Gibraltar: <span class="hlt">Observations</span> versus model results</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Tide gauge records from different ports of the Strait of Gibraltar area show events of short <span class="hlt">period</span> oscillations (minutes to tens of minutes) that persist for several days although its charactestic duration is of the order of a day. These events are <span class="hlt">observed</span> throughout the year although, when characterized by variables that account for their amplitude and duration simultaneously, they are biased toward summer months. The frequencies of these oscillations, which accumulate energy within bands centered at 7.5, 12, 19, 25 min -1, are characteristic of each port, with Tarifa showing a more selective tuning than Ceuta or Algeciras. The numerical model developed to investigate these oscillations confirms that they correspond to harbor resonance excited at the mouth of the port by oscillations in the Strait.</p> <div class="credits"> <p class="dwt_author">Delgado, J.; García-Lafuente, J.; Bruque-Pozas, E.; Naranjo, C.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">102</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25577455"> <span id="translatedtitle">Chondrosarcoma of the Temporomandibular Disc: Behavior Over a 28-Year <span class="hlt">Observation</span> <span class="hlt">Period</span>.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Chondrosarcoma of the head and neck occurs infrequently, with a recorded prevalence of only 5 to 12% of all such tumors; this in total represents only 17 to 22% of all monostotic bone malignancies. Chondrosarcomas arising in the region of the temporomandibular joint are especially rare, with only 28-including subsets-recorded in the 6 decades since the first report in 1954. The lesion described in the present report would appear to be the first arising solely from the disc itself, and the postoperative <span class="hlt">period</span> of <span class="hlt">observation</span> is the longest on record. The patient's course over 27 years shows the need for ongoing vigilance in the management of this tumor. PMID:25577455</p> <div class="credits"> <p class="dwt_author">MacIntosh, Robert B; Khan, Faisal; Waligora, Bret M</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-03-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">103</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/6097271"> <span id="translatedtitle">Cancer incidence among asbestos-exposed chemical industry workers: An extended <span class="hlt">observation</span> <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">A previous study on the incidence of cancer in a cohort of 286 asbestos-exposed electrochemical industry workers <span class="hlt">observed</span> from 1953 through 1980 has been extended with another 8 years of follow-up. The incidence of cancer was derived from the Cancer Registry of Norway, and the expected figures were calculated by a life table method. During the extended follow-up <span class="hlt">period</span> from 1981 through 1988, among the cohort members there were 12 new cancer cases versus 14.2 expected (SIR 85, 95% CI 44-158). In a lightly exposed sub-cohort, the extended follow-up revealed 4 cases of lung cancer or pleural mesothelioma (ICD, 7th revision 162-163) versus 1.6 cases expected (SIR 256, 95% CI71-654). In a heavily exposed sub-cohort, the corresponding figures were 3 and 0.5 (SIR 588, 95% CI 118-1,725).</p> <div class="credits"> <p class="dwt_author">Hilt, B.; Andersen, A.; Rosenberg, J.; Langard, S. (Department of Occupational Medicine, Telemark Sentralsjukehus, Porsgrunn (Norway))</p> <p class="dwt_publisher"></p> <p class="publishDate">1991-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">104</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/astro-ph/0401498v1"> <span id="translatedtitle">XMM-Newton EPIC & OM <span class="hlt">observations</span> of Her X-1 over the 35 day beat <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We present the results of a series of XMM-Newton EPIC and OM <span class="hlt">observations</span> of Her X-1, spread over a wide range of the 35 day precession <span class="hlt">period</span>. We confirm that the spin modulation of the neutron star is weak or absent in the low state - in marked contrast to the main or short-on states. During the states of higher intensity, we <span class="hlt">observe</span> a substructure in the broad soft X-ray modulation below ~1keV, revealing the presence of separate peaks which reflect the structure seen at higher energies. The strong fluorescence emission line at ~6.4keV is detected in all <span class="hlt">observations</span> (apart from one taken in the middle of eclipse), with higher line energy, width and normalisation during the main-on state. In addition, we report the detection of a second line near 7keV in 10 of the 15 <span class="hlt">observations</span> taken during the low-intensity states of the system. This feature is rather weak and not significantly detected during the main-on state, when the strong continuum emission dominates the X-ray spectrum. Spin resolved spectroscopy just after the rise to the main-on state shows that the variation of the Fe Kalpha line at 6.4 keV is correlated with the soft X-ray emission. This confirms our past finding based on the XMM-Newton <span class="hlt">observations</span> made further into the main-on state, and indicates the common origin for the thermal component and the Fe Kalpha line detected at these phases. We also find that the normalisation of the 6.4keV line during the low state is correlated with the binary orbital phase, having a broad maximum centered near phi_(orbit) ~ 0.5. We discuss these <span class="hlt">observations</span> in the context of previous <span class="hlt">observations</span>, investigate the origin of the soft and hard X-rays and consider the emission site of the 6.4keV and 7keV emission lines.</p> <div class="credits"> <p class="dwt_author">Silvia Zane; Gavin Ramsay; Mario A. Jimenez-Garate; Jan Willem den Herder; Charles J. Hailey</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-23</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">105</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011Icar..212..167P"> <span id="translatedtitle">Rotation <span class="hlt">periods</span> of binary asteroids with large separations - Confronting the Escaping Ejecta Binaries model with <span class="hlt">observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Durda et al. (Durda, D.D., Bottke, W.F., Enke, B.L., Merline, W.J., Asphaug, E., Richardson, D.C., Leinhardt, Z.M. [2004]. Icarus 170, 243-257), using numerical models, <span class="hlt">suggested</span> that binary asteroids with large separation, called Escaping Ejecta Binaries (EEBs), can be created by fragments ejected from a disruptive impact event. It is thought that six binary asteroids recently discovered might be EEBs because of the high separation between their components (?100 > a/Rp > ?20). However, the rotation <span class="hlt">periods</span> of four out of the six objects measured by our group and others and presented here show that these suspected EEBs have fast rotation rates of 2.5-4 h. Because of the small size of the components of these binary asteroids, linked with this fast spinning, we conclude that the rotational-fission mechanism, which is a result of the thermal YORP effect, is the most likely formation scenario. Moreover, scaling the YORP effect for these objects shows that its timescale is shorter than the estimated ages of the three relevant Hirayama families hosting these binary asteroids. Therefore, only the largest (D ? 19 km) suspected asteroid, (317) Roxane, could be, in fact, the only known EEB. In addition, our results confirm the triple nature of (3749) Balam by measuring mutual events on its lightcurve that match the orbital <span class="hlt">period</span> of a nearby satellite in addition to its distant companion. Measurements of (1509) Esclangona at different apparitions show a unique shape of the lightcurve that might be explained by color variations.</p> <div class="credits"> <p class="dwt_author">Polishook, D.; Brosch, N.; Prialnik, D.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">106</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013GeoRL..40.5581N"> <span id="translatedtitle">Concentric waves and short-<span class="hlt">period</span> oscillations <span class="hlt">observed</span> in the ionosphere after the 2013 Moore EF5 tornado</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We detected clear concentric waves and short-<span class="hlt">period</span> oscillations in the ionosphere after an Enhanced Fujita scale (EF)5 tornado hit Moore, Oklahoma, U.S., on 20 May 2013 using dense wide-coverage ionospheric total electron content (TEC) <span class="hlt">observations</span> in North America. These concentric waves were nondispersive, with a horizontal wavelength of ~120 km and a <span class="hlt">period</span> of ~13 min. They were <span class="hlt">observed</span> for more than 7 h throughout North America. TEC oscillations with a <span class="hlt">period</span> of ~4 min were also <span class="hlt">observed</span> to the south of Moore for more than 8 h. A comparison between the TEC <span class="hlt">observations</span> and infrared cloud image from the GOES satellite indicates that the concentric waves and short-<span class="hlt">period</span> oscillations are caused by supercell-induced atmospheric gravity waves and acoustic resonances, respectively. This <span class="hlt">observational</span> result provides the first clear evidence of a severe meteorological event causing atmospheric waves propagating upward in the upper atmosphere and reaching the ionosphere.</p> <div class="credits"> <p class="dwt_author">Nishioka, Michi; Tsugawa, Takuya; Kubota, Minoru; Ishii, Mamoru</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-11-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">107</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22311189"> <span id="translatedtitle"><span class="hlt">Observation</span> of atomic ordering of triple-<span class="hlt">period</span>-A and -B type in GaAsBi</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We report the <span class="hlt">observation</span> of atomic ordering of triple-<span class="hlt">period</span> (TP)-A and -B type in low temperature (LT) grown GaAsBi alloy using transmission electron microscopy (TEM). In addition to previous reports, where only TP-A ordering was identified in III-V alloys, here, we confirm by electron diffraction, high-resolution (HR) TEM, and HR Z-contrast scanning TEM that two ordering variants coexists for LT-GaAsBi. We find that the TP-A ordering variant dominates over the TP-B variant. TP-A domains extend over 50–100?nm (projected lateral width) and are of higher perfection compared to TP-B domains. HR Z-contrast scanning TEM on different domains reveals a variation in the Bi occupancy in the (111) planes with triple <span class="hlt">period</span> sequence. Since the formation of ordered phases has been directly linked to the occurrence of specific surface reconstructions, our results <span class="hlt">suggest</span> a correlation between the TP-A and B type domains and the multiple stability of n?×?3 and 3?×?n reconstructions on the (001) surface of GaAsBi under low temperature growth.</p> <div class="credits"> <p class="dwt_author">Wu, Mingjian, E-mail: mingjian@pdi-berlin.de; Luna, Esperanza; Trampert, Achim [Paul-Drude-Institut für Festkörperelektronik, Hausvogteiplatz 5–7, D-10117 Berlin (Germany); Puustinen, Janne; Guina, Mircea [Optoelectronics Research Centre, Tampere University of Technology, P.O. Box 692, FI-33101 Tampere (Finland)</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-07-28</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">108</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19950045560&hterms=flapping+tail&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dflapping%2Btail"> <span id="translatedtitle">Irregular, long-<span class="hlt">period</span> boundary oscillations beyond approximately 100 R(sub e): GEOTAIL plasma <span class="hlt">observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Near the tail boundary beyond about 100 Re, GEOTAIL often measures irregular, long-<span class="hlt">period</span> oscillations in plasma velocity and density. Flow speed and density oscillate between magnetosheath values and values an order of magnitude less. The oscillations can persist for days. A typical oscillation lasts 100 minutes, but the range is large. The oscillations are highly asymmetric in that the increasing phase of the oscillation is an order of magnitude faster than the decreasing phase. This asymmetry shows that they are a distinct class of oscillations, not previously explicitly reported, and that they are not mere consequences of tail flapping in a variable solar wind. The changes in flow direction through an oscillation imply that the oscillation results from a motion of the boundary toward and away from the spacecraft with an amplitude between 5 and 10 R(sub e). A consideration of options <span class="hlt">suggests</span> that the most plausible cause of these oscillations is the 'breathing' of the magnetotail that attends the substorm cycle.</p> <div class="credits"> <p class="dwt_author">Siscoe, G. L.; Frank, L. A.; Ackerson, K. L.; Paterson, W. R.</p> <p class="dwt_publisher"></p> <p class="publishDate">1994-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">109</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013JASTP.105....1E"> <span id="translatedtitle">Short <span class="hlt">period</span> gravity wave momentum fluxes <span class="hlt">observed</span> in the tropical troposphere, stratosphere and mesosphere</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Using long-term data (1998-2008) collected from mesosphere-stratosphere-troposphere (MST) radar and Rayleigh Lidar located at a tropical station, Gadanki (13.5°N, 79.2°E), India, vertical flux of the momentum from troposphere to mesosphere associated with the gravity waves of <span class="hlt">periods</span> in the range 20 min to 2 h is investigated for the first time. The emphasis is on seasonal variability of mean zonal and meridional momentum fluxes in mesosphere and troposphere and vertical flux of horizontal momentum in the stratosphere. At tropospheric altitudes of 11-16 km large enhancement in flux is noticed during equinoxes. In the lower mesosphere in the altitude region 58-62 km the maximum values of flux (?2.8 m2/s2) <span class="hlt">observed</span> are pragmatic in winter and spring. Interestingly, the vertical flux of horizontal momentum estimated from lidar is in the range of those estimated from radar data in the overlap altitude region, though the estimates are from two different techniques. In the mesosphere, large variations with altitude in zonal momentum flux are noticed with a magnitude ?0-4 m2/s2 in summer. In winter and summer the zonal wind direction is opposite to the momentum flux direction between 73 and 80 km and in equinoxes zonal wind follows the momentum flux. The meridional fluxes in the mesosphere are higher in equinoxes (?10-12 m2/s2).</p> <div class="credits"> <p class="dwt_author">Eswaraiah, S.; Ratnam, M. Venkat; Murthy, B. V. Krishna; Guharay, A.; Rao, S. Vijaya Bhaskara</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">110</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/astro-ph/0606127v2"> <span id="translatedtitle">Testing the Disk Regulation Paradigm with Spitzer <span class="hlt">Observations</span>. I. Rotation <span class="hlt">Periods</span> of Pre-main Sequence Stars in the IC 348 Cluster</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We present 75 new stellar rotation <span class="hlt">periods</span> in the young cluster IC348. Stars estimated to be less massive than 0.25 Mo show a unimodal distribution with a peak at P ~1-2 d) and a tail of slower rotators, while stars estimated to be more massive than 0.2 Mo show a bimodal distribution with peaks at ~2 and ~8 d. We combine all published rotation <span class="hlt">periods</span> in IC348 with Spitzer/IRAC photometry in order to test the disk-braking paradigm. We find no evidence that the tail of slow rotators in low-mass stars or the long <span class="hlt">period</span> peak in high-mass stars are preferentially populated by objects with disks as might be expected based on the current disk-braking model. Also, we find no significant correlation between <span class="hlt">period</span> and the magnitude of the IR-excess, regardless of the mass range considered. Our results do not support a strong correlation in this cluster between rotation <span class="hlt">period</span> and the presence of a disk as predicted by disk-braking theory. Rather, they are consistent with the <span class="hlt">suggestion</span> that the correlation between <span class="hlt">period</span> and the amplitude of the (I-K) excess reported in the past is a secondary manifestation of the correlation between the amplitude of near-IR excess and mass. Finally, we find some indication that the disk fraction decreases significantly for stars with very short <span class="hlt">periods</span> (P disk braking. It has been proposed that the <span class="hlt">observational</span> signatures of disk braking might be significantly masked by the intrinsic breadth of the initial <span class="hlt">period</span> distribution. We argue that more rigorous modeling of angular momentum evolution and a quantitative analysis of the <span class="hlt">observational</span> data are required before the disk-braking model can be regarded as inconsistent with <span class="hlt">observations</span>.</p> <div class="credits"> <p class="dwt_author">Lucas Cieza; Nairn Baliber</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-07-07</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">111</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/19256359"> <span id="translatedtitle">[<span class="hlt">Observational</span> study of black carbon aerosol during straw-burning <span class="hlt">period</span>].</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Black carbon aerosol (BC) has been measured at three sites in Hefei City during May and June, 2007. Analyzing these real-time BC data, the concentration characters and the sources of black carbon aerosol can be found. The average concentrations of BC in normal <span class="hlt">period</span> and straw-burning <span class="hlt">period</span> are 4.85 microg/m3 and 8.38 microg/m3, respectively. The significant difference shows that the straw-burning is one of the main sources. The correlation coefficients between daily average concentration of BC and PM10 is 0.74, while the values of BC/PM10 in normal <span class="hlt">period</span> and straw-burning <span class="hlt">period</span> are 4.7% and 7.9%, respectively. Through comparing to the BC concentration during straw-burning <span class="hlt">period</span> in 2004, the results indicated that pollution of BC has reduced after straw-burning was forbidden by the government. PMID:19256359</p> <div class="credits"> <p class="dwt_author">Wu, De-xia; Wei, Qing-nong; Wei, Jian-li; Liu, Shi-sheng; Feng, Wei-wei</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">112</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://pubs.er.usgs.gov/publication/70017592"> <span id="translatedtitle">Diurnal-<span class="hlt">period</span> currents trapped above Fieberling Guyot: <span class="hlt">observed</span> characteristics and model comparisons</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p class="result-summary">Current measurements at depths of 19, 115, 264 and 464 m above the summit of Fieberling Guyot (32??28???N, 127??47???W) for 13 months in 1989 show that the diurnal tides are strongly amplified. The measured variances for K1, P1 and O1 at the 115 m depth were 810, 140 and 80 times larger than the variances of the respective estimated barotropic tides. The diurnal currents closer to the summit were also strongly amplified, through the variance ratios were 40-50% of the ratios <span class="hlt">observed</span> at 115 m. The diurnal band currents were only amplified at the precise tidal frequencies; the bandwidth of the response was less than 0.0002 cph. The discrete character of the response <span class="hlt">suggests</span> that only currents with large spatial scales will be amplified. The characteristics of the amplified diurnal currents are compared to those predicted by a model for Fieberling Guyot of seamount-trapped waves driven by the barotropic tide. The amplitudes of the responses at this one site on the seamount compare favourably to the predicted. ?? 1994.</p> <div class="credits"> <p class="dwt_author">Noble, M.A.; Brink, K.H.; Eriksen, C.C.</p> <p class="dwt_publisher"></p> <p class="publishDate">1994-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">113</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20040088493&hterms=fat+wang&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dfat%2Bwang"> <span id="translatedtitle">Entrainment in solution of an oscillating NADH oxidase activity from the bovine milk fat globule membrane with a temperature-compensated <span class="hlt">period</span> length <span class="hlt">suggestive</span> of an ultradian time-keeping (clock) function</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Entrainment in solution of an oscillating activity with a temperature compensated <span class="hlt">period</span> of 24 min is described for a NADH oxidase (NOX) activity of the bovine milk fat globule membrane, a derivative of the mammary epithelial cell plasma membrane. The <span class="hlt">period</span> of 24 min remained unchanged at 17 degrees C, 27 degrees C and 37 degrees C whereas the amplitude approximately doubled with each 10 degree C rise in temperature (Q(10)congruent with 2). The <span class="hlt">periodicity</span> was <span class="hlt">observed</span> with both intact milk fat globule membranes and with detergent-solubilized membranes, demonstrating that the oscillations did not require an association with membranes. The <span class="hlt">periodicity</span> was not the result of instrument variation or of chemical interactions among reactants in solution. Preparations with different <span class="hlt">periodicities</span> entrained (autosynchronized) when mixed. Upon mixing, the preparations exhibited two oscillatory patterns but eventually a single pattern representing the mean of the farthest separated maxima of the two preparations analyzed separately emerged. The cell surface NOX protein is the first reported example of an entrainable biochemical entity with a temperature-compensated <span class="hlt">periodicity</span> potentially capable of functioning as an ultradian or circadian clock driver.</p> <div class="credits"> <p class="dwt_author">Morre, D. James; Lawler, Juliana; Wang, Sui; Keenan, Thomas W.; Morre, Dorothy M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">114</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/44725400"> <span id="translatedtitle">Some <span class="hlt">Observations</span> on the Greek Military in the Inter-War <span class="hlt">Period</span>, 1918-1935</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">This article provides a historical description of the Greek military in the inter-war <span class="hlt">period</span> (1918-1935), focusing on the self-image and professionalism of the officer corps as well as the civil-military relations of the <span class="hlt">period</span>. The Greek military represented an institution different than other European nations, whose armed forces often grew out of an ancien regime or represented citizen armies like</p> <div class="credits"> <p class="dwt_author">Thanos Veremis</p> <p class="dwt_publisher"></p> <p class="publishDate">1978-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">115</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014A%26A...569A..12N"> <span id="translatedtitle"><span class="hlt">Observation</span> of a high-quality quasi-<span class="hlt">periodic</span> rapidly propagating wave train using SDO/AIA</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Context. We present a new event of quasi-<span class="hlt">periodic</span> wave trains <span class="hlt">observed</span> in EUV wavebands that rapidly propagate away from an active region after a flare. Aims: We measured the parameters of a wave train <span class="hlt">observed</span> on 7 December 2013 after an M1.2 flare, such as the phase speeds, <span class="hlt">periods</span> and wavelengths, in relationship to the local coronal environment and the energy sources. Methods: We compared our <span class="hlt">observations</span> with a numerical simulation of fast magnetoacoustic waves that undergo dispersive evolution and leakage in a coronal loop embedded in a potential magnetic field. Results: The wave train is <span class="hlt">observed</span> to propagate as several arc-shaped intensity disturbances for almost half an hour, with a speed greater than 1000 km s-1 and a <span class="hlt">period</span> of about 1 min. The wave train followed two different patterns of propagation, in accordance with the magnetic structure of the active region. The oscillatory signal is found to be of high-quality, i.e. there is a large number (10 or more) of subsequent wave fronts <span class="hlt">observed</span>. The <span class="hlt">observations</span> are found to be consistent with the numerical simulation of a fast wave train generated by a localised impulsive energy release. Conclusions: Transverse structuring in the corona can efficiently create and guide high-quality quasi-<span class="hlt">periodic</span> propagating fast wave trains. The movies are available in electronic form at http://www.aanda.org</p> <div class="credits"> <p class="dwt_author">Nisticò, G.; Pascoe, D. J.; Nakariakov, V. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-09-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">116</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19760020565&hterms=Periodic+table&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D90%26Ntt%3D%2528Periodic%2Btable%2529"> <span id="translatedtitle">Quantization and symmetry in <span class="hlt">periodic</span> coverage patterns with applications to earth <span class="hlt">observation</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Analytical approaches based on an idealized physical model and concepts from number theory show that in <span class="hlt">periodic</span> coverage patterns, uniquely defined by their revolution numbers R (orbital) and N (rotational), the subnodal points are earth-fixed, and they divide the equator into R equal segments of length s. The ascending subsatellite trace crosses each point once (only) each <span class="hlt">period</span>. The descending subnodal points coincide with the ascending points if the integers N and R have like parity, and bisect the intervals between them if opposite. The interval between consecutive unidirectional crossings is Ns. Symmetries extend the equatorial results to all parallels of latitude. Complete <span class="hlt">periodic</span> patterns of traces exhibit an overall symmetry, with trace intersections confined to discrete coordinate values which are quantized in longitude (basic s-unit) and symmetric in latitude.</p> <div class="credits"> <p class="dwt_author">King, J. C.</p> <p class="dwt_publisher"></p> <p class="publishDate">1975-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">117</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/0809.1753v1"> <span id="translatedtitle">Orbital <span class="hlt">periods</span> of cataclysmic variables identified by the SDSS. V. VLT, NTT and Magellan <span class="hlt">observations</span> of nine equatorial systems</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We present VLT and Magellan spectroscopy and NTT photometry of nine faint cataclysmic variables (CVs) which were spectroscopically identified by the SDSS. We measure orbital <span class="hlt">periods</span> for five of these from the velocity variations of the cores and wings of their Halpha emission lines. Four of the five have orbital <span class="hlt">periods</span> shorter than the 2-3 hour <span class="hlt">period</span> gap <span class="hlt">observed</span> in the known population of CVs. SDSS J004335.14-003729.8 has an orbital <span class="hlt">period</span> of Porb = 82.325 +/- 0.088 min; Doppler maps show emission from the accretion disc, bright spot and the irradiated inner face of the secondary star. In its light curve we find a <span class="hlt">periodicity</span> which may be attributable to pulsations of the white dwarf. SDSS J163722.21-001957.1 has Porb = 99.75 +/- 0.86 min. By combining this new measurement with a published superhump <span class="hlt">period</span> we estimate a mass ratio of 0.16 and infer the physical properties and orbital inclination of the system. For SDSS J164248.52+134751.4 we find Porb = 113.60 +/- 1.5 min. The Doppler map of this CV shows an unusual brightness distribution in the accretion disc which would benefit from further <span class="hlt">observations</span>. SDSS J165837.70+184727.4 had spectroscopic characteristics which were very different between the SDSS spectrum and our own VLT <span class="hlt">observations</span>, despite only a small change in brightness. We measure Porb = 98.012 +/- 0.065 min from its narrow Halpha emission line. Finally, SDSS J223843.84+010820.7 has a comparatively longer <span class="hlt">period</span> of Porb = 194.30 +/- 0.16 min. It contains a magnetic white dwarf and, with g = 18.15, is brighter than the other objects studied here. These results continue the trend for the fainter CVs identified by the SDSS to be almost exclusively shorter-<span class="hlt">period</span> objects with low mass transfer rates.</p> <div class="credits"> <p class="dwt_author">John Southworth; B T Gaensicke; T R Marsh; M A P Torres; D Steeghs; P Hakala; C M Copperwheat; A Aungwerojwit; A Mukadam</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-09-10</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">118</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/20329816"> <span id="translatedtitle"><span class="hlt">Observation</span> of energy cascade creating <span class="hlt">periodic</span> shock waves in a resonator.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Nonlinear excitation of <span class="hlt">periodic</span> shock waves in high-amplitude standing waves was studied from measurements of the acoustic intensity. A gas column of atmospheric air in a cylindrical resonator was driven sinusoidally by an oscillating piston at the fundamental resonance frequency. Acoustic pressure and axial acoustic particle velocity were simultaneously measured and decomposed into the Fourier components, from which the intensity associated with each of the oscillating modes in the resonator was determined. This letter reports the energy cascade from the driven mode to the second harmonic in the <span class="hlt">periodic</span> shock waves in the resonator. PMID:20329816</p> <div class="credits"> <p class="dwt_author">Biwa, Tetsushi; Yazaki, Taichi</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-03-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">119</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19930009964&hterms=Periodic+table&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3D%2528Periodic%2Btable%2529"> <span id="translatedtitle">IUE <span class="hlt">observations</span> of <span class="hlt">periodic</span> comets Tempel-2, Kopff, and Tempel-1</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">We summarize the results of <span class="hlt">observations</span> made between 10 Jun. - 18 Dec. 1988 with the International Ultraviolet Explorer (IUS) of comet P/Tempel-2 during its 1988 appearance. The derived water production rate and relative gas/dust ratio are compared with those of P/Halley, <span class="hlt">observed</span> with IUE in 1985-86, and other potential Comet Rendezvous/Asteroid Flyby (CRAF) target comets, P/Kopff and P/Tempel-1, both <span class="hlt">observed</span> with IUE in 1983.</p> <div class="credits"> <p class="dwt_author">Feldman, Paul D.; Festou, Michel C.</p> <p class="dwt_publisher"></p> <p class="publishDate">1992-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">120</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.se.cuhk.edu.hk/~hfwang/PartialSupplyInfo.pdf"> <span id="translatedtitle">Optimal Inventory Decisions in the Multi-<span class="hlt">period</span> Newsvendor Problem with Partial-<span class="hlt">Observed</span> Markovian Supply Capacities</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">This paper considers a multi-<span class="hlt">period</span> news-vendor problem with partially <span class="hlt">observed</span> supply capacity information which evolves as a Markovian Process. The supply capacity is fully <span class="hlt">observed</span> by the buyer when the capacity is smaller than buyer's ordering quantity. With a dynamic programming formulation, we prove the existence of a unique optimal ordering policy. In a two-state Markovian capacity case, we further</p> <div class="credits"> <p class="dwt_author">Haifeng Wang; Houmin Yan</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_5");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' 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id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_6");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' href="#">4</a> <a onClick='return showDiv("page_5");' href="#">5</a> <a onClick='return showDiv("page_6");' href="#">6</a> <a style="font-weight: bold;">7</a> <a onClick='return showDiv("page_8");' href="#">8</a> <a onClick='return showDiv("page_9");' href="#">9</a> <a onClick='return showDiv("page_10");' href="#">10</a> <a onClick='return showDiv("page_11");' href="#">11</a> <a onClick='return showDiv("page_12");' href="#">12</a> <a onClick='return showDiv("page_13");' href="#">13</a> <a onClick='return showDiv("page_14");' href="#">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a onClick='return showDiv("page_16");' href="#">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a onClick='return showDiv("page_21");' href="#">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_8");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">121</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012SPIE.8696E..0JM"> <span id="translatedtitle">Aerosol disturbances of the stratosphere over Tomsk according to data of lidar <span class="hlt">observations</span> in volcanic activity <span class="hlt">period</span> 2006-2011</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We summarize and analyze the lidar measurements (Tomsk: 56.5°N; 85.0°E) of the optical characteristics of the stratospheric aerosol layer (SAL) in the volcanic activity <span class="hlt">period</span> 2006-2011. The background SAL state with minimal aerosol content, which was <span class="hlt">observed</span> since 1997 under the conditions of long-term volcanically quiescent <span class="hlt">period</span>, was interrupted in October 2006 by a series of explosive eruptions of volcanoes of the Pacific Ring of Fire: Rabaul (October 2006, New Guinea); Okmok and Kasatochi (July-August 2008, Aleutian Islands); Redoubt (March-April 2009, Alaska); Sarychev Peak (June 2009, Kuril Islands), and Grimsvötn (May 2011, Iceland). A short-term and minor disturbance of the lower stratosphere was also <span class="hlt">observed</span> in April 2010 after eruption of the Icelandic volcano Eyjafjallajokull. The developed regional empirical model of the vertical distribution of background SAL optical characteristics was used to identify the <span class="hlt">periods</span> of elevated stratospheric aerosol content after each of the volcanic eruptions.</p> <div class="credits"> <p class="dwt_author">Makeev, Andrey P.; Burlakov, Vladimir D.; Dolgii, Sergey I.; Nevzorov, Aleksey V.; Trifonov, Dimitar A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">122</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/4903431"> <span id="translatedtitle"><span class="hlt">Observation</span> of <span class="hlt">Periodic</span> Fine Structure in Reflectance from Biological Tissue: A New Technique for Measuring Nuclear Size Distribution</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">We report <span class="hlt">observation</span> of a fine structure component in backscattered light from mucosal tissue which is <span class="hlt">periodic</span> in wavelength. This structure is ordinarily masked by a diffusive background. We have identified the origin of this component as being due to light which is Mie scattered by surface epithelial cell nuclei. By analyzing the amplitude and frequency of the fine structure,</p> <div class="credits"> <p class="dwt_author">L. T. Perelman; V. Backman; M. Wallace; G. Zonios; R. Manoharan; A. Nusrat; S. Shields; M. Seiler; C. Lima; T. Hamano; I. Itzkan; J. Van Dam; J. M. Crawford; M. S. Feld</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">123</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/54820806"> <span id="translatedtitle">Non-linear dynamics of singular long-<span class="hlt">period</span> long-lasting volcanic earthquakes <span class="hlt">observed</span> at Mt. Asama</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">On September 1, 2004, a middle-scale eruption occurred at Mt. Asama. Before the eruption, we had <span class="hlt">observed</span> several kinds of singular events since October 2003. These singular events are classified into three types depending on these waveforms. The first type event (Type-1 event) has an impulsive ground velocity with a dominant <span class="hlt">period</span> up to 10 sec and outgoing initial motion</p> <div class="credits"> <p class="dwt_author">M. Takeo</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">124</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/42040533"> <span id="translatedtitle">Comparison of aerosol optical depth from four solar radiometers during the fall 1997 ARM Intensive <span class="hlt">Observation</span> <span class="hlt">Period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">In the Fall of 1997 the Atmospheric Radiation Measurement (ARM) program conducted an Intensive <span class="hlt">Observation</span> <span class="hlt">Period</span> (IOP) to study aerosols. Five sun-tracking radiometers were present to measure the total column aerosol optical depth. This comparison performed on the Southern Great Plains (SGP) demonstrates the capabilities and limitations of modern tracking sunphotometers at a location typical of where aerosol measurements are</p> <div class="credits"> <p class="dwt_author">B. Schmid; J. Michalsky; R. Halthore; M. Beauharnois; L. Harrison; J. Livingston; P. Russell; B. Holben; T. Eck; A. Smirnov</p> <p class="dwt_publisher"></p> <p class="publishDate">1999-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">125</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.agu.org/journals/ja/v086/iA12/JA086iA12p09989/JA086iA12p09989.pdf"> <span id="translatedtitle">ISEE 1 <span class="hlt">observations</span> of thermal plasma in the vicinity of the plasmasphere during <span class="hlt">periods</span> of quieting magnetic activity</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Thermal (< or approx. =100 electron volts) ion <span class="hlt">observations</span> made with the plasma composition experiment on ISEE 1 are combined with plasma density profiles obtained from plasma frequency measurements made with the plasma wave experiment to conduct an investigation of thermal plasma behavior in the vicinity of the plasmasphere during <span class="hlt">periods</span> of quieting magnetic activity. Normally, the principal thermal ion</p> <div class="credits"> <p class="dwt_author">J. L. Horwitz; C. R. Baugher; C. R. Chappell; E. G. Shelley; D. T. Young; R. R. Anderson</p> <p class="dwt_publisher"></p> <p class="publishDate">1981-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">126</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013EGUGA..15..475K"> <span id="translatedtitle"><span class="hlt">Observations</span> of quasi-inertial and short-<span class="hlt">period</span> internal waves from stationary platform in the Black Sea</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">It is well known that the major factor of the generation of the intensive internal waves on the shelves of the oceans and open seas is barotropic tide. Despite of the Black sea is closed and free-tidal sea nevertheless there are exist quite intense internal wave field in here. The results of long-term <span class="hlt">observations</span> of long- and short-<span class="hlt">period</span> internal waves measured in the Black Sea are analyzed. These studies were carried out from the stationary platform of the Marine Hydrophysical Institute of the National Academy of Sciences of Ukraine in the summer 2010 and 2011. The platform is situated on the Southern coast of Crimea in 600 m from the shore, where sea depth is about 30 m. The measurements were taken by acoustic Doppler current profilometer (ADCP) "Rio Grande 600 kHz", thermistor chain of ten sensors "Star-Oddi" and oceanographic mini profiler «MiniSVP» with measuring parameters of sound velocity and temperature. We <span class="hlt">observed</span> the well-defined temporal thermocline oscillations with <span class="hlt">period</span> close to local inertial (17.2 hours) <span class="hlt">period</span>. At the same time the clockwise rotation of the vector of currents with the inertial <span class="hlt">period</span> was detected. During the expedition in 2011 the whole water column synchronous oscillations of the first-mode were <span class="hlt">observed</span> for the first 5 days, which than changed into the second-mode oscillations. <span class="hlt">Observations</span> of 2011 were for conditions when thermocline was in the middle of water column. <span class="hlt">Observed</span> oscillations of inertial waves in 2010 were for conditions of bottom thermocline. The amplitudes of thermocline oscillations were up to 10 -12 m. Also intense short-<span class="hlt">period</span> waves with <span class="hlt">period</span> from 2 to 20 minutes and heights from 1 to 6 m were registered. Several cases of second mode short-<span class="hlt">period</span> internal waves were <span class="hlt">observed</span>. Also several passages of solitary internal waves were noticed. The peaks of inertial and high-frequency oscillations were revealed by the spectral analysis of current data and temperature records. This work was partly supported by the Russian Foundation for Basic Research.</p> <div class="credits"> <p class="dwt_author">Khymchenko, Ielizaveta; Serebryany, Andrey</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">127</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3417418"> <span id="translatedtitle">Small molecule chemokine mimetics <span class="hlt">suggest</span> a molecular basis for the <span class="hlt">observation</span> that CXCL10 and CXCL11 are allosteric ligands of CXCR3</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">BACKGROUND AND PURPOSE The chemokine receptor CXCR3 directs migration of T-cells in response to the ligands CXCL9/Mig, CXCL10/IP-10 and CXCL11/I-TAC. Both ligands and receptors are implicated in the pathogenesis of inflammatory disorders, including atherosclerosis and rheumatoid arthritis. Here, we describe the molecular mechanism by which two synthetic small molecule agonists activate CXCR3. EXPERIMENTAL APPROACH As both small molecules are basic, we hypothesized that they formed electrostatic interactions with acidic residues within CXCR3. Nine point mutants of CXCR3 were generated in which an acidic residue was mutated to its amide counterpart. Following transient expression, the ability of the constructs to bind and signal in response to natural and synthetic ligands was examined. KEY RESULTS The CXCR3 mutants D112N, D195N and E196Q were efficiently expressed and responsive in chemotaxis assays to CXCL11 but not to CXCL10 or to either of the synthetic agonists, confirmed with radioligand binding assays. Molecular modelling of both CXCL10 and CXCR3 <span class="hlt">suggests</span> that the small molecule agonists mimic a region of the ‘30s loop’ (residues 30–40 of CXCL10) which interacts with the intrahelical CXCR3 residue D112, leading to receptor activation. D195 and E196 are located in the second extracellular loop and form putative intramolecular salt bridges required for a CXCR3 conformation that recognizes CXCL10. In contrast, CXCL11 recognition by CXCR3 is largely independent of these residues. CONCLUSION AND IMPLICATIONS We provide here a molecular basis for the <span class="hlt">observation</span> that CXCL10 and CXCL11 are allosteric ligands of CXCR3. Such findings may have implications for the design of CXCR3 antagonists. LINKED ARTICLE This article is commented on by O'Boyle, pp. 895–897 of this issue. To view this commentary visit http://dx.doi.org/10.1111/j.1476-5381.2011.01759.x PMID:21895630</p> <div class="credits"> <p class="dwt_author">Nedjai, Belinda; Li, Hubert; Stroke, Ilana L; Wise, Emma L; Webb, Maria L; Merritt, J Robert; Henderson, Ian; Klon, Anthony E; Cole, Andrew G; Horuk, Richard; Vaidehi, Nagarajan; Pease, James E</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">128</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/1996PhRvL..76.3428P"> <span id="translatedtitle"><span class="hlt">Periodicity</span> of the Spin Structure <span class="hlt">Observed</span> in the Optical Response of CeBi Single Crystals</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We report a study of the optical conductivity of CeBi in different magnetic phases. Going from the paramagnetic phase to the various antiferromagnetic and ferrimagnetic phases, different new interband transitions appear below the absorption edge of the p-->d transitions. These new interband transitions disappear in a magnetic field that is sufficiently strong to align the spins parallel. The appearance of new interband transitions is indubitably associated with the folding of the Brillouin zone, which is a consequence of the change of the <span class="hlt">periodicity</span> of the spin structure.</p> <div class="credits"> <p class="dwt_author">Pittini, R.; Schoenes, J.; Hulliger, F.; Wachter, P.</p> <p class="dwt_publisher"></p> <p class="publishDate">1996-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">129</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.classzone.com/books/earth_science/terc/content/visualizations/es3006/es3006page01.cfm?chapter_no=visualization"> <span id="translatedtitle"><span class="hlt">Observe</span> an animation of an asteroid impact at the end of the Cretaceous <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">This Earth science animation shows middle and high school students how an asteroid that struck the Earth at the end of the Cretaceous <span class="hlt">period</span> may have caused a mass extinction that killed the dinosaurs. The introduction explains the basis of the asteroid theory of extinction. The animation depicts an artist's conception, presented from space, of an asteroid hitting the Gulf of Mexico and releasing a cloud that prevented sunlight from reaching the Earth. Movie controls allow students to repeat, pause, or step through the animation, which can give students more time to analyze the images. Copyright 2005 Eisenhower National Clearinghouse</p> <div class="credits"> <p class="dwt_author">TERC. Center for Earth and Space Science Education</p> <p class="dwt_publisher"></p> <p class="publishDate">2003-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">130</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2007AGUSM.G42A..06S"> <span id="translatedtitle">Short-<span class="hlt">period</span> Variations of the Earth Rotation Parameters <span class="hlt">Observed</span> by Very Long Baseline Interferometry</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">High-frequency polar motion and universal time variations are obtained from Very Long Baseline Interferometry (VLBI). The goal is to detect short-<span class="hlt">period</span> and episodic events with signatures below the 100 microarcseconds (7.5 microseconds) level. Ter-diurnal variations in the order of 40 microarcseconds in polar motion have been reported during the VLBI campaign CONT02, from October 16 to 31, 2002. But, no geophysical explanation with similar amplitudes was provided. To resolve this enigma, we re-processed the VLBI data obtained during the CONT96, CONT02, and CONT05 campaigns using identical an the most recent reduction models. Two independent software packages were used, OCCAM61E and CALC SOLVE, to assure robustness of the Earth rotation parameters (ERP) estimated with semi-hourly resolution over the fortnightly data sets. The long wavelength signal was removed by a smooth function from the final ERP. Jumps in the ERP values at session boundaries were identified. A heuristic and Fourier frequency analysis shows no significant ter-diurnal <span class="hlt">periods</span>. In addition, this high-frequency analysis allows to detect incorrect daily ERP values in the International Earth Rotation and reference Systems (IERS) C04 series.</p> <div class="credits"> <p class="dwt_author">Schuh, H.; Artz, T.; Nothnagel, A.; Mendes Cerveira, P. J.</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-05-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">131</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25253054"> <span id="translatedtitle">Influence of regional biomass burning on the highly elevated organic carbon concentrations <span class="hlt">observed</span> at Gosan, South Korea during a strong Asian dust <span class="hlt">period</span>.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">PM2.5 carbonaceous particles were measured at Gosan, South Korea during 29 March-11 April 2002 which includes a pollution <span class="hlt">period</span> (30 March-01 April) when the highest concentrations of major anthropogenic species (nss-SO4 (2-), NO3 (-), and NH4 (+)) were <span class="hlt">observed</span> and a strong Asian dust (AD) <span class="hlt">period</span> (08-10 April) when the highest concentrations of mainly dust-originated trace elements (Al, Ca, Mg, and Fe) were seen. The concentrations of elemental carbon (EC) measured in the pollution <span class="hlt">period</span> were higher than those measured in the strong AD <span class="hlt">period</span>, whereas an inverse variation in the concentrations of organic carbon (OC) was <span class="hlt">observed</span>. Based on the OC/EC ratios, the possible source that mainly contributed to the highly elevated OC concentrations measured in the strong AD <span class="hlt">period</span> was biomass burning. The influence of the long-range transport of smoke plumes emitted from regional biomass burning sources was evaluated by using MODIS (Moderate Resolution Imaging Spectroradiometer) satellite data for fire locations and the potential source contribution function analysis. The most potential source regions of biomass burning were the Primorsky and Amur regions in Far Eastern Russia and southeastern and southwestern Siberia, Russia. Further discussion on the source characteristics <span class="hlt">suggested</span> that the high OC concentrations measured in the strong AD <span class="hlt">period</span> were significantly affected by the smoldering phase of biomass burning. In addition to biomass burning, secondary OC (SOC) formed during atmospheric long-range transport should be also considered as an important source of OC concentration measured at Gosan. Although this study dealt with the episodic case of the concurrent increase of dust and biomass burning particles, understanding the characteristics of heterogeneous mixing aerosol is essential in assessing the radiative forcing of aerosol. PMID:25253054</p> <div class="credits"> <p class="dwt_author">Nguyen, Duc Luong; Kim, Jin Young; Ghim, Young Sung; Shim, Shang-Gyoo</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">132</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/671914"> <span id="translatedtitle">Daytime Raman lidar measurements of water vapor during the ARM 1997 water vapor intensive <span class="hlt">observation</span> <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Because of the importance of water vapor, the ARM program initiated a series of three intensive operating <span class="hlt">periods</span> (IOPs) at its CART (Cloud And Radiation Testbed) site. The goal of these IOPs is to improve and validate the state-of-the-art capabilities in measuring water vapor. To date, two of the planned three IOPs have occurred: the first was in September of 1996, with an emphasis on the lowest kilometer, while the second was conducted from September--October 1997 with a focus on both the upper troposphere and lowest kilometer. These IOPs provided an excellent opportunity to compare measurements from other systems with those made by the CART Raman lidar. This paper addresses primarily the daytime water vapor measurements made by the lidar system during the second of these IOPs.</p> <div class="credits"> <p class="dwt_author">Turner, D.D. [Pacific Northwest National Lab., Richland, WA (United States); Goldsmith, J.E.M. [Sandia National Labs., Livermore, CA (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">133</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19900060410&hterms=finite+state+automata&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dfinite%2Bstate%2Bautomata"> <span id="translatedtitle">On the <span class="hlt">periodicity</span> of symbolic <span class="hlt">observations</span> of piecewise smooth discrete-time systems</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">A study is made of the behavior of discrete-time systems composed of a set of smooth transition maps coupled by a quantized feedback function. The feedback function partitions the state space into disjoint regions and assigns a smooth transition function to each region. The main result is that under a constraint on the norm of the derivative of the transition maps, a bounded state trajectory with limit points in the interior of the switching regions leads to a region index sequence that is eventually <span class="hlt">periodic</span>. Under these assumptions, it is shown that eventually the feedback function is determined by a finite state automaton. A similar result is proved in the case of finite state dynamic feedback.</p> <div class="credits"> <p class="dwt_author">Ramadge, Peter J.</p> <p class="dwt_publisher"></p> <p class="publishDate">1990-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">134</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19900027065&hterms=burnett&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D80%26Ntt%3Dburnett"> <span id="translatedtitle"><span class="hlt">Periodic</span> behaviors in the <span class="hlt">observed</span> vertical column abundances of atmospheric hydroxyl</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">OH vertical column abundances measured at Fritz Peak Observatory, Colorado, from 1977 through 1988 reveal semi-annual and annual cycles which are amplitude modulated over the 11-year data base. The modulation of the OH seasonal behavior is in phase with solar activity as described by the sunspot number index. No mechanism for the <span class="hlt">observed</span> covariance of this OH behavior with solar activity has yet been identified.</p> <div class="credits"> <p class="dwt_author">Burnett, Elizabeth Beaver; Burnett, Clyde R.; Minschwaner, Kenneth R.</p> <p class="dwt_publisher"></p> <p class="publishDate">1989-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">135</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014ApJ...790..150S"> <span id="translatedtitle">Imaging <span class="hlt">Observation</span> of Quasi-<span class="hlt">periodic</span> Disturbances' Amplitudes Increasing with Height in the Polar Region of the Solar Corona</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">At present, there have been few extreme ultraviolet (EUV) imaging <span class="hlt">observations</span> of spatial variations of the density perturbations due to the slow magnetoacoustic waves (SMWs) propagating along the solar coronal magnetic fields. In this paper, we present such <span class="hlt">observations</span> taken from the polar region of the corona with the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory and investigate the amplitude of quasi-<span class="hlt">periodic</span> propagating disturbances that increase with height in the lower corona (0-9 Mm over the solar limb). We statistically determined the following parameters associated with the disturbances: pressure scale height, <span class="hlt">period</span>, and wavelength in AIA 171 Å, 193 Å, and 211 Å channels. The scale height and wavelength are dependent of temperature, while the <span class="hlt">period</span> is independent of temperature. The acoustic velocities inferred from the scale height highly correlate with the ratios of wavelength to <span class="hlt">period</span>, i.e., phase speeds. They provide evidence that the propagating disturbances in the lower corona are likely SMWs and the spatial variations in EUV intensity in the polar region likely reflects the density compressional effect by the propagating SMWs.</p> <div class="credits"> <p class="dwt_author">Su, J. T.; Liu, Y.; Shen, Y. D.; Priya, T. G.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-08-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">136</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19950053070&hterms=spatial+variability+patterns&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dspatial%2Bvariability%2Bpatterns"> <span id="translatedtitle"><span class="hlt">Observations</span> on the long-<span class="hlt">period</span> variability of the Gulf Stream downstream of Cape Hatteras</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">To examine the long-<span class="hlt">period</span> variability of the Gulf Stream, sea level residuals relative to a 2-year mean sea level in the Gulf Stream downstream of Cape Hatteras (between 75 deg W and 60 deg W longitude) are used. Residuals, as derived from Geosat altimetry between November 1986 and December 1988, were gridded in space and time at a temporal resolution of 10 days and spatial resolution of 1/4 deg. Complex empirical orthogonal function (CEOF) analysis was applied to the data set to extract the spatially correlated signal with the original data subsampled to 1/2 deg. In addition to determining the space-time scales and propagation characterisitics of the different modes, wavenumber-frequency spectral techniques were used to separate the variability into propagating and stationary components. The CEOF technique applied to the data set indicated that the first four CEOF modes accounted for 60% of the variability and were found to be above the noise leve 99% of the time. CEOF 1 was associated with westward propagation at 5 km/d at a wavelength of 2000 km and eastward propagation at 1-2 km/d centered at a 500-km wavelength. This first CEOF is in good agreement with thin-jet equivalent barotropic models which predict westward propagation for wavelengths greater than 1130 km. A deflection of the wavelike pattern at 65 deg W also indicates a possible topographic effect. A simple scaling of the effect of topography indicates that for length scales longer than the internal Rossby radius of deformation, the topographic term is at least of the same order of magnitude as the beta effect. The second CEOF was more broadbanded in wavenumber space, with eastward propagation occurring in a wavenumber-frequency band between 300 and 1400 km and 0.5 and 2.0 cycles/yr. The third CEOF is similar in structure to the first, but with less energy. CEOF 4 was clearly identifiable with higher frequencies than the first three with westward propagation at 4 km/d. The spatial location of this mode along with the westward propagation indicates possible influences from eddy-stream interactions. Thus topography, Rossby wave dynamics and eddy-stream interactions all appear to have a significant role in determining the space-time scales and propagation properties of the long-<span class="hlt">period</span> response of sea level in the Gulf Stream.</p> <div class="credits"> <p class="dwt_author">Vazquez, Jorge</p> <p class="dwt_publisher"></p> <p class="publishDate">1993-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">137</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19820029721&hterms=thermal+plasma&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dthermal%2Bplasma"> <span id="translatedtitle">ISEE 1 <span class="hlt">observations</span> of thermal plasma in the vicinity of the plasmasphere during <span class="hlt">periods</span> of quieting magnetic activity</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">An investigation of thermal plasma behavior in the vicinity of the plasmasphere during <span class="hlt">periods</span> of quieting magnetic activity was conducted by combining thermal ion <span class="hlt">observations</span> made with the plasma composition experiment on ISEE 1 with plasma density profiles obtained from plasma frequency measurements made with the same satellite's plasma wave experiment. During <span class="hlt">periods</span> in which the magnetic activity quiets, the two regions characterized by H(+):He(+):O(+) (isotropic) and H(+):O(+):He(+) (field-aligned) ion species distributions (in order of dominance) are separated by a new region in which low-energy H(+) and He(+) are found flowing along the magnetic field lines. At other times, following quieting magnetic activity, distributions having peak fluxes at 90 deg pitch angle are <span class="hlt">observed</span> in this region.</p> <div class="credits"> <p class="dwt_author">Horwitz, J. L.; Baugher, C. R.; Chappell, C. R.; Shelley, E. G.; Young, D. T.; Anderson, R. R.</p> <p class="dwt_publisher"></p> <p class="publishDate">1981-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">138</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015AJ....149...66N"> <span id="translatedtitle">VI-Band Follow-Up <span class="hlt">Observations</span> of Ultra-Long-<span class="hlt">Period</span> Cepheid Candidates in M31</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The ultra-long-<span class="hlt">period</span> Cepheids (ULPCs) are classical Cepheids with pulsation <span class="hlt">periods</span> exceeding ? 80 days. The intrinsic brightness of ULPCs are ˜ 1 to ˜ 3 mag brighter than their shorter <span class="hlt">period</span> counterparts. This makes them attractive in future distance scale work to derive distances beyond the limit set by the shorter <span class="hlt">period</span> Cepheids. We have initiated a program to search for ULPCs in M31, using the single-band data taken from the Palomar Transient Factory, and identified eight possible candidates. In this work, we presented the VI-band follow-up <span class="hlt">observations</span> of these eight candidates. Based on our VI-band light curves of these candidates and their locations in the color-magnitude diagram and the <span class="hlt">Period</span>-Wesenheit diagram, we verify two candidates as being truly ULPCs. The six other candidates are most likely other kinds of long-<span class="hlt">period</span> variables. With the two confirmed M31 ULPCs, we tested the applicability of ULPCs in distance scale work by deriving the distance modulus of M31. It was found to be {{? }M31,ULPC}=24.30+/- 0.76 mag. The large error in the derived distance modulus, together with the large intrinsic dispersion of the <span class="hlt">Period</span>-Wesenheit (PW) relation and the small number of ULPCs in a given host galaxy, means that the question of the suitability of ULPCs as standard candles is still open. Further work is needed to enlarge the sample of calibrating ULPCs and reduce the intrinsic dispersion of the PW relation before re-considering ULPCs as suitable distance indicators.</p> <div class="credits"> <p class="dwt_author">Ngeow, Chow-Choong; Lee, Chien-Hsiu; Yang, Michael Ting-Chang, Michael; Lin, Chi-Sheng; Hsiao, Hsiang-Yao; Cheng, Yu-Chi; Lin, Zhong-Yi; Lin, I.-Ling; Kanbur, Shashi M.; Ip, Wing-Huen</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-02-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">139</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.eri.u-tokyo.ac.jp/seno/Papers/2007columbia.univ.press.pdf"> <span id="translatedtitle">On the basis of the <span class="hlt">observation</span> that there is no intraslab seismicity or low-frequency tremor north of the Izu collision zone in central Honshu, I <span class="hlt">suggest</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">- frequency tremor north of the Izu collision zone in central Honshu, I <span class="hlt">suggest</span> that the lack of dehydration a viewpoint of dehydration of the subducting slab. The non- existence of low-frequency tremors in some parts</p> <div class="credits"> <p class="dwt_author">Seno, Tetsuzo</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">140</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/42044577"> <span id="translatedtitle">Hisslers: Quasi-<span class="hlt">periodic</span> VLF noise forms <span class="hlt">observed</span> at low latitude ground station Jammu (L = 1.17)</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">This paper reports the <span class="hlt">observation</span> of hisslers at a low latitude ground station Jammu (geomag. lat., 22°26'N), which are falling tone noises during the <span class="hlt">period</span> of hiss activity and appear in minute-long sequences with average spacing between individual bursts of the order of 0.2 seconds and falling tones do not overlap in time. Generation and propagation mechanisms are briefly discussed.</p> <div class="credits"> <p class="dwt_author">Krishna Kumar Singh; Rajesh Singh; R. P. Singh; Shyampati</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_6");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return 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onClick='return showDiv("page_12");' href="#">12</a> <a onClick='return showDiv("page_13");' href="#">13</a> <a onClick='return showDiv("page_14");' href="#">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a onClick='return showDiv("page_16");' href="#">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a onClick='return showDiv("page_21");' href="#">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_9");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">141</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.dtm.ciw.edu/users/paul/journals/laugh04.pdf"> <span id="translatedtitle">A Comparison of <span class="hlt">Observationally</span> Determined Radii with Theoretical Radius Predictions for Short-<span class="hlt">Period</span> Transiting Extrasolar Planets</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Two extrasolar planets, HD 209458b and TrES-1, are currently known to transit bright parent stars for which physical properties can be accurately determined. The two transiting planets have very similar masses and <span class="hlt">periods</span> and hence invite detailed comparisons between their <span class="hlt">observed</span> and theoretically predicted properties. In this paper, we carry out these comparisons. We first report photometric and spectroscopic follow-up</p> <div class="credits"> <p class="dwt_author">Gregory Laughlin; Aaron Wolf; Tonny Vanmunster; Peter Bodenheimer; Debra Fischer; Geoff Marcy; Paul Butler; Steve Vogt</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">142</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011ApJ...730L...3M"> <span id="translatedtitle"><span class="hlt">Observing</span> Evolution in the Supergranular Network Length Scale During <span class="hlt">Periods</span> of Low Solar Activity</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We present the initial results of an <span class="hlt">observational</span> study into the variation of the dominant length scale of quiet solar emission: supergranulation. The distribution of magnetic elements in the lanes that from the network affects, and reflects, the radiative energy in the plasma of the upper solar chromosphere and transition region at the magnetic network boundaries forming as a result of the relentless interaction of magnetic fields and convective motions of the Suns' interior. We demonstrate that a net difference of ~0.5 Mm in the supergranular emission length scale occurs when comparing <span class="hlt">observation</span> cycle 22/23 and cycle 23/24 minima. This variation in scale is reproduced in the data sets of multiple space- and ground-based instruments and using different diagnostic measures. By means of extension, we consider the variation of the supergranular length scale over multiple solar minima by analyzing a subset of the Mount Wilson Solar Observatory Ca II K image record. The <span class="hlt">observations</span> and analysis presented provide a tantalizing look at solar activity in the absence of large-scale flux emergence, offering insight into times of "extreme" solar minimum and general behavior such as the phasing and cross-dependence of different components of the spectral irradiance. Given that the modulation of the supergranular scale imprints itself in variations of the Suns' spectral irradiance, as well as in the mass and energy transport into the entire outer atmosphere, this preliminary investigation is an important step in understanding the impact of the quiet Sun on the heliospheric system.</p> <div class="credits"> <p class="dwt_author">McIntosh, Scott W.; Leamon, Robert J.; Hock, Rachel A.; Rast, Mark P.; Ulrich, Roger K.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-03-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">143</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/21560441"> <span id="translatedtitle"><span class="hlt">OBSERVING</span> EVOLUTION IN THE SUPERGRANULAR NETWORK LENGTH SCALE DURING <span class="hlt">PERIODS</span> OF LOW SOLAR ACTIVITY</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We present the initial results of an <span class="hlt">observational</span> study into the variation of the dominant length scale of quiet solar emission: supergranulation. The distribution of magnetic elements in the lanes that from the network affects, and reflects, the radiative energy in the plasma of the upper solar chromosphere and transition region at the magnetic network boundaries forming as a result of the relentless interaction of magnetic fields and convective motions of the Suns' interior. We demonstrate that a net difference of {approx}0.5 Mm in the supergranular emission length scale occurs when comparing <span class="hlt">observation</span> cycle 22/23 and cycle 23/24 minima. This variation in scale is reproduced in the data sets of multiple space- and ground-based instruments and using different diagnostic measures. By means of extension, we consider the variation of the supergranular length scale over multiple solar minima by analyzing a subset of the Mount Wilson Solar Observatory Ca II K image record. The <span class="hlt">observations</span> and analysis presented provide a tantalizing look at solar activity in the absence of large-scale flux emergence, offering insight into times of 'extreme' solar minimum and general behavior such as the phasing and cross-dependence of different components of the spectral irradiance. Given that the modulation of the supergranular scale imprints itself in variations of the Suns' spectral irradiance, as well as in the mass and energy transport into the entire outer atmosphere, this preliminary investigation is an important step in understanding the impact of the quiet Sun on the heliospheric system.</p> <div class="credits"> <p class="dwt_author">McIntosh, Scott W.; Rast, Mark P. [High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307 (United States); Leamon, Robert J. [Department of Physics, Montana State University, Bozeman, MT 59717 (United States); Hock, Rachel A. [Laboratory for Atmospheric and Space Physics, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309 (United States); Ulrich, Roger K. [Division of Astronomy and Astrophysics, University of California, Los Angeles, CA 90095 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-03-20</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">144</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/1030530"> <span id="translatedtitle">Suzaku And Multi-Wavelength <span class="hlt">Observations</span> of OJ 287 During the <span class="hlt">Periodic</span> Optical Outburst in 2007</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Suzaku <span class="hlt">observations</span> of the blazar OJ 287 were performed in 2007 April 10-13 and November 7-9. They correspond to a quiescent and a flaring state, respectively. The X-ray spectra of the source can be well described with single power-law models in both exposures. The derived X-ray photon index and the flux density at 1 keV were found to be {Lambda} = 1.65 {+-} 0.02 and S{sub 1keV} = 215 {+-} 5 nJy, in the quiescent state. In the flaring state, the source exhibited a harder X-ray spectrum ({Lambda} = 1.50 {+-} 0.01) with a nearly doubled X-ray flux density S{sub 1keV} = 404{sub -5}{sup +6} nJy. Moreover, significant hard X-ray signals were detected up to {approx} 27 keV. In cooperation with the Suzaku, simultaneous radio, optical, and very-high-energy {gamma}-ray <span class="hlt">observations</span> of OJ 287 were performed with the Nobeyama Millimeter Array, the KANATA telescope, and the MAGIC telescope, respectively. The radio and optical fluxes in the flaring state (3.04 {+-} 0.46 Jy and 8.93 {+-} 0.05 mJy at 86.75 Hz and in the V-band, respectively) were found to be higher by a factor of 2-3 than those in the quiescent state (1.73 {+-} 0.26 Jy and 3.03 {+-} 0.01 mJy at 86.75 Hz and in the V-band, respectively). No notable {gamma}-ray events were detected in either <span class="hlt">observation</span>. The spectral energy distribution of OJ 287 indicated that the X-ray spectrum was dominated by inverse Compton radiation in both <span class="hlt">observations</span>, while synchrotron radiation exhibited a spectral cutoff around the optical frequency. Furthermore, no significant difference in the synchrotron cutoff frequency was found between the quiescent and flaring states. According to a simple synchrotron self-Compton model, the change of the spectral energy distribution is due to an increase in the energy density of electrons with small changes of both the magnetic field strength and the maximum Lorentz factor of electrons.</p> <div class="credits"> <p class="dwt_author">Seta, Hiromi; /Saitama U.; Isobe, N.; /Kyoto U.; Tashiro, Makoto S.; /Saitama U.; Yaji, Yuichi; /Saitama U.; Arai, Akira; /Hiroshima U.; Fukuhara, Masayuki; /Tokyo U. /Grad. U. for Adv. Stud., Nagano; Kohno, Kotaro; /Tokyo U.; Nakanishi, Koichiro; /Grad. U. for Adv. Stud., Nagano; Sasada, Mahito; /Hiroshima U.; Shimajiri, Yoshito; /Tokyo U. /Grad. U. for Adv. Stud., Nagano; Tosaki, Tomoka; /Grad. U. for Adv. Stud., Nagano; Uemura, Makoto; /Hiroshima U.; Anderhub, Hans; /Zurich, ETH; Antonelli, L.A.; /INFN, Rome; Antoranz, Pedro; /Madrid U.; Backes, Michael; /Dortmund U.; Baixeras, Carmen; /Barcelona, Autonoma U.; Balestra, Silvia; /Madrid U.; Barrio, Juan Abel; /Madrid U.; Bastieri, Denis; /Padua U. /INFN, Padua; Becerra Gonzalez, Josefa; /IAC, La Laguna /Dortmund U. /Lodz U. /Lodz U. /DESY /Zurich, ETH /Munich, Max Planck Inst. /Padua U. /INFN, Padua /Siena U. /INFN, Siena /Barcelona, IEEC /Munich, Max Planck Inst. /Barcelona, IEEC /Madrid U. /Zurich, ETH /Wurzburg U. /Zurich, ETH /Madrid U. /Munich, Max Planck Inst. /Zurich, ETH /Madrid U. /Barcelona, IFAE /IAC, La Laguna /Laguna U., Tenerife /INFN, Rome /Dortmund U. /Udine U. /INFN, Udine /INFN, Padua /Udine U. /INFN, Udine /Barcelona, IEEC /Madrid U. /Udine U. /INFN, Udine /Udine U. /INFN, Udine /Udine U. /INFN, Udine /IAC, La Laguna /Madrid, CIEMAT /Sierra Nevada Observ. /Zurich, ETH /Padua U. /INFN, Padua /Wurzburg U. /Barcelona, IFAE /UC, Davis /Barcelona, IFAE /Barcelona, IFAE /Madrid U. /Barcelona, Autonoma U. /Munich, Max Planck Inst. /IAC, La Laguna /Laguna U., Tenerife /Barcelona, IFAE /IAC, La Laguna /Munich, Max Planck Inst. /Barcelona, Autonoma U. /Munich, Max Planck Inst. /SLAC /IAC, La Laguna /Laguna U., Tenerife /Zurich, ETH /Wurzburg U. /Munich, Max Planck Inst. /Munich, Max Planck Inst. /Munich, Max Planck Inst. /Zurich, ETH /INFN, Rome /UC, Davis /Siena U. /INFN, Siena /Turku U. /Padua U. /INFN, Padua /Udine U. /INFN, Udine /Padua U. /INFN, Padua /Zurich, ETH /Munich, Max Planck Inst. /DESY /Sofiya, Inst. Nucl. Res. /Udine U. /INFN, Udine /Wurzburg U. /INFN, Rome /Padua U. /INFN, Padua /Barcelona, IFAE /Barcelona, IFAE /Siena U. /INFN, Siena /Wurzburg U. /Madrid U. /Munich, Max Planck Inst. /Munich, Max Planck Inst. /Barcelona, IEEC /Sierra Nevada Observ. /Barcelona, IFAE /Madrid U. /Turku U. /Munich, Max Planck Inst. /Munich, Max Planck Inst. /UC, Santa Cruz /Madrid U. /Siena U. /INFN, Siena /Barcelona, IEEC /Turku U. /Padua U. /INFN, Padua /Zurich, ETH /Siena U. /INFN, Siena /Sierra Nevada Observ. /Udine U. /INFN, Udine /INFN, Trieste /Padua U. /INFN, Padua /Sierra Nevada Observ. /Padua U. /INFN, Padua /Barcelona, IFAE /Barcelona, IFAE /Dortmund U. /Barcelona, IEEC /ICREA, Barcelona /Barcelona, IFAE /Zurich, ETH /Barcelona, Autonoma U. /Wurzburg U. /Padua U. /INFN, Padua /Munich, Max Planck Inst. /INFN, Rome /Sierra Nevada Observ. /DESY /Padua U. /INFN, Padua /Udine U. /INFN, Udine /Munich, Max Planck Inst. /Munich, Max Planck Inst. /Pisa U. /INFN, Pisa /Barcelona, IFAE /Barcelona, IEEC /Turku U. /Munich, Max Planck Inst. /Lodz U. /Lodz U. /Wurzburg U. /Siena U. /INFN, Siena /Zurich, ETH /Turku U. /INFN, Rome /Sofiya, Inst. Nucl. Res. /Barcelona, IFAE /Munich, Max Planck Inst. /DESY /ICREA, Barcelona /Barcelona, IEEC /Siena U. /INFN, Siena /Sofiya, Inst. Nucl. Res. /Munich, Max Planck Inst. /Munich, Max Planck Inst. /Barcelona, IEEC /Sierra Nevada Observ. /Barcelona, IFAE /Barcelona, Autonoma U.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">145</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014AdSpR..53...48K"> <span id="translatedtitle">Traveling ionospheric disturbances <span class="hlt">observed</span> at South African midlatitudes during the 29-31 October 2003 geomagnetically disturbed <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This paper presents traveling ionospheric disturbances (TIDs) <span class="hlt">observations</span> from GPS measurements over the South African region during the geomagnetically disturbed <span class="hlt">period</span> of 29-31 October 2003. Two receiver arrays, which were along two distinct longitudinal sectors of about 18°-20° and 27°-28° were used in order to investigate the amplitude, <span class="hlt">periods</span> and virtual propagation characteristics of the storm induced ionospheric disturbances. The study revealed a large sudden TEC increase on 28 October 2003, the day before the first of the two major storms studied here, that was recorded simultaneously by all the receivers used. This pre-storm enhancement was linked to an X-class solar flare, auroral/magnetospheric activities and vertical plasma drift, based on the behaviour of the geomagnetic storm and auroral indices as well as strong equatorial electrojet. Diurnal trends of the TEC and foF2 measurements revealed that the geomagnetic storm caused a negative ionospheric storm; these parameters were depleted between 29 and 31 October 2003. Large scale traveling ionospheric disturbances were <span class="hlt">observed</span> on the days of the geomagnetic storms (29 and 31 October 2003), using line-of-sight vertical TEC (vTEC) measurements from individual satellites. Amplitude and dominant <span class="hlt">periods</span> of these structures varied between 0.08-2.16 TECU, and 1.07-2.13 h respectively. The wave structures were <span class="hlt">observed</span> to propagate towards the equator with velocities between 587.04 and 1635.09 m/s.</p> <div class="credits"> <p class="dwt_author">Katamzi, Zama T.; Habarulema, John Bosco</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">146</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19920006241&hterms=quantifying+methane+oxidation&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dquantifying%2Bmethane%2Boxidation"> <span id="translatedtitle">Theory and <span class="hlt">observations</span>: Model simulations of the <span class="hlt">period</span> 1955-1985</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The main objective of the theoretical studies presented here is to apply models of stratospheric chemistry and transport in order to understand the processes that control stratospheric ozone and that are responsible for the <span class="hlt">observed</span> variations. The model calculations are intended to simulate the <span class="hlt">observed</span> behavior of atmospheric ozone over the past three decades (1955-1985), for which there exists a substantial record of both ground-based and, more recently, satellite measurements. Ozone concentrations in the atmosphere vary on different time scales and for several different causes. The models described here were designed to simulate the effect on ozone of changes in the concentration of such trace gases as CFC, CH4, N2O, and CO2. Changes from year to year in ultraviolet radiation associated with the solar cycle are also included in the models. A third source of variability explicitly considered is the sporadic introduction of large amounts of NO sub x into the stratosphere during atmospheric nuclear tests.</p> <div class="credits"> <p class="dwt_author">Isaksen, Ivar S. A.; Eckman, R.; Lacis, A.; Ko, Malcolm K. W.; Prather, M.; Pyle, J.; Rodhe, H.; Stordal, Frode; Stolarski, R. S.; Turco, R. P.</p> <p class="dwt_publisher"></p> <p class="publishDate">1989-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">147</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/5496693"> <span id="translatedtitle">Plasma-wave <span class="hlt">observations</span> at Uranus from Voyager 2. Progress report for <span class="hlt">period</span> ending February 1986</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Radio emissions from Uranus were detected by the Voyager 2 plasma-wave instrument about 5 days before closest approach at frequencies of 31.1 and 56.2 khz. The bow shock was identified by an abrupt broadband burst of electrostatic turbulence about 10 hours before closest approach at a radial distance of 23.5 ru. Once inside of the magnetosphere, strong whistler mode hiss and chorus emissions were <span class="hlt">observed</span> at radial distances less than about 8 R/sub u/, in the same region where the energetic-particle instruments detected intense fluxes of energetic electrons. A variety of other plasma waves, such as (f sub c) electron-cyclotron waves, were also <span class="hlt">observed</span> in this same region. At the ring plane crossing, the plasma wave instrument detected a large number of impulsive events that are interpreted as impacts of micron-sized dust particles on the spacecraft. The maximum impact rate was about 20 to 30 impacts/sec, and the north-south thickness of the impact region was about 4000 km. This paper presents an overview of the principal results from the plasma-wave instrument, starting with the first detection of radio emissions from Uranus, and ending a few days after closest approach.</p> <div class="credits"> <p class="dwt_author">Gurnett, D.A.; Kurth, W.S.; Scarf, F.L.; Poynter, R.L.</p> <p class="dwt_publisher"></p> <p class="publishDate">1986-03-26</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">148</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/671917"> <span id="translatedtitle">Water vapor measurements by Raman lidar during the ARM 1997 water vapor intensive <span class="hlt">observation</span> <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Water vapor is the most important greenhouse gas in the atmosphere, as it is the most active infrared absorber and emitter of radiation, and it also plays an important role in energy transport and cloud formation. Accurate, high resolution measurements of this variable are critical in order to improve the understanding of these processes and thus their ability to model them. Because of the importance of water vapor, the Department of Energy`s Atmospheric Radiation Measurement (ARM) program initiated a series of three intensive operating <span class="hlt">periods</span> (IOPs) at its Cloud and Radiation Testbed (CART) site in northern Oklahoma. The goal of these IOPs is to improve and validate the state-of-the-art capabilities in measuring water vapor. To date, two of the planned three IOPs have occurred: the first was in September of 1996, with an emphasis on the lowest kilometer, while the second was conducted from September--October 1997 with a focus on both the upper troposphere and lowest kilometer. The ARM CART site is the home of several different water vapor measurement systems. These systems include a Raman lidar, a microwave radiometer, a radiosonde launch site, and an instrumented tower. During these IOPs, additional instrumentation was brought to the site to augment the normal measurements in the attempt to characterize the CART instruments and to address the need to improve water vapor measurement capabilities. Some of the instruments brought to the CART site include a scanning Raman lidar system from NASA/GSFC, additional microwave radiometers from NOAA/ETL, a chilled mirror that was flown on a tethersonde and kite system, and dewpoint hygrometer instruments flow on the North Dakota Citation. This paper will focus on the Raman lidar intercomparisons from the second IOP.</p> <div class="credits"> <p class="dwt_author">Turner, D.D. [Pacific Northwest National Lab., Richland, WA (United States); Whiteman, D.N.; Schwemmer, G.K. [National Aeronautics and Space Administration, Greenbelt, MD (United States). Goddard Space Flight Center; Evans, K.D. [Univ. of Maryland, Baltimore, MD (United States)]|[National Aeronautics and Space Administration, Greenbelt, MD (United States). Goddard Space Flight Center; Melfi, S.H. [Univ. of Maryland, Baltimore, MD (United States); Goldsmith, J.E. [Sandia National Labs., Livermore, CA (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">149</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/astro-ph/0204246v1"> <span id="translatedtitle"><span class="hlt">Observation</span> of <span class="hlt">periodic</span> variable stars towards the galactic spiral arms by EROS II</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We present the results of a massive variability search based on a photometric survey of a six square degree region along the Galactic plane at ($l = 305^\\circ$, $b = -0.8^\\circ$) and ($l = 330^\\circ$, $b = -2.5^\\circ$). This survey was performed in the framework of the EROS II (Exp\\'erience de Recherche d'Objets Sombres) microlensing program. The variable stars were found among 1,913,576 stars that were monitored between April and June 1998 in two passbands, with an average of 60 measurements. A new <span class="hlt">period</span>-search technique is proposed which makes use of a statistical variable that characterizes the overall regularity of the flux versus phase diagram. This method is well suited when the photometric data are unevenly distributed in time, as is our case. 1,362 objects whose luminosity varies were selected. Among them we identified 9 Cepheids, 19 RR Lyrae, 34 Miras, 176 eclipsing binaries and 266 Semi-Regular stars. Most of them are newly identified objects. The cross-identification with known catalogues has been performed. The mean distance of the RR Lyrae is estimated to be $\\sim 4.9 \\pm 0.3$ kpc undergoing an average absorption of $\\sim 3.4 \\pm 0.2$ magnitudes. This distance is in good agreement with the one of disc stars which contribute to the microlensing source star population.Our catalogue and light curves are available electronically from the CDS, Strasbourg and from our Web site http://eros.in2p3.fr.</p> <div class="credits"> <p class="dwt_author">F. Derue; J. B. Marquette; S. Lupone; C. Afonso; C. Alard; J-N. Albert; A. Amadon; J. Andersen; R. Ansari; E. Aubourg; P. Bareyre; F. Bauer; J-P. Beaulieu; G. Blanc</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-04-15</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">150</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20140017166&hterms=alert&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dalert"> <span id="translatedtitle">Superorbital <span class="hlt">Periodic</span> Modulation in Wind-Accretion High-Mass X-Ray Binaries from Swift Burst Alert Telescope <span class="hlt">Observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">We report the discovery using data from the Swift-Burst Alert Telescope (BAT) of superorbital modulation in the wind-accretion supergiant high-mass X-ray binaries 4U 1909+07 (= X 1908+075), IGR J16418-4532, and IGR J16479-4514. Together with already known superorbital <span class="hlt">periodicities</span> in 2S 0114+650 and IGR J16493-4348, the systems exhibit a monotonic relationship between superorbital and orbital <span class="hlt">periods</span>. These systems include both supergiant fast X-ray transients and classical supergiant systems, and have a range of inclination angles. This <span class="hlt">suggests</span> an underlying physical mechanism which is connected to the orbital <span class="hlt">period</span>. In addition to these sources with clear detections of superorbital <span class="hlt">periods</span>, IGR J16393-4643 (= AX J16390.4-4642) is identified as a system that may have superorbital modulation due to the coincidence of low-amplitude peaks in power spectra derived from BAT, Rossi X-Ray Timing Explorer Proportional Counter Array, and International Gamma-Ray Astrophysics Laboratory light curves. 1E 1145.1-6141 may also be worthy of further attention due to the amount of low-frequency modulation of its light curve. However, we find that the presence of superorbital modulation is not a universal feature of wind-accretion supergiant X-ray binaries.</p> <div class="credits"> <p class="dwt_author">Corbet, Robin H. D.; Krimm, Hans A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">151</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013JGRB..118.6311B"> <span id="translatedtitle">Change of apparent segmentation of the San Andreas fault around Parkfield from space geodetic <span class="hlt">observations</span> across multiple <span class="hlt">periods</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Sequences of earthquakes are commonly represented as a succession of <span class="hlt">periods</span> of interseismic stress accumulation followed by coseismic and postseismic phases of stress release. Because the recurrence time of large earthquakes is often greater than the available span of space geodetic data, it has been challenging to monitor the evolution of interseismic loading in its entire duration. Here we analyze large data sets of surface deformation at different key episodes around the Cholame, Parkfield and creeping segments of the San Andreas Fault that show evidence of significant deceleration of fault slip during the interseismic <span class="hlt">period</span>. We compare the average fault slip rates before and after the 2004 Mw6 Parkfield earthquake, in the 1986-2004 and 2006-2012 <span class="hlt">periods</span>, respectively, avoiding 2 years of postseismic deformation after 2004. Using a combination of GPS data from the Plate Boundary Observatory, the Southern California Earthquake Center Crustal Motion Map and the Bay Area Velocity Unification networks and interferometric synthetic aperture radar from the Advanced Land <span class="hlt">Observing</span> Satellite (ALOS) and Envisat satellites, we show that the area of coupling at the transition between the Parkfield and Cholame segments appears larger later in the interseismic <span class="hlt">period</span> than it does earlier on. While strong plate coupling is uniform across the Parkfield and Cholame segments in the 1986-2004 <span class="hlt">period</span>, creep occurs south of the 2004 epicenter after 2006, making segmentation of the San Andreas Fault south of Parkfield more clearly apparent. These <span class="hlt">observations</span> indicate that analyses of surface deformation late in the earthquake cycle may overestimate the area of plate coupling. A fault surface creeping much below plate rate may in some case be a region that does not promote earthquake nucleation but rather just be at a slower stage of its evolution. Our analysis also shows signs of large variation of slip velocity above and below plate rate in the creeping segment indicating that cycles of weakening and hardening can also be at play in dominantly aseismic areas.</p> <div class="credits"> <p class="dwt_author">Barbot, Sylvain; Agram, Piyush; De Michele, Marcello</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">152</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014AtmRe.145...12C"> <span id="translatedtitle">Long-term trends and extremes in <span class="hlt">observed</span> daily precipitation and near surface air temperature in the Philippines for the <span class="hlt">period</span> 1951-2010</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary"><span class="hlt">Observed</span> daily precipitation and near surface air temperature data from 34 synoptic weather stations in the Philippines for the <span class="hlt">period</span> 1951-2010 were subjected to trend analysis which revealed an overall warming tendency compared to the normal mean values for the <span class="hlt">period</span> 1961-1990. This warming trend can be <span class="hlt">observed</span> in the annual mean temperatures, daily minimum mean temperatures and to a lesser extent, daily maximum mean temperatures. Precipitation and temperature extremes for the <span class="hlt">period</span> 1951-2010 were also analysed relative to the mean 1961-1990 baseline values. Some stations (Cotabato, Iloilo, Laoag and Tacloban,) show increases in both frequency and intensity of extreme daily rainfall events which are significant at the 95% level with none of the stations showing decreasing trends. The frequency of daily temperature maximum above the 99th percentile (hot days) and nights at the 1st percentile (cold nights) <span class="hlt">suggests</span> that both days and nights in particular are becoming warmer. Such indicators of a warming trend and increase in extreme events in the Philippines are discussed in the context of similar national, regional (Asia Pacific) and global studies. The relevance of such empirically based climatology studies, particularly for nations such as the Philippines which are increasingly vulnerable to the multiple impacts of global climate change, is also considered.</p> <div class="credits"> <p class="dwt_author">Cinco, Thelma A.; de Guzman, Rosalina G.; Hilario, Flaviana D.; Wilson, David M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-08-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">153</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22224072"> <span id="translatedtitle">SWIFT <span class="hlt">OBSERVATIONS</span> OF THE HIGH-MASS X-RAY BINARY IGR J16283-4838 UNVEIL A 288 DAY ORBITAL <span class="hlt">PERIOD</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We report on the temporal and spectral properties of the high-mass X-ray binary IGR J16283-4838 in the hard X-ray band. We searched the first 88 months of Swift Burst Alert Telescope (BAT) survey data for long-term <span class="hlt">periodic</span> modulations. We also investigated the broad band (0.2-150 keV) spectral properties of IGR J16283-4838 complementing the BAT dataset with soft X-ray data from the available Swift-XRT pointed <span class="hlt">observations</span>. The BAT light curve of IGR J16283-4838 revealed a <span class="hlt">periodic</span> modulation at P{sub o} = 287.6 ± 1.7 days (with a significance higher than 4 standard deviations). The profile of the light curve folded at P{sub o} shows a sharp peak lasting ?12 days over a flat plateau. The long-term light curve also shows a ?300 day interval of prolonged enhanced emission. The <span class="hlt">observed</span> phenomenology <span class="hlt">suggests</span> that IGR J16283-4838 has a Be nature, where the narrow <span class="hlt">periodic</span> peaks and the ?300 day outburst can be interpreted as Type I and Type II outbursts, respectively. The broad band 0.2-150 keV spectrum can be described with an absorbed power-law and a steepening in the BAT energy range.</p> <div class="credits"> <p class="dwt_author">Cusumano, G.; Segreto, A.; La Parola, V. [INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Via U. La Malfa 153, I-90146, Palermo (Italy)] [INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Via U. La Malfa 153, I-90146, Palermo (Italy); D'Aì, A. [Dipartimento di Fisica, Università di Palermo, via Archirafi 36, I-90123, Palermo (Italy)] [Dipartimento di Fisica, Università di Palermo, via Archirafi 36, I-90123, Palermo (Italy); Masetti, N. [INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, I-40129, Bologna (Italy)] [INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, I-40129, Bologna (Italy); Tagliaferri, G., E-mail: cusumano@ifc.inaf.it [INAF-Brera Astronomical Observatory, via Bianchi 46, I-23807, Merate (Italy)</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-09-20</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">154</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/1502.07117.pdf"> <span id="translatedtitle">X-ray and EUV <span class="hlt">Observations</span> of Simultaneous Short and Long <span class="hlt">Period</span> Oscillations in Hot Coronal Arcade Loops</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We report decaying quasi-<span class="hlt">periodic</span> intensity oscillations in the X-ray (6-12 keV) and extreme ultraviolet (EUV) channels (131, 94, 1600, 304 \\AA) <span class="hlt">observed</span> by the Fermi GBM (Gamma-ray Burst Monitor) and SDO/AIA, respectively, during a C-class flare. The estimated <span class="hlt">period</span> of oscillation and decay time in the X-ray channel (6-12 keV) was about 202 s and 154 s, respectively. A similar oscillation <span class="hlt">period</span> was detected at the footpoint of the arcade loops in the AIA 1600 and 304 \\AA channels. Simultaneously, AIA hot channels (94 and 131 \\AA) reveal propagating EUV disturbances bouncing back and forth between the footpoints of the arcade loops. The <span class="hlt">period</span> of the oscillation and decay time were about 409 s and 1121 s, respectively. The characteristic phase speed of the wave is about 560 km/s for about 115 Mm loop length, which is roughly consistent with the sound speed at the temperature about 10-16 MK (480-608 km/s). These EUV oscillations are consistent with the SOHO/SUMER Doppler-shift oscillations interpreted as the...</p> <div class="credits"> <p class="dwt_author">Kumar, Pankaj; Cho, Kyung-Suk</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">155</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015MNRAS.448.2890D"> <span id="translatedtitle">Ultrashort-<span class="hlt">period</span> main-sequence eclipsing systems: new <span class="hlt">observations</span> and light-curve solutions of six NSVS binaries</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We carried out photometric and low-resolution spectral <span class="hlt">observations</span> of six eclipsing ultrashort-<span class="hlt">period</span> binaries with main-sequence (MS)components. The light-curve solutions of the Rozhen <span class="hlt">observations</span> show that all targets are overcontact systems. We found a well-defined empirical relation between <span class="hlt">period</span> and semi-major axis for the short-<span class="hlt">period</span> binaries and used it for estimation of the global parameters of the targets. Our results revealed that NSVS 925605 is quite an interesting target: (i) it is one of a few contact binaries with M components; (ii) it exhibits high activity (emission in the H? line, X-ray emission, large cool spots, non-Planck energy distribution); (iii) its components differ in temperature by 700 K. All the appearances of high magnetic activity and the huge fill-out factor (0.7) of NSVS 925605 may be a precursor of the predicted merging of close magnetic binaries. Another unusual binary is NSVS 2700153, which reveals considerable long-term variability.</p> <div class="credits"> <p class="dwt_author">Dimitrov, Dinko P.; Kjurkchieva, Diana P.</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">156</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/21567730"> <span id="translatedtitle">TESTING THE NO-HAIR THEOREM WITH <span class="hlt">OBSERVATIONS</span> IN THE ELECTROMAGNETIC SPECTRUM. III. QUASI-<span class="hlt">PERIODIC</span> VARIABILITY</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">According to the no-hair theorem, astrophysical black holes are uniquely described by their masses and spins. An <span class="hlt">observational</span> test of the no-hair theorem can be performed by measuring at least three different multipole moments of the spacetime of a black hole and verifying whether their values are consistent with the unique combinations of the Kerr solution. In this paper, we study quasi-<span class="hlt">periodic</span> variability <span class="hlt">observed</span> in the emission from black holes across the electromagnetic spectrum as a test of the no-hair theorem. We derive expressions for the Keplerian and epicyclic frequencies in a quasi-Kerr spacetime, in which the quadrupole moment is a free parameter in addition to mass and spin. We show that, for moderate spins, the Keplerian frequency is practically independent of small deviations of the quadrupole moment from the Kerr value, while the epicyclic frequencies exhibit significant variations. We apply this framework to quasi-<span class="hlt">periodic</span> oscillations (QPOs) in black hole X-ray binaries in two different scenarios. In the case that a pair of QPOs can be identified as the fundamental g- and c-modes in the accretion disk, we show that the no-hair theorem can be tested in conjunction with an independent mass measurement. If pairs of oscillations are identified with non-parametric resonance of dynamical frequencies in the accretion disk, then testing the no-hair theorem also requires an independent measurement of the black hole spin. In addition, we argue that VLBI <span class="hlt">observations</span> of Sgr A* may test the no-hair theorem through a combination of imaging <span class="hlt">observations</span> and the detection of quasi-<span class="hlt">periodic</span> variability.</p> <div class="credits"> <p class="dwt_author">Johannsen, Tim [Physics Department, University of Arizona, 1118 East 4th Street, Tucson, AZ 85721 (United States); Psaltis, Dimitrios, E-mail: timj@physics.arizona.edu, E-mail: dpsaltis@email.arizona.edu [Astronomy Department, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">157</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011OAP....24...78U"> <span id="translatedtitle">Investigation of the Activity of the Nucleus of Seyfert Galaxy NGC 7469 during the <span class="hlt">Observation</span> <span class="hlt">Period</span> from 1990 TO 2008</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We combine many published photometrical <span class="hlt">observations</span> of the Seyfert Galaxy (SG) NGC 7469 and also new results from Hubble Space Telescope which can be used for future research of some properties of the activity of the nuclear of the SG. A drift of the activity maximum from 1997 to 1998 is <span class="hlt">observed</span> with an increased of the wave length similarly to some blazars in radio range. Analyzing the surface photometry according to data obtained both at the Maidanak observatory and HST data an intensity asymmetry at the SG central region image is <span class="hlt">observed</span> at different <span class="hlt">periods</span>. The existence of a second component might be supposed. The radius of the active region itself inside the SG kernel is 40-50 parsec.</p> <div class="credits"> <p class="dwt_author">Ugolkova, L. S.; Artamonov, B. P.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">158</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2006AGUFM.H34A..04M"> <span id="translatedtitle">Distributed Data Integration Prototype System for Coordinated Enhanced <span class="hlt">Observing</span> <span class="hlt">Period</span> (CEOP) Data</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The purpose of the JAXA Prototype for CEOP Distributed Data Integration Service is to provide user-friendly access to the CEOP (in-situ, satellite and global gridded model output) data. The system is distributed in the sense that, while the system is located in Tokyo, the data is located in archive centers which are globally distributed. The in-situ data is archived at the National Center for Atmospheric Research (NCAR) Earth <span class="hlt">Observing</span> Laboratory (EOL) in Boulder, Colorado, USA. The NWP global gridded model output data is archived at the Max Planck Institute for Meteorology (MPIM) in cooperation with the World Data Center for Climate (WDC-Climate) in Hamburg, Germany. The satellite data is archived at the IIS (Institute of Industrial Science) at the University of Tokyo, in Tokyo, Japan. Other (non-CEOP) globally distributed data that is on DODS servers can be added in the future according to scientist's requests. The system is integrated in the sense that all of the data is temporally and geospatially coordinated and can be selected and viewed within the same system. The in-situ data are time series data and the global gridded model output data and satellite data are 4D (time series of 2D scenes at levels or in multiple frequency bands). The system knows the geolocation and time of all data sets and supports selection of the data through a uniform set of menus, by data type, reference site and station, and supports sub-setting according to time, area and height/depth. The basic concept for developing the JAXA prototype is " to use existing software where possible". Based on this concept, OPeNDAP, which is widely used in the ocean and atmospheric sciences, was chosen as the data access protocol to enable "access to distributed data". And also the open source Live Access Serve (LAS) was selected as the JAXA Prototype component to enable "integration service". Users can access the system at http://jaxa.ceos.org/wtf_ceop. This system has been online since June 1, 2005 and has more than 90 registered users as of July, 2006 (The site requires a brief registration to satisfy the CEOP data policy of keeping a record of users who receive CEOP data.). All in-situ data is available on the system while satellite and global gridded model output data are being added steadily. When fully established the system should include over 1,000,000 scenes of satellite data contributed by JAXA, NASA, ESA and Eumetsat, and a total of over 40-50 Terabytes of integrated in-situ, satellite and global gridded model output data.</p> <div class="credits"> <p class="dwt_author">Miura, S. H.; Aizawa, K.</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">159</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011ACPD...1128851K"> <span id="translatedtitle">Comparisons of <span class="hlt">observed</span> and modeled OH and HO2 concentrations during the ambient measurement <span class="hlt">period</span> of the HOxComp field campaign</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">A photochemical box model constrained by ancillary <span class="hlt">observations</span> was used to simulate OH and HO2 concentrations for three days of ambient <span class="hlt">observations</span> during the HOxComp field campaign held in Jülich, Germany in July 2005. OH and HO2 levels, <span class="hlt">observed</span> by four and three instruments, respectively, were fairly well reproduced to within 33% by a base model run (Regional Atmospheric Chemistry Mechanism with updated isoprene chemistry adapted from Master Chemical Mechanism ver. 3.1) with high R2 values (0.72-0.97) over a range of isoprene (0.3-2 ppb) and NO (0.1-10 ppb) mixing ratios. Adding isomerization of isoprene peroxy radicals to the model increased OH and HO2 by 43% and 48% on average. Although these are still only 15% and 21% higher than the <span class="hlt">observations</span> made by one of the instruments, larger overestimations (>60%) occurred with respect to the <span class="hlt">observations</span> made by the other three instruments, <span class="hlt">suggesting</span> that the rates of the isomerization were not readily supported by the ensemble of radical <span class="hlt">observations</span>. These model runs tend to underestimate <span class="hlt">observed</span> OH reactivity which may be explained by unmeasured hydrocarbon species. By selecting hydrocarbon types to be added to the model in amounts that accounted for the missing fractions of <span class="hlt">observed</span> OH reactivity, the gaps between HOx <span class="hlt">observations</span> and model results with and without isomerization could be individually diminished to within uncertainty levels. In this case, however, the HO2/OH ratio rose on addition of hydrocarbons and diverged from <span class="hlt">observations</span>. In the case where we used modeled HO2(*), taking into account the sensitivity toward speciated RO2 (organic peroxy) radicals, as recently reported from one of the participating instruments in the HO2 measurement mode, the model's overestimation for HO2 became evident (by factors of more than 1.8). These results strongly indicated that more loss processes for peroxy radicals were necessary to explain the <span class="hlt">observations</span>. One of the measurement days was characterized by low isoprene concentrations (~0.5 ppb) and OH reactivity that was well explained by the <span class="hlt">observed</span> species, especially before noon. For this selected <span class="hlt">period</span>, as opposed to the general behavior, the model tended to underestimate HO2 (and HO2(*)) with respect to <span class="hlt">observations</span> made by the three instruments. We found that this tendency is associated with high NOx concentrations, <span class="hlt">suggesting</span> that some HO2 production or HO2 regeneration processes under high NOx conditions were being overlooked; this might require revision of ozone production regimes.</p> <div class="credits"> <p class="dwt_author">Kanaya, Y.; Hofzumahaus, A.; Dorn, H.-P.; Brauers, T.; Fuchs, H.; Holland, F.; Rohrer, F.; Bohn, B.; Tillmann, R.; Wegener, R.; Wahner, A.; Kajii, Y.; Miyamoto, K.; Nishida, S.; Watanabe, K.; Yoshino, A.; Kubistin, D.; Martinez, M.; Rudolf, M.; Harder, H.; Berresheim, H.; Elste, T.; Plass-Dülmer, C.; Stange, G.; Kleffmann, J.; Elshorbany, Y.; Schurath, U.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-10-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">160</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013ACPD...13.2641B"> <span id="translatedtitle">Variability of aerosol properties over Eastern Europe <span class="hlt">observed</span> from ground and satellites in the <span class="hlt">period</span> from 2003 to 2011</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The paper presents the study of aerosol variability in the <span class="hlt">period</span> from 2003 to 2011 over Eastern Europe region with latitude ranging from 40° N to 60° N and longitude from 20° E to 50° E. The analysis was based on the POLDER/PARASOL and POLDER-2/ADEOS satellites and AERONET ground-based sunphotometer <span class="hlt">observations</span>. The aerosol optical thickness (AOT) of the studied area is characterized by the values (referenced to 870 nm wavelength) ranging from 0.05 to 0.2 except the <span class="hlt">period</span> of July-August 2010 with strong forest and peat wildfires when the AOT typical values range from 0.3 to 0.5. The analysis of seasonal dynamics of aerosol loading has revealed two AOT high value peaks. The first peak <span class="hlt">observed</span> in April-May is the result of solitary transportation of Sahara dust in the atmosphere over Eastern Europe, infrequent agricultural fires, transportation of sea salt aerosols by southern winds to Ukraine and Moldova from the Black and Azov Seas. The second peak in August-September is associated with forest and peat wildfires, considerable transportation of Sahara dust and presence of soil dust aerosols due to harvesting activity. The maximum values of AOT are <span class="hlt">observed</span> in May 2006 (0.1-0.15), April 2009 (0.07-0.15) and August 2010 (0.2-0.5). Furthermore, the study has identified a distinct pattern of anthropogenic aerosols over the industrial areas, especially in the central Ukraine, eastern Belarus, as well as Moscow, Nizhny Novgorod and Stavropol regions in Russia. The comparison of the fine mode AOT (particle radius < 0.3 ?m) derived by standard algorithm POLDER/PARASOL from reflected polarized radiances with those recomputed from AERONET inversions was performed over a number of AERONET sites: over Kyiv and Sevastopol sites for the <span class="hlt">period</span> of 2008-2009 and over Moscow, Minsk, Belsk, and Moldova sites for the <span class="hlt">period</span> of 2005-2009. The correlation coefficients are 0.78 for Moscow, 0.76 - Minsk, 0.86 - Belsk, 0.93 - Kyiv, 0.81 - Moldova and 0.63 for Sevastopol sites. The deviations are explained by the spatial inhomogeneity of the surface polarization that has stronger effect on aerosol retrieval for clear atmospheric conditions with low aerosol loading when surface impact on satellite <span class="hlt">observations</span> is more pronounced. In addition, the preliminary analysis of the detailed aerosol properties derived by new generation PARASOL algorithm was accomplished. The AOT and single scattering albedo retrieved by the algorithm over Kyiv were compared with the closest AERONET retrievals within two hour of satellite overpass time and the stable atmospheric conditions.</p> <div class="credits"> <p class="dwt_author">Bovchaliuk, A.; Milinevsky, G.; Danylevsky, V.; Goloub, P.; Dubovik, O.; Holdak, A.; Ducos, F.; Sosonkin, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_7");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" 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showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_10");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">161</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013AGUFM.H31H1288S"> <span id="translatedtitle">Water quality <span class="hlt">observations</span> of ice-covered, stagnant, eutrophic water bodies and analysis of influence of ice-covered <span class="hlt">period</span> on water quality</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The water quality characteristics of ice-covered, stagnant, eutrophic water bodies have not been clarified because of insufficient <span class="hlt">observations</span>. It has been pointed out that climate change has been shortening the duration of ice-cover; however, the influence of climate change on water quality has not been clarified. This study clarifies the water quality characteristics of stagnant, eutrophic water bodies that freeze in winter, based on our surveys and simulations, and examines how climate change may influence those characteristics. We made fixed-point <span class="hlt">observation</span> using self-registering equipment and vertical water sampling. Self-registering equipment measured water temperature and dissolved oxygen(DO).vertical water sampling analyzed biological oxygen demand(BOD), total nitrogen(T-N), nitrate nitrogen(NO3-N), nitrite nitrogen(NO2-N), ammonium nitrogen(NH4-N), total phosphorus(TP), orthophosphoric phosphorus(PO4-P) and chlorophyll-a(Chl-a). The survey found that climate-change-related increases in water temperature were suppressed by ice covering the water area, which also blocked oxygen supply. It was also clarified that the bottom sediment consumed oxygen and turned the water layers anaerobic beginning from the bottom layer, and that nutrient salts eluted from the bottom sediment. The eluted nutrient salts were stored in the water body until the ice melted. The ice-covered <span class="hlt">period</span> of water bodies has been shortening, a finding based on the analysis of weather and water quality data from 1998 to 2008. Climate change was surveyed as having caused decreases in nutrient salts concentration because of the shortened ice-covered <span class="hlt">period</span>. However, BOD in spring showed a tendency to increase because of the proliferation of phytoplankton that was promoted by the climate-change-related increase in water temperature. To forecast the water quality by using these findings, particularly the influence of climate change, we constructed a water quality simulation model that incorporates the freezing-over of water bodies. The constructed model shows good temporal and spatial reproducibility and enables water quality to be forecast throughout the year, including during the ice-covered <span class="hlt">period</span>. The forecasts using the model agree well with the survey results of shortened ice <span class="hlt">period</span> and climate-change-related increase in the BOD in spring. From the result of calculations and <span class="hlt">observations</span>, it is <span class="hlt">suggested</span> that water quality of spring has been deteriorate because of freezing <span class="hlt">period</span> to be shortened due to temperature rising.</p> <div class="credits"> <p class="dwt_author">sugihara, K.; Nakatsugawa, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">162</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013JAHH...16..312M"> <span id="translatedtitle">Eclipses in the Middle East from the Late Medieval Islamic <span class="hlt">Period</span> to the Early Modern <span class="hlt">Period</span>. Part 1: The <span class="hlt">observation</span> of six lunar eclipses from the Late Medieval Islamic <span class="hlt">Period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This paper deals with the analysis of data obtained from <span class="hlt">observations</span> of two sets of three lunar eclipses in the Late Medieval Islamic <span class="hlt">Period</span>. The first trio consists of the lunar eclipses of 7 March 1262, 7 April 1270 and 24 January 1274, <span class="hlt">observed</span> by Muḥy? al-D?n al-Maghrib?; from the Maragha Observatory (in north-western Iran), and the second includes those of 2 June and 26 November 1406, and 22 May 1407, <span class="hlt">observed</span> by Jamsh?d Ghiy?th al-D?n al-K?sh? from K?sh?n (in central Iran). The results are that al-Maghrib?'s values for the magnitudes of these eclipses agree excellently with modern data, and his values for the times when the maximum phases occurred agree to within five minutes with modern values. Al-K?sh?'s values for the times of the maximum phases show a rather larger divergence from modern data, varying from about ten minutes to about one hour. The errors in all six values both astronomers computed from their own solar parameters for the longitude of the Sun at the instant of the opposition of the Moon to the Sun in these eclipses remain below ten minutes of arc. The motivation for doing these <span class="hlt">observations</span> was to measure the lunar epicycle radius r in the Ptolemaic model. Al-Maghrib? achieved r = 5;12 and al-K?sh? r ? 5;17,1 in terms of the radius of an orbit of R = 60 arbitrary units. It is argued that comparing with modern theory, neither of these two medieval values can be considered an improvement on Ptolemy's value of r = 5;15.</p> <div class="credits"> <p class="dwt_author">Mozaffari, S. Mohammad</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-11-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">163</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010cosp...38.2214C"> <span id="translatedtitle">FASTSAT-HSV01 synergistic <span class="hlt">observations</span> of the magnetospheric response during active <span class="hlt">periods</span>: MINI-ME, PISA and TTI</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Understanding the complex processes within the inner magnetosphere of Earth particularly during storm <span class="hlt">periods</span> requires coordinated <span class="hlt">observations</span> of the particle and field environment using both in-situ and remote sensing techniques. In fact in order to gain a better understand-ing of our Heliophysics and potentially improve our space weather forecasting capabilities, new <span class="hlt">observation</span> mission approaches and new instrument technologies which can provide both cost effective and robust regular <span class="hlt">observations</span> of magnetospheric activity and other space weather related phenomenon are necessary. As part of the effort to demonstrate new instrument tech-niques and achieve necessary coordinated <span class="hlt">observation</span> missions, NASA's Fast Affordable Sci-ence and Technology Satellite Huntsville 01 mission (FASTSAT-HSV01) scheduled for launch in 2010 will afford a highly synergistic solution which satisfies payload mission opportunities and launch requirements as well as contributing in the near term to our improved understanding of Heliophysics. NASA's FASTSAT-HSV01 spacecraft on the DoD Space Test Program-S26 (STP-S26) Mission is a multi-payload mission executed by the DoD Space Test Program (STP) at the Space Development and Test Wing (SDTW), Kirtland AFB, NM. and is an example of a responsive and economical breakthrough in providing new possibilities for small space technology-driven and research missions. FASTSAT-HSV is a unique spacecraft platform that can carry multiple small instruments or experiments to low-Earth orbit on a wide range of expendable launch vehicles for a fraction of the cost traditionally required for such missions. The FASTSAT-HSV01 mission allows NASA to mature and transition a technical capability to industry while increasing low-cost access to space for small science and technology (ST) payloads. The FASTSAT-HSV01 payload includes three NASA Goddard Space Flight Center (GSFC) new technology built instruments that will study the terrestrial space environment and potentially contribute to space weather research in a synergistic manner. MINI-ME, a neutral atom imager, will <span class="hlt">observe</span> the neutral atom inputs to ionospheric heating which can be important during high levels of magnetospheric activity. PISA, a plasma impedance spec-trometer, will measure simultaneously the local electron densities and temperatures as well as measure small scale density structure (500 m spatial scale) during these active <span class="hlt">periods</span>. TTI, a thermospheric imager, will remotely determine the thermospheric temperature response to this magnetospheric activity. Together, these <span class="hlt">observations</span> will contribute significantly to a comprehensive understanding of the flow of energy through and the response of the storm-time terrestrial magnetosphere.</p> <div class="credits"> <p class="dwt_author">Casas, Joseph; Collier, Michael; Rowland, Douglas; Sigwarth, John; Boudreaux, Mark</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">164</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20100031078&hterms=variables+STAR&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dvariables%2BSTAR"> <span id="translatedtitle">High Angular Resolution <span class="hlt">Observations</span> of Episodic Dust Emission from Long <span class="hlt">Period</span> Variable Stars Twenty Years of <span class="hlt">Observations</span> with the Berkeley Infrared Spatial Interferometer</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Over the past twenty years the U. C. Berkeley Infrared Spatial Interferometer has <span class="hlt">observed</span> a number of Long <span class="hlt">Period</span> Variable stars in the mid-infrared, obtaining information on the spatial distribution of dust around these stars with resolutions of the order of a few tens of milliarcseconds. The ISI is a heterodyne interferometer operating mostly at 11.15 microns, initially with two telescopes. In the last decade, it has been taking data regularly with three telescopes, thus obtaining visibility data on three baselines and also a closure phase. Over the course of the years, the ISI has been able to measure the physical properties of the dust shells surrounding these stars, in particular the inner radii of the dust shells, as well as the temperature and density distribution. For some stars, the ISI has also made precision measurements of their diameters in the mid-infrared. Closure phase measurements have revealed asymmetries in the dust distributions around many stars. Most surprisingly the ISI data has shown evidence for substantial changes in the amount of dust on time scales of 5-10 years, rather than being directly correlated with the stellar pulsation <span class="hlt">periods</span>, which are of the order of one year. We discuss past results and new results from the ISI that highlight the dynamic environment around these stars.</p> <div class="credits"> <p class="dwt_author">Danchi, William</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">165</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014AMTD....7.8013D"> <span id="translatedtitle">An overview of the lightning and atmospheric electricity <span class="hlt">observations</span> collected in Southern France during the HYdrological cycle in Mediterranean EXperiment (HyMeX), Special <span class="hlt">Observation</span> <span class="hlt">Period</span> 1</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The PEACH (Projet en Electricité Atmosphérique pour la Campagne HyMeX - the Atmospheric Electricity Project of HyMeX Program) project is the Atmospheric Electricity component of the HyMeX (Hydrology cycle in the Mediterranean Experiment) experiment and is dedicated to the <span class="hlt">observation</span> of both lightning activity and electrical state of continental and maritime thunderstorms in the area of the Mediterranean Sea. During the HyMeX SOP1 (Special <span class="hlt">Observation</span> <span class="hlt">Period</span>; 5 September-6 November 2012), four European Operational Lightning Locating Systems (OLLSs) (ATDNET, EUCLID, LINET, ZEUS) and the HyMeX Lightning Mapping Array network (HyLMA) were used to locate and characterize the lightning activity over the Southeastern Mediterranean at flash, storm and regional scales. Additional research instruments like slow antennas, video cameras, micro-barometer and microphone arrays were also operated. All these <span class="hlt">observations</span> in conjunction with operational/research ground-based and airborne radars, rain gauges and in situ microphysical records aimed at characterizing and understanding electrically active and highly precipitating events over Southeastern France that often lead to severe flash floods. Simulations performed with Cloud Resolving Models like Meso-NH and WRF are used to interpret the results and to investigate further the links between dynamics, microphysics, electrification and lightning occurrence. A description of the different instruments deployed during the field campaign as well as the available datasets is given first. Examples of concurrent <span class="hlt">observations</span> from radio frequency to acoustic for regular and atypical lightning flashes are then presented showing a rather comprehensive description of lightning flashes available from the SOP1 records. Then examples of storms recorded during HyMeX SOP1 over Southeastern France are briefly described to highlight the unique and rich dataset collected. Finally the next steps of the work required for the delivery of reliable lightning-derived products to the HyMeX community are discussed.</p> <div class="credits"> <p class="dwt_author">Defer, E.; Pinty, J.-P.; Coquillat, S.; Martin, J.-M.; Prieur, S.; Soula, S.; Richard, E.; Rison, W.; Krehbiel, P.; Thomas, R.; Rodeheffer, D.; Vergeiner, C.; Malaterre, F.; Pedeboy, S.; Schulz, W.; Farges, T.; Gallin, L.-J.; Ortéga, P.; Ribaud, J.-F.; Anderson, G.; Betz, H.-D.; Meneux, B.; Kotroni, V.; Lagouvardos, K.; Roos, S.; Ducrocq, V.; Roussot, O.; Labatut, L.; Molinié, G.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-08-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">166</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015GMDD....8.1801F"> <span id="translatedtitle">AROME-WMED, a real-time mesoscale model designed for the HyMeX Special <span class="hlt">Observation</span> <span class="hlt">Periods</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">During autumn 2012 and winter 2013, two Special <span class="hlt">Observation</span> <span class="hlt">Periods</span> (SOPs) of the Hydrological cycle in the Mediterranean Experiment (HyMeX) took place. For the preparatory studies and to support the instrument deployment during the field campaign, a dedicated version of the operational convective-scale AROME-France model was developed: the AROME-WMED model. It covers the western Mediterranean basin with a 48 h forecast range. It provided real time analyses and forecasts which were sent daily to the HyMeX operational centre to forecast high precipitation events and to help decision makers on the deployment of <span class="hlt">observation</span> instruments. This paper presents the main features of this numerical weather prediction system in terms of data assimilation and forecast. Some specific data of the HyMeX SOP were assimilated in real time. The forecast skill of the AROME-WMED is then assessed with objective scores and compared to the operational AROME-France model, for both autumn 2012 (5 September to 6 November 2012) and winter 2013 (1 February to 15 March 2013) SOPs. The overall performance of AROME-WMED is good and similar to those of AROME-France for the 0 to 30 h common forecast range. The 24 to 48 h forecast range is of course less accurate but remains useful for scheduling <span class="hlt">observation</span> deployment. The characteristics of parameters such as precipitation, temperature or humidity, are illustrated by one heavy precipitation case study that occurred over the south of Spain.</p> <div class="credits"> <p class="dwt_author">Fourrié, N.; Bresson, É.; Nuret, M.; Jany, C.; Brousseau, P.; Doerenbecher, A.; Kreitz, M.; Nuissier, O.; Sevault, E.; Bénichou, H.; Amodei, M.; Pouponneau, F.</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-02-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">167</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013ACP....13.6587B"> <span id="translatedtitle">Variability of aerosol properties over Eastern Europe <span class="hlt">observed</span> from ground and satellites in the <span class="hlt">period</span> from 2003 to 2011</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The paper presents some results of the study on aerosol variability in the <span class="hlt">period</span> from 2003 to 2011 over the Eastern Europe region, with latitude ranging from 40° N to 60° N and longitude from 20° E to 50° E. The analysis was based on the POLDER/PARASOL and POLDER-2/ADEOS satellites and AERONET (AErosol RObotic NETwork) ground-based sun photometer <span class="hlt">observations</span>. The aerosol optical thickness (AOT) of the studied area is characterized by values (referenced to 870 nm wavelength) ranging from 0.05 to 0.2, except for in the <span class="hlt">period</span> of July-August 2010 with strong forest and peat wildfires when the AOT typical values range from 0.3 to 0.5 according to both retrievals. The analysis of seasonal dynamics of aerosol loading has revealed two AOT high value peaks. The spring peak <span class="hlt">observed</span> in April-May is the result of solitary transportation of Saharan dust in the atmosphere over Eastern Europe, infrequent agricultural fires, transportation of sea salt aerosols by southern winds to Ukraine and Moldova from the Black and Azov seas. The autumn peak in August-September is associated with forest and peat wildfires, considerable transportation of Saharan dust and the presence of soil dust aerosols due to harvesting activity. The maximum values of AOT are <span class="hlt">observed</span> in May 2006 (0.1-0.15), April 2009 (0.07-0.15) and August 2010 (0.2-0.5). Furthermore, the study has identified a distinct pattern of anthropogenic aerosols over the industrial areas, especially in central Ukraine and eastern Belarus as well as Moscow region in Russia. The comparison of the AOT derived by standard algorithm POLDER/PARASOL with those recomputed from AERONET inversions for fine mode particles with radius < 0.3 ?m was performed over several AERONET sites. The correlation coefficients for the POLDER/AERONET AOT retrieval comparisons are equal: 0.78 for Moscow site, 0.76 - Minsk, 0.86 - Belsk, 0.81 - Moldova (<span class="hlt">period</span> 2005-2009), 0.93 - Kyiv and 0.63 for Sevastopol sites (2008-2009). The deviations are explained by the spatial inhomogeneity of the surface polarization that has a stronger effect on aerosol retrieval for clear atmospheric conditions with low aerosol loading when surface impact on satellite <span class="hlt">observations</span> is more pronounced. In addition, the preliminary analysis of the detailed aerosol properties derived by a new generation PARASOL algorithm was evaluated. The comparison of AOT and single scattering albedo retrieved from the POLDER/PARASOL <span class="hlt">observations</span> over Kyiv with the closest AERONET retrievals within 30 min of satellite overpass time and with a cloudless day shows acceptable agreement of the aerosol dynamics. The correspondence of those data is <span class="hlt">observed</span> even for extreme AOT440 value 1.14, which was caused by the forest and peat fires in August 2010.</p> <div class="credits"> <p class="dwt_author">Bovchaliuk, A.; Milinevsky, G.; Danylevsky, V.; Goloub, P.; Dubovik, O.; Holdak, A.; Ducos, F.; Sosonkin, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">168</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/891111"> <span id="translatedtitle">Shortwave Radiative Closure Studies for Clear Skies During the Atmospheric Radiation Measurement 2003 Aerosol Intensive <span class="hlt">Observation</span> <span class="hlt">Period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The Department of Energy's Atmospheric Radiation Measurement (ARM) program sponsored a large aerosol intensive <span class="hlt">observation</span> <span class="hlt">period</span> (AIOP) to study aerosol during the month of May 2003 around the Southern Great Plains (SGP) Climate Research Facility (CRF) in north central Oklahoma. Redundant measurements of aerosol optical properties were made using different techniques at the surface as well as in vertical profile with sensors aboard two aircraft. One of the principal motivations for this experiment was to resolve the disagreement between models and measurements of diffuse horizontal broadband shortwave irradiance at the surface, especially for modest aerosol loading. This paper focuses on using the redundant aerosol and radiation measurements during this AIOP to compare direct beam and diffuse horizontal broadband shortwave irradiance measurements and models at the surface for a wide range of aerosol cases that occurred during 30 clear-sky <span class="hlt">periods</span> on 13 days of May 2003. Models and measurements are compared over a large range of solar-zenith angles. Six different models are used to assess the relative agreement among them and the measurements. Better agreement than previously achieved appears to be the result of better specification of input parameters and better measurements of irradiances than in prior studies. Biases between modeled and measured direct irradiances are in the worst case 1%, and biases between modeled and measured diffuse irradiances are less than 1.9%.</p> <div class="credits"> <p class="dwt_author">Michalsky, Joseph J.; Anderson, Gail; Barnard, James C.; Delamere, Jennifer; Gueymard, C.; Kato, Seiji; Kiedron, P.; McComiskey, A.; Ricchiazzi, P.</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-07-20</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">169</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014AdSpR..54.2151M"> <span id="translatedtitle">Variations in Electron Content Ratio and Semi-thickness Ratio during LSA and MSA <span class="hlt">periods</span> and some Cyclone Genesis <span class="hlt">Periods</span> using COSMIC satellite <span class="hlt">observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In this study for the first time, COSMIC satellite data have been used to deduce values of ionospheric Electron Content Ratio (ECR) and Semi-thickness Ratio (Rtb) for Low Solar Activity (LSA) (2008) and Moderate Solar Activity (MSA) (2012) <span class="hlt">periods</span> over the Indian low-latitude (15-30°N) region with 80-95°E longitude. These two ratios provide sensitive information about bottom and topside ionosphere for different geophysical conditions. Extraction of suspected patterns and discrepancies unfold that the deviations between ECR and Rtb values during LSA <span class="hlt">period</span> are comparatively higher than that of MSA <span class="hlt">period</span> when the diurnal variability in these two parameters is flatter along with the diurnal-dips during pre-noon hours. The correlative relationship of ECR exhibits low association with NmF2 and anti-correlation with HmF2, whereas its correlation with Rtb is extremely high. During Cyclone Genesis <span class="hlt">Period</span> (CGP) strong dips in ECR and Rtb values with respect to pre and post CGP occurred which helps to take decisive conclusion about the ionospheric variations to be dominant through getting relatively higher Ne concentration in the bottom side part of the ionosphere.</p> <div class="credits"> <p class="dwt_author">Mondal, Gopal; Gupta, Manojit; Sen, Goutam Kumar</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">170</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2008AGUFM.A22D..06B"> <span id="translatedtitle"><span class="hlt">Observations</span> of Non-Methane Hydrocarbons Over India During the Asian Summer Monsoon <span class="hlt">Period</span>: Results from CARIBIC</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The CARIBIC project (Civil Aircraft for the Regular Investigation of the Atmosphere Based on an Instrument Container, www.caribic-atmospheric.com) involves the monthly deployment of an instrument container equipped to make atmospheric measurements from onboard a long-range commercial airliner. Since December 2004, flights for the second phase of CARIBIC have been aboard a Lufthansa Airbus A340-600 traveling between Frankfurt, Germany and destinations in Asia, North America and South America. The instrument package housed in the container (1.5 ton) is fully automated and during each monthly set of flights carries out a variety of real-time trace gas and aerosol measurements, and also collects 28 air samples, which are analyzed upon return to the laboratory. Routine measurements made from the sampling flasks include non-methane hydrocarbon (NMHC) analysis, and these measurements provide the basis for the data presented here. Between April and September of 2008, the container was deployed monthly on two sequential roundtrip flights between Frankfurt and Chennai, India. To achieve greater resolution, air samples were collected only on the first of the roundtrip flights, with 14 samples collected on the flight to Chennai and 14 collected on the return. These flights provided the opportunity to study the composition of the upper troposphere in this region during the Asian summer monsoon <span class="hlt">period</span> (typically June-September), which is characterized by anticyclonic circulation in the upper troposphere coupled with deep convection. Samples collected during the monsoon <span class="hlt">period</span> exhibit elevated levels of NMHCs relative to samples collected outside of the monsoon <span class="hlt">period</span>, with enhancements in ethyne and benzene being more substantial than enhancements in the alkanes. Enhanced mixing ratios are <span class="hlt">observed</span> between 15N and 40N, and correspond to enhancements in other trace gases, namely methane and CO. Ethyne in particular is strongly correlated with both methane and CO in this region; while CO and ethyne share a common, combustion, source, methane and ethyne do not, and this relationship indicates convection of a well-mixed air mass that is strongly and recently influenced by both agricultural and anthropogenic/urban sources. Trends in and relationships between NMHCs during the monsoon <span class="hlt">period</span> will be discussed here, as well as their relationships to other trace gases.</p> <div class="credits"> <p class="dwt_author">Baker, A. K.; Schuck, T. J.; Slemr, F.; Brenninkmeijer, C. A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">171</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012EGUGA..14.4765K"> <span id="translatedtitle">Comparisons of <span class="hlt">observed</span> and modeled OH and HO2 concentrations during the ambient measurement <span class="hlt">period</span> of the HOxComp field campaign</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">A photochemical box model constrained by ancillary <span class="hlt">observations</span> was used to simulate OH and HO2 concentrations for three days of ambient <span class="hlt">observations</span> during the HOxComp field campaign held in Jülich, Germany in July 2005. Daytime OH levels <span class="hlt">observed</span> by four instruments were fairly well reproduced to within 33% by a base model run (Regional Atmospheric Chemistry Mechanism with updated isoprene chemistry adapted from Master Chemical Mechanism ver. 3.1) with high R2 values (0.72-0.97) over a range of isoprene (0.3-2 ppb) and NO (0.1-10 ppb) mixing ratios. Daytime HO2(*) levels, reconstructed from the base model results taking into account the sensitivity toward speciated RO2 (organic peroxy) radicals, as recently reported from one of the participating instruments in the HO2 measurement mode, were 93% higher than the <span class="hlt">observations</span> made by the single instrument. Adding isomerization of isoprene peroxy radicals to the model increased OH and HO2(*) by 28% and 13% on average. Although these are still only 4% higher than the OH <span class="hlt">observations</span> made by one of the instruments, larger overestimations (42-70%) occurred with respect to the OH <span class="hlt">observations</span> made by the other three instruments. These model runs tend to underestimate <span class="hlt">observed</span> OH reactivity which may be explained by unmeasured hydrocarbon species. In the base run, the good agreement for the OH levels was retained when four different types of hydrocarbons were added as mixture to explain the missing OH reactivity. In the model run with isomerization of isoprene peroxy radicals, on the other hand, OH levels agreed to the ensemble of <span class="hlt">observations</span> only when unmeasured anthropogenic hydrocarbons was added at implausibly high concentrations, implying that the rates of the isomerization were not readily supported by the ensemble of radical <span class="hlt">observations</span>. The overprediction of the HO2(*) levels by the model occurred independently of the inclusion of the isoprene isomerization scheme, indicating that more loss processes for peroxy radicals were necessary to explain the <span class="hlt">observations</span>. One of the measurement days was characterized by low isoprene concentrations (~0.5 ppb) and OH reactivity that was well explained by the <span class="hlt">observed</span> species, especially before noon. For this selected <span class="hlt">period</span>, as opposed to the general behavior, the model tended to underestimate HO2(*). We found that this tendency is associated with high NOx concentrations, <span class="hlt">suggesting</span> that some HO2 production or regeneration processes under high NOx conditions were being overlooked; this might require revision of ozone production regimes.</p> <div class="credits"> <p class="dwt_author">Kanaya, Y.; Hofzumahaus, A.; Dorn, H.-P.; Brauers, T.; Fuchs, H.; Holland, F.; Rohrer, F.; Bohn, B.; Tillmann, R.; Wegener, R.; Wahner, A.; Kajii, Y.; Miyamoto, K.; Nishida, S.; Watanabe, K.; Yoshino, A.; Kubistin, D.; Martinez, M.; Rudolf, M.; Harder, H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">172</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015AMT.....8..649D"> <span id="translatedtitle">An overview of the lightning and atmospheric electricity <span class="hlt">observations</span> collected in southern France during the HYdrological cycle in Mediterranean EXperiment (HyMeX), Special <span class="hlt">Observation</span> <span class="hlt">Period</span> 1</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The PEACH project (Projet en Electricité Atmosphérique pour la Campagne HyMeX - the Atmospheric Electricity Project of the HyMeX Program) is the atmospheric electricity component of the Hydrology cycle in the Mediterranean Experiment (HyMeX) experiment and is dedicated to the <span class="hlt">observation</span> of both lightning activity and electrical state of continental and maritime thunderstorms in the area of the Mediterranean Sea. During the HyMeX SOP1 (Special <span class="hlt">Observation</span> <span class="hlt">Period</span>) from 5 September to 6 November 2012, four European operational lightning locating systems (ATDnet, EUCLID, LINET, ZEUS) and the HyMeX lightning mapping array network (HyLMA) were used to locate and characterize the lightning activity over the northwestern Mediterranean at flash, storm and regional scales. Additional research instruments like slow antennas, video cameras, microbarometer and microphone arrays were also operated. All these <span class="hlt">observations</span> in conjunction with operational/research ground-based and airborne radars, rain gauges and in situ microphysical records are aimed at characterizing and understanding electrically active and highly precipitating events over southeastern France that often lead to severe flash floods. Simulations performed with cloud resolving models like Meso-NH and Weather Research and Forecasting are used to interpret the results and to investigate further the links between dynamics, microphysics, electrification and lightning occurrence. Herein we present an overview of the PEACH project and its different instruments. Examples are discussed to illustrate the comprehensive and unique lightning data set, from radio frequency to acoustics, collected during the SOP1 for lightning phenomenology understanding, instrumentation validation, storm characterization and modeling.</p> <div class="credits"> <p class="dwt_author">Defer, E.; Pinty, J.-P.; Coquillat, S.; Martin, J.-M.; Prieur, S.; Soula, S.; Richard, E.; Rison, W.; Krehbiel, P.; Thomas, R.; Rodeheffer, D.; Vergeiner, C.; Malaterre, F.; Pedeboy, S.; Schulz, W.; Farges, T.; Gallin, L.-J.; Ortéga, P.; Ribaud, J.-F.; Anderson, G.; Betz, H.-D.; Meneux, B.; Kotroni, V.; Lagouvardos, K.; Roos, S.; Ducrocq, V.; Roussot, O.; Labatut, L.; Molinié, G.</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-02-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">173</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013JGRD..118.8426T"> <span id="translatedtitle">Meteorological and dust aerosol conditions over the western Saharan region <span class="hlt">observed</span> at Fennec Supersite-2 during the intensive <span class="hlt">observation</span> <span class="hlt">period</span> in June 2011</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The climate of the Sahara is relatively poorly <span class="hlt">observed</span> and understood, leading to errors in forecast model simulations. We describe <span class="hlt">observations</span> from the Fennec Supersite-2 (SS2) at Zouerate, Mauritania during the June 2011 Fennec Intensive <span class="hlt">Observation</span> <span class="hlt">Period</span>. These provide an improved basis for understanding and evaluating processes, models, and remote sensing. Conditions during June 2011 show a marked distinction between: (i) a "Maritime phase" during the early part of the month when the western sector of the Sahara experienced cool northwesterly maritime flow throughout the lower troposphere with shallow daytime boundary layers, very little dust uplift/transport or cloud cover. (ii) A subsequent "heat low" phase which coincided with a marked and rapid westward shift in the Saharan heat low towards its mid-summer climatological position and advection of a deep hot, dusty air layer from the central Sahara (the "Saharan residual layer"). This transition affected the entire western-central Sahara. Dust advected over SS2 was primarily from episodic low-level jet (LLJ)-generated emission in the northeasterly flow around surface troughs. Unlike Fennec SS1, SS2 does not often experience cold pools from moist convection and associated dust emissions. The diurnal evolution at SS2 is strongly influenced by the Atlantic inflow (AI), a northwesterly flow of shallow, cool and moist air propagating overnight from coastal West Africa to reach SS2 in the early hours. The AI cools and moistens the western Saharan and weakens the nocturnal LLJ, limiting its dust-raising potential. We quantify the ventilation and moistening of the western flank of the Sahara by (i) the large-scale flow and (ii) the regular nocturnal AI and LLJ mesoscale processes.</p> <div class="credits"> <p class="dwt_author">Todd, M. C.; Allen, C. J. T.; Bart, M.; Bechir, M.; Bentefouet, J.; Brooks, B. J.; Cavazos-Guerra, C.; Clovis, T.; Deyane, S.; Dieh, M.; Engelstaedter, S.; Flamant, C.; Garcia-Carreras, L.; Gandega, A.; Gascoyne, M.; Hobby, M.; Kocha, C.; Lavaysse, C.; Marsham, J. H.; Martins, J. V.; McQuaid, J. B.; Ngamini, J. B.; Parker, D. J.; Podvin, T.; Rocha-Lima, A.; Traore, S.; Wang, Y.; Washington, R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-08-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">174</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015OcDyn..65..173C"> <span id="translatedtitle"><span class="hlt">Observed</span> year-to-year sea surface salinity variability in the Bay of Bengal during the 2009-2014 <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The present study describes the <span class="hlt">observed</span> sea surface salinity (SSS) interannual variability in the Bay of Bengal over the 2009-2014 <span class="hlt">period</span>. It is based on an original compilation of all available in situ SSS <span class="hlt">observations</span> in that region, assembled in a 2°-resolution trimonthly gridded field. We find that year-to-year SSS variability is particularly strong in the north-eastern part of the bay. Over recent years, this variability takes the form of two successive and opposite phases: a saltening phase from mid-2009 to late 2010, immediately followed by a freshening phase from late 2010 to late 2011. The typical magnitude of each anomalous spell is about one in the practical salinity scale, making this area one of the most variable of the tropical oceans at interannual timescales. A simple mixed-layer salt budget indicates that year-to-year large-scale SSS variability in the Northern Bay of Bengal is primarily driven by freshwater flux variability with a correlation of 0.68, with rather independent contributions from precipitation and river run-off. The oceanic surface circulation variability contributes less systematically to the large-scale SSS evolution in the Northern Bay of Bengal over the entire record with a correlation of 0.13, despite a strong contribution at times, in particular, during the 2011 positive Indian Ocean Dipole (IOD) freshening.</p> <div class="credits"> <p class="dwt_author">Chaitanya, Akurathi Venkata Sai; Durand, Fabien; Mathew, Simi; Gopalakrishna, Vissa Venkata; Papa, Fabrice; Lengaigne, Matthieu; Vialard, Jerome; Kranthikumar, Chanda; Venkatesan, R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-02-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">175</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/1107.1620.pdf"> <span id="translatedtitle">Quasi <span class="hlt">periodic</span> oscillations of solar active regions in connection with their flare activity - NoRH <span class="hlt">observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">The sunspot-associated sources at the frequency of 17 GHz give information on plasma parameters in the regions of magnetic field about B=2000 G at the level of the chromosphere-corona transition region. The <span class="hlt">observations</span> of short <span class="hlt">period</span> (from 1 to 10 minutes) oscillations in sunspots reflect propagation of magnetohydrodynamic (MHD) waves in the magnetic flux tubes of the sunspots. We investigate the oscillation parameters in active regions in connection with their flare activity. We confirm the existence of a link between the oscillation spectrum and flare activity. We find differences in the oscillations between pre-flare and post-flare phases. In particular, we demonstrate a case of powerful three-minute oscillations that start just before the burst. This event is similar to the cases of the precursors investigated by Sych, R. et al. (Astron. Astrophys., vol.505, p.791, 2009). We also found well-defined eight-minute oscillations of microwave emission from sunspot. We interpret our <span class="hlt">observations</span> in terms of a ...</p> <div class="credits"> <p class="dwt_author">Abramov-Maximov, Vladimir E; Shibasaki, Kiyoto</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">176</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3890821"> <span id="translatedtitle">Direct <span class="hlt">observation</span> of single stationary-phase bacteria reveals a surprisingly long <span class="hlt">period</span> of constant protein production activity</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Exponentially growing bacteria are rarely found in the wild, as microorganisms tend to spend most of their lifetime at stationary phase. Despite this general prevalence of stationary-phase bacteria, they are as yet poorly characterized. Our goal was to quantitatively study this phase by direct <span class="hlt">observation</span> of single bacteria as they enter into stationary phase and by monitoring their activity over several days during growth arrest. For this purpose, we devised an experimental procedure for starving single Escherichia coli bacteria in microfluidic devices and measured their activity by monitoring the production rate of fluorescent proteins. When amino acids were the sole carbon source, the production rate decreased by an order of magnitude upon entry into stationary phase. We found that, even while growth-arrested, bacteria continued to produce proteins at a surprisingly constant rate over several days. Our identification of this newly <span class="hlt">observed</span> <span class="hlt">period</span> of constant activity in nongrowing cells, designated as constant activity stationary phase, makes possible the conduction of assays that require constant protein expression over time, and are therefore difficult to perform under exponential growth conditions. Moreover, we show that exogenous protein expression bears no fitness cost on the regrowth of the population when starvation ends. Further characterization of constant activity stationary phase—a phase where nongrowing bacteria can be quantitatively studied over several days in a reproducible manner—should contribute to a better understanding of this ubiquitous but overlooked physiological state of bacteria in nature. PMID:24344288</p> <div class="credits"> <p class="dwt_author">Gefen, Orit; Fridman, Ofer; Ronin, Irine; Balaban, Nathalie Q.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">177</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015GeoRL..42..282W"> <span id="translatedtitle">Some <span class="hlt">observations</span> regarding the thermal flux from Earth's erupting volcanoes for the <span class="hlt">period</span> of 2000 to 2014</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">present satellite measurements of the thermal flux <span class="hlt">observed</span> from 95 active volcanoes, based on <span class="hlt">observations</span> made daily over the past 15 years by NASA's Terra and Aqua Moderate Resolution Imaging Spectroradiometer sensors. Excursions from an apparent baseline level of thermal emission are attributable to episodic lava-flow-forming eruptions. Highest average intensity was associated with the July 2001 eruption of Etna, Italy, which radiated an average of 2.5 × 109 W over 23 days. However, recent fissure eruptions in the Afar Rift have attained higher average intensities of 2.4-4.4 × 109 W, albeit for days, not weeks. The largest magnitude eruption was the ongoing eruption of Bardarbunga, Iceland, which radiated 2.6 × 1016 J. K?lauea, Hawai'i, has radiated the most energy since 2000, although the lava lake at Nyiragongo, Democratic Republic of Congo, comes a close second. Time series analysis reveals evidence for <span class="hlt">periodicity</span> in radiant flux at some volcanoes but not at others.</p> <div class="credits"> <p class="dwt_author">Wright, Robert; Blackett, Matthew; Hill-Butler, Charley</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">178</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013EGUGA..15.9814R"> <span id="translatedtitle">Far Eastern Pacific Fresh Pool surface salinity variability <span class="hlt">observed</span> by SMOS and Aquarius sensors over the <span class="hlt">period</span> 2010-2012</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The seasonal and interannual variability of the Sea Surface Salinity (SSS) deduced from SMOS and Aquarius/SAC-D satellite missions are analyzed over the <span class="hlt">period</span> 2010-2012 in the Far Eastern Pacific Fresh Pool. The lowest values of salinity in surface layers (<33) in the tropical Pacific Ocean are found in this region of intense precipitation, associated with the northward migration of the Intertropical Convergence Zone (ITCZ) over Central America (Alory et al., 2012). During the boreal winter, as the ITCZ moves southward, the north-easterly Panama gap wind creates a south-westward jet-like current in its path with a dipole of Ekman pumping/eddies on its flanks. As a result, upwelling in the Panama Bight brings cold and salty waters to the surface which erode the fresh pool on its eastern side while surface currents stretch the pool westward. The present study focuses on the fresh pool patterns ranging from the seasonal and interannual variability over the last 3 year <span class="hlt">period</span>. Each year, satellite SSS products reveal the erosion of the fresh pool by the Panama upwelling. Compared to the SSS climatology from the World Ocean Atlas, satellite SSS data systematically exhibit fresher surface water (by ~0.5 to 1 unit in SSS) just after the occurrence of the maximum SSS reached in the region during the Panama upwelling events (April-May). Using Tropical Rainfall Measuring Mission (TRMM) data, we found that these fresh anomalies coincide with local excess precipitation. Moreover, except during the boreal winter 2011, saltier surface waters than in the climatology were <span class="hlt">observed</span> during the intensification phase of the Panama upwelling events (Fev-March). Using ASCAT sensor surface winds, TRMM data, surface current deduced from altimeter data combined with the satellite SSS, the study will analyze how these <span class="hlt">observed</span> SSS anomalies could be related to the interannual variability in the dominant physical mechanisms involved in the freshpool dynamics. A particular focus will be set on the consistency between SMOS and Aquarius <span class="hlt">observations</span> and on the potential role of the surface freshwater induced-barrier layer processes in modulating the interannual signals.</p> <div class="credits"> <p class="dwt_author">Reul, Nicolas; Alory, Gael; Maes, Christophe; Illig, Serena; Chapron, Bertrand</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">179</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012ACP....12.2567K"> <span id="translatedtitle">Comparisons of <span class="hlt">observed</span> and modeled OH and HO2 concentrations during the ambient measurement <span class="hlt">period</span> of the HOxComp field campaign</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">A photochemical box model constrained by ancillary <span class="hlt">observations</span> was used to simulate OH and HO2 concentrations for three days of ambient <span class="hlt">observations</span> during the HOxComp field campaign held in Jülich, Germany in July 2005. Daytime OH levels <span class="hlt">observed</span> by four instruments were fairly well reproduced to within 33% by a base model run (Regional Atmospheric Chemistry Mechanism with updated isoprene chemistry adapted from Master Chemical Mechanism ver. 3.1) with high R2 values (0.72-0.97) over a range of isoprene (0.3-2 ppb) and NO (0.1-10 ppb) mixing ratios. Daytime HO2(*) levels, reconstructed from the base model results taking into account the sensitivity toward speciated RO2 (organic peroxy) radicals, as recently reported from one of the participating instruments in the HO2 measurement mode, were 93% higher than the <span class="hlt">observations</span> made by the single instrument. This also indicates an overprediction of the HO2 to OH recycling. Together with the good model-measurement agreement for OH, it implies a missing OH source in the model. Modeled OH and HO2(*) could only be matched to the <span class="hlt">observations</span> by addition of a strong unknown loss process for HO2(*) that recycles OH at a high yield. Adding to the base model, instead, the recently proposed isomerization mechanism of isoprene peroxy radicals (Peeters and Müller, 2010) increased OH and HO2(*) by 28% and 13% on average. Although these were still only 4% higher than the OH <span class="hlt">observations</span> made by one of the instruments, larger overestimations (42-70%) occurred with respect to the OH <span class="hlt">observations</span> made by the other three instruments. The overestimation in OH could be diminished only when reactive alkanes (HC8) were solely introduced to the model to explain the missing fraction of <span class="hlt">observed</span> OH reactivity. Moreover, the overprediction of HO2(*) became even larger than in the base case. These analyses imply that the rates of the isomerization are not readily supported by the ensemble of radical <span class="hlt">observations</span>. One of the measurement days was characterized by low isoprene concentrations (∼0.5 ppb) and OH reactivity that was well explained by the <span class="hlt">observed</span> species, especially before noon. For this selected <span class="hlt">period</span>, as opposed to the general behavior, the model tended to underestimate HO2(*). We found that this tendency is associated with high NOx concentrations, <span class="hlt">suggesting</span> that some HO2 production or regeneration processes under high NOx conditions were being overlooked; this might require revision of ozone production regimes.</p> <div class="credits"> <p class="dwt_author">Kanaya, Y.; Hofzumahaus, A.; Dorn, H.-P.; Brauers, T.; Fuchs, H.; Holland, F.; Rohrer, F.; Bohn, B.; Tillmann, R.; Wegener, R.; Wahner, A.; Kajii, Y.; Miyamoto, K.; Nishida, S.; Watanabe, K.; Yoshino, A.; Kubistin, D.; Martinez, M.; Rudolf, M.; Harder, H.; Berresheim, H.; Elste, T.; Plass-Dülmer, C.; Stange, G.; Kleffmann, J.; Elshorbany, Y.; Schurath, U.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">180</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22047913"> <span id="translatedtitle">TIME DELAYS IN QUASI-<span class="hlt">PERIODIC</span> PULSATIONS <span class="hlt">OBSERVED</span> DURING THE X2.2 SOLAR FLARE ON 2011 FEBRUARY 15</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We report <span class="hlt">observations</span> of quasi-<span class="hlt">periodic</span> pulsations (QPPs) during the X2.2 flare of 2011 February 15, <span class="hlt">observed</span> simultaneously in several wavebands. We focus on fluctuations on timescale 1-30 s and find different time lags between different wavebands. During the impulsive phase, the Reuven Ramaty High Energy Solar Spectroscopic Imager channels in the range 25-100 keV lead all the other channels. They are followed by the Nobeyama RadioPolarimeters at 9 and 17 GHz and the extreme-ultraviolet (EUV) channels of the Euv SpectroPhotometer (ESP) on board the Solar Dynamic Observatory. The zirconium and aluminum filter channels of the Large Yield Radiometer on board the Project for On-Board Autonomy satellite and the soft X-ray (SXR) channel of ESP follow. The largest lags occur in <span class="hlt">observations</span> from the Geostationary Operational Environmental Satellite, where the channel at 1-8 A leads the 0.5-4 A channel by several seconds. The time lags between the first and last channels is up to Almost-Equal-To 9 s. We identified at least two distinct time intervals during the flare impulsive phase, during which the QPPs were associated with two different sources in the Nobeyama RadioHeliograph at 17 GHz. The radio as well as the hard X-ray channels showed different lags during these two intervals. To our knowledge, this is the first time that time lags are reported between EUV and SXR fluctuations on these timescales. We discuss possible emission mechanisms and interpretations, including flare electron trapping.</p> <div class="credits"> <p class="dwt_author">Dolla, L.; Marque, C.; Seaton, D. B.; Dominique, M.; Berghmans, D.; Cabanas, C.; De Groof, A.; Verdini, A.; West, M. J.; Zhukov, A. N. [Solar-Terrestrial Center of Excellence, Royal Observatory of Belgium, Avenue Circulaire 3, B-1180 Brussels (Belgium); Van Doorsselaere, T. [Centrum voor Plasma-Astrofysica, Department of Mathematics, KULeuven, Celestijnenlaan 200B bus 2400, B-3001 Leuven (Belgium); Schmutz, W. [Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center, Davos Dorf (Switzerland); Zender, J., E-mail: dolla@sidc.be [European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ Noordwijk (Netherlands)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-04-10</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_8");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a 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showDiv("page_11");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">181</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012A%26A...539A.135S"> <span id="translatedtitle">The quasi-biennial <span class="hlt">periodicity</span> (QBP) in velocity and intensity helioseismic <span class="hlt">observations</span>. The seismic QBP over solar cycle 23</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Aims: We looked for signatures of quasi-biennial <span class="hlt">periodicity</span> (QBP) over different phases of solar cycle by means of acoustic modes of oscillation. Low-degree p-mode frequencies are shown to be sensitive to changes in magnetic activity due to the global dynamo. Recently there has been reported evidence of two-year variations in p-mode frequencies. Methods: Long high-quality helioseismic data are provided by BiSON (Birmingham Solar Oscillation Network), GONG (Global Oscillation Network Group), GOLF (Global Oscillation at Low Frequency) and VIRGO (Variability of Solar IRradiance and Gravity Oscillation) instruments. We determined the solar cycle changes in p-mode frequencies for spherical degree ? = 0, 1, 2 with their azimuthal components in the frequency range 2.5 mHz ? ? ? 3.5 mHz. Results: We found signatures of QBP at all levels of solar activity in the modes more sensitive to higher latitudes. The signal strength increases with latitude and the equatorial component also seems to be modulated by the 11-year envelope. Conclusions: The persistent nature of the seismic QBP is not <span class="hlt">observed</span> in the surface activity indices, where mid-term variations are found only from time to time and mainly in <span class="hlt">periods</span> of high activity. This feature, together with the latitudinal dependence, provides more evidence of a mechanism that is almost independent and different from the one that brings the active regions up to the surface. Therefore, these findings can be used to provide more constraints on dynamo models that consider a further cyclic component on top of the 11-year cycle.</p> <div class="credits"> <p class="dwt_author">Simoniello, R.; Finsterle, W.; Salabert, D.; García, R. A.; Turck-Chièze, S.; Jiménez, A.; Roth, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">182</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/19597869"> <span id="translatedtitle"><span class="hlt">Observations</span> of atmospheric nitrogen and phosphorus deposition during the <span class="hlt">period</span> of algal bloom formation in northern Lake Taihu, China.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Cyanobacterial blooms in Lake Taihu occurred at the end of April 2007 and had crucial impacts on the livelihood of millions of people living there. Excessive nutrients may promote bloom formation. Atmospheric nitrogen (N) and phosphorus (P) deposition appears to play an important role in algal bloom formation. Bulk deposition and rain water samples were collected respectively from May 1 to November 30, 2007, the <span class="hlt">period</span> of optimal algal growth, to measure the bulk atmospheric deposition rate, wet deposition rate, and dry deposition rate for total nitrogen (TN; i.e., all species of nitrogen), and total phosphorus (TP; i.e., all species of phosphorus), in northern Lake Taihu, China. The trends of the bulk atmospheric deposition rate for TN and the wet deposition rate for TN showed double peaks during the <span class="hlt">observation</span> <span class="hlt">period</span> and distinct influence with plum rains and typhoons. Meanwhile, monthly bulk atmospheric deposition rates for TP showed little influence of annual precipitation. However, excessive rain may lead to high atmospheric N and P deposition rates. In bulk deposition samples, the average percentage of total dissolved nitrogen accounting for TN was 91.2% and changed little with time. However, the average percentage of total dissolved phosphorus accounting for TP was 65.6% and changed substantially with time. Annual bulk atmospheric deposition rates of TN and TP during 2007 in Lake Taihu were estimated to be 2,976 and 84 kg km(-2) a(-1), respectively. The results showed decreases of 34.4% and 78.7%, respectively, compared to 2002-2003. Annual bulk deposition load of TN for Lake Taihu was estimated at 6,958 t a(-1) in 2007 including 4,642 t a(-1) of wet deposition, lower than the values obtained in 2002-2003. This may be due to measures taken to save energy and emission control regulations in the Yangtze River Delta. Nevertheless, high atmospheric N and P deposition loads helped support cyanobacterial blooms in northern Lake Taihu during summer and autumn, the <span class="hlt">period</span> of favorable algal growth. PMID:19597869</p> <div class="credits"> <p class="dwt_author">Zhai, Shuijing; Yang, Longyuan; Hu, Weiping</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-09-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">183</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009EnMan..44..542Z"> <span id="translatedtitle"><span class="hlt">Observations</span> of Atmospheric Nitrogen and Phosphorus Deposition During the <span class="hlt">Period</span> of Algal Bloom Formation in Northern Lake Taihu, China</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Cyanobacterial blooms in Lake Taihu occurred at the end of April 2007 and had crucial impacts on the livelihood of millions of people living there. Excessive nutrients may promote bloom formation. Atmospheric nitrogen (N) and phosphorus (P) deposition appears to play an important role in algal bloom formation. Bulk deposition and rain water samples were collected respectively from May 1 to November 30, 2007, the <span class="hlt">period</span> of optimal algal growth, to measure the bulk atmospheric deposition rate, wet deposition rate, and dry deposition rate for total nitrogen (TN; i.e., all species of nitrogen), and total phosphorus (TP; i.e., all species of phosphorus), in northern Lake Taihu, China. The trends of the bulk atmospheric deposition rate for TN and the wet deposition rate for TN showed double peaks during the <span class="hlt">observation</span> <span class="hlt">period</span> and distinct influence with plum rains and typhoons. Meanwhile, monthly bulk atmospheric deposition rates for TP showed little influence of annual precipitation. However, excessive rain may lead to high atmospheric N and P deposition rates. In bulk deposition samples, the average percentage of total dissolved nitrogen accounting for TN was 91.2% and changed little with time. However, the average percentage of total dissolved phosphorus accounting for TP was 65.6% and changed substantially with time. Annual bulk atmospheric deposition rates of TN and TP during 2007 in Lake Taihu were estimated to be 2,976 and 84 kg km-2 a-1, respectively. The results showed decreases of 34.4% and 78.7%, respectively, compared to 2002-2003. Annual bulk deposition load of TN for Lake Taihu was estimated at 6,958 t a-1 in 2007 including 4,642 t a-1 of wet deposition, lower than the values obtained in 2002-2003. This may be due to measures taken to save energy and emission control regulations in the Yangtze River Delta. Nevertheless, high atmospheric N and P deposition loads helped support cyanobacterial blooms in northern Lake Taihu during summer and autumn, the <span class="hlt">period</span> of favorable algal growth.</p> <div class="credits"> <p class="dwt_author">Zhai, Shuijing; Yang, Longyuan; Hu, Weiping</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-09-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">184</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015AJ....149...25H"> <span id="translatedtitle">Pulsations and <span class="hlt">Period</span> Changes of the Non-Blazhko RR Lyrae Variable Y Oct <span class="hlt">Observed</span> from Dome A, Antarctica</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">During the operation of the Chinese Small Telescope Array (CSTAR) in Dome A of Antarctica in the years 2008, 2009, and 2010, large amounts of photometric data have been obtained for variable stars in the CSTAR field. We present here the study of one of six RR Lyrae variables, Y Oct, <span class="hlt">observed</span> with CSTAR in Dome A, Antarctica. Photometric data in the i band were obtained in 2008 and 2010, with a duty cycle (defined as the fraction of time representing scientifically available data to CSTAR <span class="hlt">observation</span> time) of about 44% and 52%, respectively. In 2009, photometric data in the g and r bands were gathered for this star, with a duty cycle of 65% and 60%, respectively. Fourier analysis of the data in the three bands only shows the fundamental frequency and its harmonics, which is characteristic of the non-Blazhko RR Lyrae variables. Values of the fundamental frequency and the amplitudes, as well as the total pulsation amplitude, are obtained from the data in the three bands separately. The amplitude of the fundamental frequency and the total pulsation amplitude in the g band are the largest, and those in the i band the smallest. Two-hundred fifty-one times of maximum are obtained from the three seasons of data, which are analyzed together with 38 maximum times provided in the GEOS RR Lyrae database. A <span class="hlt">period</span> change rate of -0.96 ± 0.07 days Myr-1 is then obtained, which is a surprisingly large negative value. Based on relations available in the literature, the following physical parameters are derived: [Fe/H] = -1.41 ± 0.14, MV = 0.696 ± 0.014 mag, V-K = 1.182 ± 0.028 mag, log {{T}eff} = 3.802 ± 0.003 K, log g = 2.705 ± 0.004, log L/{{L}? } = 1.625 ± 0.013, and log M/{{M}? } = -0.240 ± 0.019.</p> <div class="credits"> <p class="dwt_author">Huang, Zhihua; Fu, Jianning; Zong, Weikai; Wang, Lingzhi; Macri, Lucas M.; Wang, Lifan; Ashley, Michael C. B.; Cui, Xiangqun; Feng, Long-Long; Gong, Xuefei; Lawrence, Jon S.; Liu, Qiang; Luong-Van, Daniel; Pennypacker, Carl R.; Yang, Huigen; Yuan, Xiangyan; York, Donald; Xu, Zhou; Zhu, Zhenxi; Zhu, Zonghong</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">185</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2003HESS....7..877B"> <span id="translatedtitle">Hydrometeorological aspects of the Real-Time Ultrafinescale Forecast Support during the Special <span class="hlt">Observing</span> <span class="hlt">Period</span> of the MAP*</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">During the Special <span class="hlt">Observation</span> <span class="hlt">Period</span> (SOP, 7 September-15 November, 1999) of the Mesoscale Alpine Programme (MAP), the Canadian Mesoscale Compressible Community Model (MC2) was run in real time at a horizontal resolution of 3 km on a computational domain of 350?300?50 grid points, covering the whole of the Alpine region. The WATFLOOD model was passively coupled to the MC2; the former is an integrated set of computer programs to forecast flood flows, using all available data, for catchments with response times ranging from one hour to several weeks. The unique aspect of this contribution is the operational application of numerical weather prediction data to forecast flows over a very large, multinational domain. An overview of the system performance from the hydrometeorological aspect is presented, mostly for the real-time results, but also from subsequent analyses. A streamflow validation of the precipitation is included for large basins covering upper parts of the Rhine and the Rhone, and parts of the Po and of the Danube. In general, the MC2/WATFLOOD model underestimated the total runoff because of the under-prediction of precipitation by MC2 during the MAP SOP. After the field experiment, a coding error in the cloud microphysics scheme of MC2 explains this underestimation to a large extent. A sensitivity study revealed that the simulated flows reproduce the major features of the <span class="hlt">observed</span> flow record for most of the flow stations. The experiment was considered successful because two out of three possible flood events in the Swiss-Italian border region were predicted correctly by data from the numerical weather models linked to the hydrological model and no flow events were missed. This study has demonstrated that a flow forecast from a coupled atmospheric-hydrological model can serve as a useful first alert and quantitative forecast.</p> <div class="credits"> <p class="dwt_author">Benoit, R.; Kouwen, N.; Yu, W.; Chamberland, S.; Pellerin, P.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">186</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20010074719&hterms=great+falls+park&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dgreat%2Bfalls%2Bpark"> <span id="translatedtitle">Comparison of Columnar Water Vapor Measurements During The Fall 1997 ARM Intensive <span class="hlt">Observation</span> <span class="hlt">Period</span>: Solar Transmittance Methods</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">In the fall of 1997, during an Intensive <span class="hlt">Observation</span> <span class="hlt">Period</span> (IOP), the Atmospheric Radiation Measurement (ARM) program conducted a study of water vapor abundance measurement at its Southern Great Plains (SGP) site. Among a large number of instruments, four sun-tracking radiometers were present to measure the columnar water vapor (CWV). All four solar radiometers retrieve CWV by measuring total solar transmittance in the 0.94-gm water vapor absorption band and subtracting contributions due to Rayleigh, ozone and aerosol transmittances. The aerosol optical depth comparisons among the same four radiometers has been presented elsewhere (Geophys. Res. Lett., 26, 17, 2725-2728, 1999). We have used three different methods to retrieve CWV. In a first round of comparison no attempt was made to standardize on the same radiative transfer model and its underlying water vapor spectroscopy. In the second round of comparison we used the same line-by-line code (which includes recently corrected H2O spectroscopy) to retrieve CAN from all four suntracking radiometers. This decreased the mean CWV by 8% or 13%. The spread of 8% in the solar radiometer results found when using the same model is an indication of the other-than-model uncertainties involved in determining CWV from solar transmittance measurements with current instrumentation.</p> <div class="credits"> <p class="dwt_author">Schmid, B.; Michalsky, J. J.; Slater, D. W.; Barnard, J. C.; Halthore, R. N.; Liljegren, J. C.; Holben, B. N.; Eck, T. F.; Livingston, J. M.; Russell, P. B.</p> <p class="dwt_publisher"></p> <p class="publishDate">2000-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">187</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/263553"> <span id="translatedtitle">Remote Cloud Sensing Intensive <span class="hlt">Observation</span> <span class="hlt">Period</span> (RCS-IOP) millimeter-wave radar calibration and data intercomparison</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">During April 1994, the University of Massachusetts (UMass) and the Pennsylvania State University (Penn State) fielded two millimeter-wave atmospheric radars in the Atmospheric Radiation Measurement Remote Cloud Sensing Intensive Operation <span class="hlt">Period</span> (RCS-IOP) experiment. The UMass Cloud Profiling Radar System (CPRS) operates simultaneously at 33.12 GHz and 94.92 GHz through a single antenna. The Penn State radar operates at 93.95 GHz and has separate transmitting and receiving antennas. The two systems were separated by approximately 75 meters and simultaneously <span class="hlt">observed</span> a variety of cloud types at verticle incidence over the course of the experiment. This abstract presents some initial results from our calibration efforts. An absolute calibration of the UMass radar was made from radar measurements of a trihedral corner reflector, which has a known radar cross-section. A relative calibration of between the Penn State and UMass radars is made from the statistical comparison of zenith pointing measurements of low altitude liquid clouds. Attenuation is removed with the aid of radiosonde data, and the difference in the calibration between the UMass and Penn State radars is determined by comparing the ratio of 94-GHz and 95-GHz reflectivity values to a model that accounts for parallax effects of the two antennas used in the Penn State system.</p> <div class="credits"> <p class="dwt_author">Sekelsky, S.M.; Firda, J.M.; McIntosh, R.E. [Univ. of Massachusetts, Amherst, MA (United States)] [and others</p> <p class="dwt_publisher"></p> <p class="publishDate">1996-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">188</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013EGUGA..15.8375S"> <span id="translatedtitle">The HyMeX Special <span class="hlt">Observation</span> <span class="hlt">Period</span> in Central Italy: precipitation measurements, retrieval techniques and preliminary results</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The Mediterranean area concentrates the major natural risks related to the water cycle, including heavy precipitation and flash-flooding during the fall season. The capability to predict such high-impact events remains weak because of the contribution of very fine-scale processes and their non-linear interactions with the larger scale processes. These societal and science issues motivate the HyMeX (Hydrological cycle in the Mediterranean Experiment, http://www.hymex.org/) experimental programme. HyMeX aims at a better quantification and understanding of the water cycle in the Mediterranean with emphasis on intense events. The <span class="hlt">observation</span> strategy of HyMEX is organized in a long-term (4 years) Enhanced <span class="hlt">Observation</span> <span class="hlt">Periods</span> (EOP) and short-term (2 months) Special <span class="hlt">Observation</span> <span class="hlt">Periods</span> (SOP). HyMEX has identified 3 main Mediterranean target areas: North-West (NW), Adriatic (A) and South-East (SE). Within each target area several hydrometeorological sites for heavy rainfall and flash flooding have been set up. The hydrometeorological site in Central Italy (CI) is interested by both western and eastern fronts coming from the Atlantic Ocean and Siberia, respectively. Orographic precipitations play an important role due to the central Apennine range, which reaches nearly 3000 m (Gran Sasso peak). Moreover, convective systems commonly develop in CI during late summer and beginning of autumn, often causing localized hailstorms with cluster organized cells. Western fronts may heavily hit the Tiber basin crossing large urban areas (Rome), whereas eastern fronts can cause flash floods along the Adriatic coastline. Two major basins are involved within CI region: Tiber basin (1000 km long) and its tributary Aniene and the Aterno-Pescara basin (300 km long). The first HyMeX SOP1.1 was carried out from Sept. till Nov. 2012 in the NW target area. The Italian SOP1.1 was coordinated by the Centre of Excellence CETEMPS, University of L'Aquila, a city located in the CI heart. The CI area was covered by a uniquely dense meteorological instrumentation thanks to a synergy between Italian institutions and NASA-GSFC. The following RADARs were operated: a Doppler single-polarization C-band radar located at Mt. Midia; the Polar 55C Doppler dual-polarization C-band radar located in Rome; a Doppler C-band polarimetric radar located at Il Monte (Abruzzo); a polarimetric X-band mini-radar in L'Aquila; a polarimetric X-band portable mini-radar in Rome; a single-polarization X-band mini-radar in Rome. DISDROMETERs were also deployed: 4 Parsivel optical disdrometers in Rome (at Sapienza, CNR-ISAC and CNR-INSEAN); 1 2D-video disdrometer in Rome; 3 Parsivels optical disdrometer respectively in L'Aquila (Abruzzo), Avezzano (Abruzzo) and Pescara (Abruzzo). Other INSTRUMENTS were available: 1 K-band vertically-pointing micro rain-radar (MRR), 2 Pludix X-band disdrometers, 1 VLF lightining sensor, 1 microwave radiometer at 23-31 GHz in Rome (at Sapienza); the raingauge network with more than 200 stations in Central Italy. Three overpasses in CI were also performed by the Falcon 20 aircraft equipped with the 95GHz cloud radar RASTA. Analysis of the SOP1.1 main events in CI will be described by focusing on the raindrop size distribution statistics and its geographical variability. Intercomparison of rainfall estimates from disdrometers, raingauges and radars will be illustrated with the aim to provide a quality-controlled and physically consistent rainfall dataset for meteorological modeling validation and assimilation purposes.</p> <div class="credits"> <p class="dwt_author">Silvio Marzano, Frank; Baldini, Luca; Picciotti, Errico; Colantonio, Matteo; Barbieri, Stefano; Di Fabio, Saverio; Montopoli, Mario; Vulpiani, Gianfranco; Roberto, Nicoletta; Adirosi, Elisa; Gorgucci, Eugenio; Anagnostou, Marios N.; Kalogiros, John; Anagnostou, Emmanouil N.; Ferretti, Rossella; Gatlin, Patrick.; Wingo, Matt; Petersen, Walt</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">189</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3852097"> <span id="translatedtitle">Change in heart rate variability precedes the occurrence of <span class="hlt">periodic</span> leg movements during sleep: an <span class="hlt">observational</span> study</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Background Several reports have described that individual <span class="hlt">periodic</span> leg movements during sleep (PLMS) activities are associated with autonomic nervous system activity occurring shortly before each PLMS activity. Nevertheless, no study has investigated dynamic changes of autonomic nervous system activity before the onset of PLMS. This study detected changes in heart rate variability (HRV) at the onset of the <span class="hlt">period</span> with PLMS using complex demodulation method. Methods This study enrolled 14 patients diagnosed as having idiopathic PLMS disorder (PLMD). In <span class="hlt">periods</span> with and without PLMS during sleep stage 2, HRV-related variables and the spectral power of fluctuation of a high frequency (HF) band (FHFB) were analyzed and compared. The changes of those parameters during transition from the <span class="hlt">period</span> without PLMS to that with PLMS were explored. Results Spectral power in the low frequency (LF) band and very low frequency (VLF) band were higher in the <span class="hlt">period</span> with PLMS. Additionally, the average frequency in FHFB was higher. The frequency in this band fluctuated during the <span class="hlt">period</span> with PLMS with remarkable elevation of FHFB. Moreover, spectral powers in FHFB, LF, and VLF were remarkably elevated shortly before the beginning of the <span class="hlt">period</span> with PLMS (FHFB, -65 s; LF, -53 s; and VLF, -45 s). Conclusions Elevation of sympathetic nervous system activity and mean frequency fluctuation in an HF band can occur several tens of seconds before the <span class="hlt">period</span> with PLMS. Dynamic changes in the autonomic nervous system activity might be related to the vulnerability to PLMS occurrence during the night. PMID:24093585</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">190</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014ACP....14.5807Z"> <span id="translatedtitle">Estimating Asian terrestrial carbon fluxes from CONTRAIL aircraft and surface CO2 <span class="hlt">observations</span> for the <span class="hlt">period</span> 2006-2010</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Current estimates of the terrestrial carbon fluxes in Asia show large uncertainties particularly in the boreal and mid-latitudes and in China. In this paper, we present an updated carbon flux estimate for Asia ("Asia" refers to lands as far west as the Urals and is divided into boreal Eurasia, temperate Eurasia and tropical Asia based on TransCom regions) by introducing aircraft CO2 measurements from the CONTRAIL (Comprehensive <span class="hlt">Observation</span> Network for Trace gases by Airline) program into an inversion modeling system based on the CarbonTracker framework. We estimated the averaged annual total Asian terrestrial land CO2 sink was about -1.56 Pg C yr-1 over the <span class="hlt">period</span> 2006-2010, which offsets about one-third of the fossil fuel emission from Asia (+4.15 Pg C yr-1). The uncertainty of the terrestrial uptake estimate was derived from a set of sensitivity tests and ranged from -1.07 to -1.80 Pg C yr-1, comparable to the formal Gaussian error of ±1.18 Pg C yr-1 (1-sigma). The largest sink was found in forests, predominantly in coniferous forests (-0.64 ± 0.70 Pg C yr-1) and mixed forests (-0.14 ± 0.27 Pg C yr-1); and the second and third large carbon sinks were found in grass/shrub lands and croplands, accounting for -0.44 ± 0.48 Pg C yr-1 and -0.20 ± 0.48 Pg C yr-1, respectively. The carbon fluxes per ecosystem type have large a priori Gaussian uncertainties, and the reduction of uncertainty based on assimilation of sparse <span class="hlt">observations</span> over Asia is modest (8.7-25.5%) for most individual ecosystems. The ecosystem flux adjustments follow the detailed a priori spatial patterns by design, which further increases the reliance on the a priori biosphere exchange model. The peak-to-peak amplitude of inter-annual variability (IAV) was 0.57 Pg C yr-1 ranging from -1.71 Pg C yr-1 to -2.28 Pg C yr-1. The IAV analysis reveals that the Asian CO2 sink was sensitive to climate variations, with the lowest uptake in 2010 concurrent with a summer flood and autumn drought and the largest CO2 sink in 2009 owing to favorable temperature and plentiful precipitation conditions. We also found the inclusion of the CONTRAIL data in the inversion modeling system reduced the uncertainty by 11% over the whole Asian region, with a large reduction in the southeast of boreal Eurasia, southeast of temperate Eurasia and most tropical Asian areas.</p> <div class="credits"> <p class="dwt_author">Zhang, H. F.; Chen, B. Z.; Machida, T.; Matsueda, H.; Sawa, Y.; Fukuyama, Y.; Langenfelds, R.; van der Schoot, M.; Xu, G.; Yan, J. W.; Cheng, M. L.; Zhou, L. X.; Tans, P. P.; Peters, W.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">191</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://math.la.asu.edu/~andrzej/teachold/419Spr02/sp10.pdf"> <span id="translatedtitle"><span class="hlt">Suggested</span> Problems A. Czygrinow</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary"><span class="hlt">Suggested</span> Problems Set 10 A. Czygrinow Department of Mathematics Arizona State University <span class="hlt">Suggested</span> Problems ­ p.1/9 #12;Problem 1 Show that in any tree any two nodes are connected by exactly one path Show that tree is a bipartite graph Show that any tree on ¡ nodes has ¡ ¢ £ arcs <span class="hlt">Suggested</span> Problems</p> <div class="credits"> <p class="dwt_author">Czygrinow, Andrzej</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">192</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=pearce&pg=5&id=EJ903423"> <span id="translatedtitle">The Life of <span class="hlt">Suggestions</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Using the notion of a <span class="hlt">suggestion</span>, or rather charting the life of <span class="hlt">suggestions</span>, this article considers the happenings of chance and embodiment as the "problems that got away." The life of <span class="hlt">suggestions</span> helps us to ask how connectivities are made, how desire functions, and how "immanence" rather than "transcendence" can open up the politics and ethics…</p> <div class="credits"> <p class="dwt_author">Pearce, Cathie</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">193</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015NHESS..15....1M"> <span id="translatedtitle">A new high-resolution BOLAM-MOLOCH suite for the SIMM forecasting system: assessment over two HyMeX intense <span class="hlt">observation</span> <span class="hlt">periods</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">High-resolution numerical models can be effective in monitoring and predicting natural hazards, especially when dealing with Mediterranean atmospheric and marine intense/severe events characterised by a wide range of interacting scales. The understanding of the key factors associated to these Mediterranean phenomena, and the usefulness of adopting high-resolution numerical models in their simulation, are among the aims of the international initiative HyMeX - HYdrological cycle in Mediterranean EXperiment. At the turn of 2013, two monitoring campaigns (SOPs - Special <span class="hlt">Observation</span> <span class="hlt">Periods</span>) were devoted to these issues. For this purpose, a new high-resolution BOlogna Limited Area Model-MOdello LOCale (BOLAM-MOLOCH) suite was implemented in the Institute for Environmental Protection and Research (ISPRA) hydro-meteo-marine forecasting system (SIMM - Sistema Idro-Meteo-Mare) as a possible alternative to the operational meteorological component based on the BOLAM model self-nested over two lower-resolution domains. The present paper provides an assessment of this new configuration of SIMM with respect to the operational one that was also used during the two SOPs. More in details, it investigates the forecast performance of these SIMM configurations during two of the Intense <span class="hlt">Observation</span> <span class="hlt">Periods</span> (IOPs) declared in the first SOP campaign. These IOPs were characterised by high precipitations and very intense and exceptional high waters over the northern Adriatic Sea (acqua alta). Concerning the meteorological component, the high-resolution BOLAM-MOLOCH forecasts are compared against the lower-resolution BOLAM forecasts over three areas - mostly corresponding to the Italian HyMeX hydrometeorological sites - using the rainfall <span class="hlt">observations</span> collected in the HyMeX database. Three-month categorical scores are also calculated for the MOLOCH model. Despite the presence of a slight positive bias of the MOLOCH model, the results show that the precipitation forecast turns out to improve with increasing resolution. In both SIMM configurations, the sea storm surge component is based on the same version of the Shallow water HYdrodynamic Finite Element Model (SHYFEM). Hence, it is evaluated the impact of the meteorological forcing provided by the two adopted BOLAM configurations on the SHYFEM forecasts for six tide-gauge stations. A benchmark for this part of the study is given by the performance of the SHYFEM model forced by the ECMWF IFS forecast fields. For this component, both BOLAM-SHYFEM configurations clearly outperform the benchmark. The results are, however, strongly affected by the predictability of the weather systems associated to the IOPs, thus <span class="hlt">suggesting</span> the opportunity to develop and test a time-lagged multi-model ensemble for the prediction of high storm surge events.</p> <div class="credits"> <p class="dwt_author">Mariani, S.; Casaioli, M.; Coraci, E.; Malguzzi, P.</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">194</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20030111483&hterms=periodic&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dperiodic"> <span id="translatedtitle"><span class="hlt">Observations</span> of <span class="hlt">Periodic</span> Comet 2P/Encke: Physical Properties of the Nucleus and First Visual-Wavelength Detection of Its Dust Trail</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">We are conducting an <span class="hlt">observational</span> program designed to determine the overall distributions of size, shape, rotation <span class="hlt">period</span>, and surface characteristics of cometary nuclei. Here, we present results from a study of the Jupiter- family comet 2P/Encke based on <span class="hlt">observations</span> from Steward Observatory's 2.3m Bok Telescope at Kitt Peak. This comet has been <span class="hlt">observed</span> extensively in the past and was one of the primary flyby targets of the recently failed CONTOUR mission.</p> <div class="credits"> <p class="dwt_author">Lowry, Stephen C.; Weissman, Paul R.; Sykes, Mark V.; Reach, William T.</p> <p class="dwt_publisher"></p> <p class="publishDate">2003-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">195</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19850064518&hterms=Epstein&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3DEpstein"> <span id="translatedtitle">Mercury - Thermal emission at radio wavelengths. I - 3.3- and 28-mm <span class="hlt">observed</span> brightness temperatures and <span class="hlt">periodicities</span> therein</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The thermal radio emission from Mercury at 3.3 mm and 28 mm was measured over a <span class="hlt">period</span> of several years, and the results of a statistical analysis of the data are reported. The disk-average brightness temperature is reported as a function of longitude, and other <span class="hlt">periodicities</span> are reported. The range of values of the thermophysical parameters is constrained by comparing the data with models.</p> <div class="credits"> <p class="dwt_author">Epstein, E. E.; Andrew, B. H.</p> <p class="dwt_publisher"></p> <p class="publishDate">1985-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">196</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013ACPD...1327597Z"> <span id="translatedtitle">Estimating Asian terrestrial carbon fluxes from CONTRAIL aircraft and surface CO2 <span class="hlt">observations</span> for the <span class="hlt">period</span> 2006 to 2010</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Current estimates of the terrestrial carbon fluxes in Asia ("Asia" refers to lands as far west as the Urals and is divided into Boreal Eurasia, Temperate Eurasia and tropical Asia based on TransCom regions) show large uncertainties particularly in the boreal and mid-latitudes and in China. In this paper, we present an updated carbon flux estimate for Asia by introducing aircraft CO2 measurements from the CONTRAIL (Comprehensive <span class="hlt">Observation</span> Network for Trace gases by Airline) program into an inversion modeling system based on the CarbonTracker framework. We estimated the averaged annual total Asian terrestrial land CO2 sink was about -1.56 Pg C yr-1 over the <span class="hlt">period</span> 2006-2010, which offsets about one-third of the fossil fuel emission from Asia (+4.15 Pg C yr-1). The uncertainty of the terrestrial uptake estimate was derived from a set of sensitivity tests and ranged from -1.07 to -1.80 Pg C yr-1, comparable to the formal Gaussian error of ±1.18 Pg C yr-1 (1-sigma). The largest sink was found in forests, predominantly in coniferous forests (-0.64 Pg C yr-1) and mixed forests (-0.14 Pg C yr-1); and the second and third large carbon sinks were found in grass/shrub lands and crop lands, accounting for -0.44 Pg C yr-1 and -0.20 Pg C yr-1, respectively. The peak-to-peak amplitude of inter-annual variability (IAV) was 0.57 Pg C yr-1 ranging from -1.71 Pg C yr-1 to -2.28 Pg C yr-1. The IAV analysis reveals that the Asian CO2 sink was sensitive to climate variations, with the lowest uptake in 2010 concurrent with summer flood/autumn drought and the largest CO2 sink in 2009 owing to favorable temperature and plentiful precipitation conditions. We also found the inclusion of the CONTRAIL data in the inversion modeling system reduced the uncertainty by 11% over the whole Asian region, with a large reduction in the southeast of Boreal Eurasia, southeast of Temperate Eurasia and most Tropical Asian areas.</p> <div class="credits"> <p class="dwt_author">Zhang, H. F.; Chen, B. Z.; van der Laan-Luijkx, I. T.; Machida, T.; Matsueda, H.; Sawa, Y.; Fukuyama, Y.; Labuschagne, C.; Langenfelds, R.; van der Schoot, M.; Xu, G.; Yan, J. W.; Zhou, L. X.; Tans, P. P.; Peters, W.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-10-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">197</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://cds.cern.ch/record/646798/files/0310119.pdf"> <span id="translatedtitle">The orbital <span class="hlt">period</span> of the dipping, bursting, globular cluster X-ray source XB 1746-371 from Rossi X-ray Timing Explorer <span class="hlt">observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We present results from two long <span class="hlt">observations</span> of XB 1746-371 by the Rossi X-ray Timing Explorer (RXTE) in 2002 January and May, lasting 4 and 5 days respectively. Dips are <span class="hlt">observed</span> in the X-ray light curves with a depth of 25 per cent, largely independent of energy within the usable band of the PCA instrument of 2.1 - 16.0 keV. X-ray bursting and flaring activity are also evident. The dips define the orbital <span class="hlt">period</span> of the system, and using a power spectral analysis and a cycle counting technique we derive an accurate <span class="hlt">period</span> of P_orb = 5.16 +/- 0.01 hr. The previously-reported candidate <span class="hlt">period</span> of 5.73$\\pm$0.15 hr, obtained using Ginga data, is inconsistent with our determination, perhaps due to the weakness of the dipping and the variability of the source during that <span class="hlt">observation</span>. The dips in the RXTE <span class="hlt">observations</span> presented here do not align with the Ginga <span class="hlt">period</span>, however our improved <span class="hlt">period</span> is consistent with a wide range of archival data.</p> <div class="credits"> <p class="dwt_author">Balucinska-Church, M; Smale, A P</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">198</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=organic+AND+chemistry+AND+inorganic&pg=4&id=ED245913"> <span id="translatedtitle">Chemistry Curricula. Course <span class="hlt">Suggestions</span>.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Listings of <span class="hlt">suggested</span> topics aimed at helping university and college faculties plan courses in the main areas of the chemistry curricula are provided. The <span class="hlt">suggestions</span> were originally offered as appendices to the American Chemical Society's (ACS) Committee on Professional Training's 1983 guidelines for ACS-approved schools. The course data included…</p> <div class="credits"> <p class="dwt_author">American Chemical Society, Washington, DC.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">199</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014Ap%26SS.352..353E"> <span id="translatedtitle"><span class="hlt">Observation</span> of the <span class="hlt">period</span> ratio P 1/ P 2 of transversal oscillations in solar macro-spicules</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We analyze the time series of oxygen line profiles (O vi 1031.93 Å and O vi 1037.61 Å) obtained from SUMER/SOHO on the solar south limb. We calculated Doppler shifts and consequently Doppler velocities in three heights 4?, 14?, and 24? from the limb on a coronal hole region. Then, we performed wavelet analysis with Morlet wavelet transform to determine the <span class="hlt">periods</span> of fundamental mode and its first harmonic mode. The calculated <span class="hlt">period</span> ratios have departures from its canonical value of 2. The density stratification and magnetic twist are two main factors which may cause these departures.</p> <div class="credits"> <p class="dwt_author">Ebadi, H.; Khoshrangbaf, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-08-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">200</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/astro-ph/0205030v1"> <span id="translatedtitle">Eclipse Timings of the Low Mass X-ray Binary EXO0748-676 III. An Apparent Orbital <span class="hlt">Period</span> Glitch <span class="hlt">Observed</span> with USA and RXTE</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We present 7 eclipse timings of the low mass X-ray binary EXO0748-676 obtained with the USA experiment during 1999-2000 as well as 122 eclipse timings obtained with RXTE during 1996-2000. According to our analysis, the mean orbital <span class="hlt">period</span> has increased by ~8 ms between the pre-RXTE era (1985-1990) and the RXTE/USA era (1996-2000). This corresponds to an orbital <span class="hlt">period</span> derivative of P(orb)/(dP(orb)/dt)~2x10^7 years. However, neither a constant orbital <span class="hlt">period</span> derivative nor any other simple ephemeris provides an acceptable fit to the data: individual timings of eclipse centers have residuals of up to 15 or more seconds away from our derived smooth ephemerides. When we consider all published eclipse timing data including those presented here, a model that includes <span class="hlt">observational</span> measurement error, cumulative <span class="hlt">period</span> jitter, and underlying <span class="hlt">period</span> evolution is found to be consistent with the timing data. We discuss several physical mechanisms for LMXB orbital evolution in an effort to account for the change in orbital <span class="hlt">period</span> and the <span class="hlt">observed</span> intrinsic jitter in the mid-eclipse times.</p> <div class="credits"> <p class="dwt_author">M. T. Wolff; P. Hertz; K. S. Wood; P. S. Ray; R. M. Bandyopadhyay</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-05-02</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_9");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' 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onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">201</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/43152612"> <span id="translatedtitle">Spectral Index and Quasi-<span class="hlt">Periodic</span> Oscillation Frequency Correlation in Black Hole Sources: <span class="hlt">Observational</span> Evidence of Two Phases and Phase Transition in Black Holes</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Recent studies have shown that strong correlations are <span class="hlt">observed</span> between the low frequencies (1-10 Hz) of quasi-<span class="hlt">periodic</span> oscillations (QPOs) and the spectral power law index of several black hole (BH) candidate sources, in low (hard) states, steep power law (soft) states, and transitions between these states. The <span class="hlt">observations</span> indicate that the X-ray spectra of such state (phases) show the presence</p> <div class="credits"> <p class="dwt_author">Lev Titarchuk; Ralph Fiorito</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">202</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://repository.tamu.edu/handle/1969.1/129106"> <span id="translatedtitle">Soybean Insect Control <span class="hlt">Suggestions</span>.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">and during the pod-formation stage. It is not recommended where heavy populations develop during the pod-filling <span class="hlt">period</span>. This pro duct will not control defoliating beetles, grasshop pers or pod-feeding stink bugs. 9 10 Bacillus thuringiensis use...N? Diazinon?) Dimethoate (Cygon?, Defend?) Fenvalerate (Pydrin?) Methyl parathion Parathion (ethyl) Permethrin (Ambush?, Pounce?) Group 2 - Moderately Toxic Methomyl (Lannate?, Nudrin?) Group 3 - Relatively NonToxic Bacillus thuringiensis (Dipel...</p> <div class="credits"> <p class="dwt_author">Drees, B.M.</p> <p class="dwt_publisher"></p> <p class="publishDate">1985-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">203</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ucm.es/info/Astrof/users/dmg/papers/p_cs13_icc.pdf"> <span id="translatedtitle">Program Stars and Stellar Parameters Table. 1: Stellar parameters of the <span class="hlt">observed</span> stars: spectral type (SpT), vsin(i) and photometric <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">for spectroscopic binaries (singled lined (1) and double lined (2)) and T for triple star systems. The numberProgram Stars and Stellar Parameters Table. 1: Stellar parameters of the <span class="hlt">observed</span> stars: spectral type (SpT), vsin(i) and photometric <span class="hlt">period</span> (Pphot). The remark is -- for single stars, SB</p> <div class="credits"> <p class="dwt_author">Complutense de Madrid, Universidad</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">204</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/1992AdSpR..12...93M"> <span id="translatedtitle">Thermosphere and ionosphere dynamics during 20-30 March 1979 time <span class="hlt">period</span> - Comparison of TIGCM calculated densities with <span class="hlt">observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The Thermosphere Ionosphere General Circulation Model developed at the National Center for Atmospheric Research (NCAR TIGCM), has been used to simulate the time-dependent variations of global thermosphere and ionosphere structure and dynamics during the 20-30 March 1979 time <span class="hlt">period</span>. Thermospheric density variations predicted by the TIGCM during this <span class="hlt">period</span> are statistically compared to satellite electrostatic triaxial accelerometer neutral density measurements obtained between 170 and 240 km altitude and to predictions made by the Mass Spectrometer Incoherent Scatter empirical model (MSIS-86). In its present state of development, the TIGCM has attained about the same accuracy (standard deviation), as MSIS-86. Incorporation of improved representation of ion drag, resulting from the downward flow of magnetospheric plasma on the nightside, has contributed to the TIGCM model accuracy.</p> <div class="credits"> <p class="dwt_author">Marcos, F. A.; Roble, R. G.; Killeen, T. L.</p> <p class="dwt_publisher"></p> <p class="publishDate">1992-08-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">205</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/1424468"> <span id="translatedtitle">A <span class="hlt">periodic</span> table of ion charge-state distributions <span class="hlt">observed</span> in the transition region between vacuum sparks and vacuum arcs</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Ion charge-state distributions have been measured with high time resolution for short (20 ?s) and long (250 ?s) vacuum discharges of 300 A. Charge-state data for 3 ?s after discharge ignition and quasi-steady-state values are given for most conductive elements in a <span class="hlt">Periodic</span> Table, including data for a few elements (rhodium, europium, and terbium) that were never before reported in</p> <div class="credits"> <p class="dwt_author">André Anders</p> <p class="dwt_publisher"></p> <p class="publishDate">2001-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">206</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2004ApJ...612..988T"> <span id="translatedtitle">Spectral Index and Quasi-<span class="hlt">Periodic</span> Oscillation Frequency Correlation in Black Hole Sources: <span class="hlt">Observational</span> Evidence of Two Phases and Phase Transition in Black Holes</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Recent studies have shown that strong correlations are <span class="hlt">observed</span> between the low frequencies (1-10 Hz) of quasi-<span class="hlt">periodic</span> oscillations (QPOs) and the spectral power law index of several black hole (BH) candidate sources, in low (hard) states, steep power law (soft) states, and transitions between these states. The <span class="hlt">observations</span> indicate that the X-ray spectra of such state (phases) show the presence of a power-law component and are sometimes related to simultaneous radio emission, indicating the probable presence of a jet. Strong QPOs (>20% rms) are present in the power density spectrum in the spectral range where the power-law component is dominant (i.e., 60%-90%). This evidence contradicts the dominant, long-standing interpretation of QPOs as a signature of the thermal accretion disk. We present the data from the literature and our own data to illustrate the dominance of power-law index-QPO frequency correlations. We provide a model that identifies and explains the origin of the QPOs and how they are imprinted on the properties of the power-law flux component. We argue for the existence of a bounded compact coronal region that is a natural consequence of the adjustment of the Keplerian disk flow to the innermost sub-Keplerian boundary conditions near the central object and that ultimately leads to the formation of a transition layer (TL) between the adjustment radius and the innermost boundary. The model predicts two phases or states dictated by the photon upscattering produced in the TL: (1) a hard state, in which the TL is optically thin and very hot (kT>~50 keV), producing photon upscattering via thermal Comptonization (the photon spectrum index ?~1.7 for this state is dictated by gravitational energy release and Compton cooling in an optically thin shock near the adjustment radius), and (2) a soft state that is optically thick and relatively cold (kT<~5 keV; the index for this state, ?~2.8, is determined by soft-photon upscattering and photon trapping in a converging flow into the BH). In the TL model for the corona, the QPO frequency ?high is related to the gravitational (close to Keplerian) frequency ?K at the outer (adjustment) radius and ?low is related to the TL's normal mode (magnetoacoustic) oscillation frequency ?MA. The <span class="hlt">observed</span> correlations between index and low and high QPO frequencies are readily explained in terms of this model. We also <span class="hlt">suggest</span> a new method for evaluation of the BH mass using the index-frequency correlation.</p> <div class="credits"> <p class="dwt_author">Titarchuk, Lev; Fiorito, Ralph</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-09-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">207</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=retroactive&pg=5&id=EJ153844"> <span id="translatedtitle"><span class="hlt">Suggestions</span> for the Professors</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Some major learning theory principles are reviewed and <span class="hlt">suggestions</span> are made for integrating them into the process of education at the college or graduate school level. The theories deal with reinforcement, behavior modification, reactive inhibition, cognitive maps, incidental learning, retroactive inhibition, proactive inhibition, and spontaneous…</p> <div class="credits"> <p class="dwt_author">Fassler, Joan</p> <p class="dwt_publisher"></p> <p class="publishDate">1976-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">208</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25766424"> <span id="translatedtitle">Partly visible <span class="hlt">periods</span> in posture <span class="hlt">observation</span> from video: Prevalence and effect on summary estimates of postures in the job.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">This paper investigated the extent to which <span class="hlt">observers</span> rated clearly visible postures on video differently from partly visible postures, and whether visibility affected full-shift posture summaries. Trunk and upper arm postures were <span class="hlt">observed</span> from 10,413 video frames representing 80 shifts of baggage handling; <span class="hlt">observers</span> reported postures as fully or only partly visible. Postures were summarized for each shift into several standard metrics using all available data, only fully visible frames, or only partly visible frames. 78% of trunk and 70% of upper arm postural <span class="hlt">observations</span> were inferred. When based on all data, mean and 90th percentile trunk postures were 1.8° and 5.6° lower, respectively, than when based only on fully visible situations. For the arm; differences in mean and 90th percentile were 0.7° and 8.2°. Daily posture summaries were significantly influenced by whether partly visible postures are included or not. PMID:25766424</p> <div class="credits"> <p class="dwt_author">Trask, Catherine; Mathiassen, Svend Erik; Rostami, Mehdi</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-07-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">209</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4318590"> <span id="translatedtitle">Trends in Epithelial Cell Abnormalities <span class="hlt">Observed</span> on Cervical Smears over a 21-Year <span class="hlt">Period</span> in a Tertiary Care Hospital in Kuwait</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Objectives: This study aimed to analyse trends in epithelial cell abnormalities (ECAs) in cervical cytology at a tertiary care hospital in Kuwait. Methods: ECAs in 135,766 reports were compared over three seven-year <span class="hlt">periods</span> between 1992 and 2012. Conventional Papanicolaou (Pap) smear tests were used in the first two <span class="hlt">periods</span> and ThinPrep (Hologic Corp., Bedford, Massachusetts, USA) tests were used in the third. Results: Significant increases in satisfactory smears, atypical squamous cells of undetermined significance (ASCUS) and atypical glandular cells of undetermined significance/atypical glandular cells (AGUS/AGCs) were seen in the second and third <span class="hlt">periods</span> (P <0.001). No significant increases were <span class="hlt">observed</span> among low-grade squamous intraepithelial lesions (LSILs) or high-grade squamous intraepithelial lesions (HSILs) (P >0.05). An increase was noted in carcinomas between the first and second <span class="hlt">periods</span> although a significant decline was seen in the third (P <0.014). Conclusion: Satisfactory smears, ASCUS and AGUS/AGC increased during the study <span class="hlt">period</span> although no significant increases in LSILs, HSILs or carcinomas were <span class="hlt">observed</span>. PMID:25685369</p> <div class="credits"> <p class="dwt_author">Kapila, Kusum; Sharma, Prem N.; George, Sara S.; Al-Shaheen, Azza; Al-Juwaiser, Ahlam; Al-Awadhi, Rana</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">210</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20010093230&hterms=earth+day&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dearth%2Bday"> <span id="translatedtitle">Earth <span class="hlt">Observing</span>-1 Advanced Imager Flight Performance Assessment: Investigating Dark Current Stability Over One-Half Orbit <span class="hlt">Period</span> during the First 60 Days</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The stability of the EO-1 Advanced Land Imager dark current levels over the <span class="hlt">period</span> of one-half orbit is investigated. A series of two-second dark current collections, over the course of 40 minutes, was performed during the first sixty days the instrument was in orbit. Analysis of this data indicates only two dark current reference <span class="hlt">periods</span>, obtained entering and exiting eclipse, are required to remove ALI dark current offsets for 99.9% of the focal plane to within 1.5 digital numbers for any <span class="hlt">observation</span> on the solar illuminated portion of the orbit.</p> <div class="credits"> <p class="dwt_author">Mendenhall, J. A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2001-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">211</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.agu.org/journals/jc/v086/iC10/JC086iC10p09698/JC086iC10p09698.pdf"> <span id="translatedtitle">Inertio-Gravity Wave Induced Accelerations of Mean Flow Having an Imposed <span class="hlt">Periodic</span> Component: Implications for Tidal <span class="hlt">Observations</span> in the Meteor Region</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The semidiurnal harmonic exhibits great day-to-day variability in amplitude and phase. In addition, the variability appears to be substantially local and random, <span class="hlt">suggesting</span> a connection with gravity wave activity. We <span class="hlt">suggest</span> that a significant contribution to the <span class="hlt">observed</span> semidiurnal harmonic at meteor heights might result from inertio-gravity wave induced accelerations of the mean flow. The rate of wave forcing of</p> <div class="credits"> <p class="dwt_author">R. L. Walterscheid</p> <p class="dwt_publisher"></p> <p class="publishDate">1981-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">212</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/1464382"> <span id="translatedtitle">Satellite calibration using a collocated nadir <span class="hlt">observation</span> technique: theoretical basis and application to the GMS-5 Pathfinder benchmark <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">A collocated nadir <span class="hlt">observation</span> technique has been used as part of the geostationary meteorological satellite (GMS) pathfinder project and is now employed at the Australian Bureau of Meteorology Research Centre to calibrate the visible infrared spin scan radiometer (VISSR) instrument used on GMS-5. It uses satellite-to-satellite cross calibration to bypass many of the problems inherent in the absolute calibration of</p> <div class="credits"> <p class="dwt_author">John F. Le Marshall; James J. Simpson; Zhonghai Jin</p> <p class="dwt_publisher"></p> <p class="publishDate">1999-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">213</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/astro-ph/0309110v1"> <span id="translatedtitle">XMM-Newton <span class="hlt">observations</span> of three short <span class="hlt">period</span> polars: V347 Pav, GG Leo and EU UMa</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We present phase-resolved XMM_Newton data of three short <span class="hlt">period</span> polars: V347 Pav, GG Leo and EU UMa. All three systems show one dominant accretion region which is seen for approximately half of the orbital cycle. GG Leo shows a strong dip feature in its X-ray and UV light curves which is due to absorption of X-rays from the accretion site by the accretion stream. The emission in the case of EU UMa is dominated by soft X-rays: its soft/hard X-ray ratio is amongst the highest seen in these objects. In contrast, GG Leo and V347 Pav shows a ratio consistent with that predicted by the standard shock model. We infer the mass of the white dwarf and explore the affect of restricting the energy range on the derived parameters.</p> <div class="credits"> <p class="dwt_author">Gavin Ramsay; Mark Cropper; K. O. Mason; F. A. Cordova; W. Priedhorsky</p> <p class="dwt_publisher"></p> <p class="publishDate">2003-09-03</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">214</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013AGUFMAE33B0343A"> <span id="translatedtitle">How well does WWLLN reproduce the satellite-<span class="hlt">observed</span> distribution of flashes during the 2007-2012 time <span class="hlt">period</span>?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Lightning is the dominant source of nitrogen oxides (NOx) involved in the production of ozone in the middle and upper troposphere in the tropics and in summer in the midlatitudes. Therefore it is imperative that the lightning NOx (LNOx) source strength per flash be better constrained. This process requires accurate information on the location and timing of lightning flashes. In the past fifteen years satellite-based lightning monitoring by the Optical Transient Detector (OTD) and Lightning Imaging Sensor (LIS) has greatly increased our understanding of the global distribution of lightning as a function of season and time-of-day. However, detailed information at higher temporal resolutions is only available for limited regions where ground-based networks such as the United States National Lightning Detection Network (NLDN) exist. In 2004, the ground-based World Wide Lightning Location Network (WWLLN) was formed with the goal of providing continuous flash rate information over the entire globe. It detects very low frequency (VLF) radio waves emitted by lightning with a detection efficiency (DE) that varies with stroke energy, time-of-day, surface type, and network coverage. This study evaluated the DE of WWLLN strokes relative to climatological OTD/LIS flashes using data from the 2007 to 2012 time <span class="hlt">period</span>, a <span class="hlt">period</span> during which the mean number of working sensors increased from 28 to 53. The analysis revealed that the mean global DE increased from 5% in 2007 to 13% in 2012. Regional variations were substantial with mean 2012 DEs of 5-10% over much of Argentina, Africa, and Asia and 15-30% over much of the Atlantic, Pacific, and Indian Oceans, the United States and the Maritime Continent. Detection-efficiency adjusted WWLLN flash rates were then compared to NLDN-based flash rates. Spatial correlations for individual summer months ranged from 0.66 to 0.93. Temporal correlations are currently being examined for regions of the U.S. and will also be shown.</p> <div class="credits"> <p class="dwt_author">Allen, D. J.; Pickering, K. E.; Ring, A.; Holzworth, R. H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">215</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014SoPh..289.1239N"> <span id="translatedtitle">Imaging <span class="hlt">Observations</span> of X-Ray Quasi-<span class="hlt">periodic</span> Oscillations at 3 - 6 keV in the 26 December 2002 Solar Flare</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Quasi-<span class="hlt">periodic</span> oscillations in soft X-rays (SXR) are not well known due to the instrument limitations, especially the absence of imaging <span class="hlt">observations</span> of SXR oscillations. We explore the quasi-<span class="hlt">periodic</span> oscillations of SXR at 3 - 6 keV in a solar flare <span class="hlt">observed</span> by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) on 26 December 2002. This was a B8.1 class event and showed three X-ray sources (S1, S2, and S3) at 3 - 6 keV and two sources (S1 and S2) at 12 - 25 keV. The light curves of the total fluxes display a two-minute oscillation at 3 - 6 keV, but not in the energy bands above 8 keV. To investigate imaging <span class="hlt">observations</span> of the oscillations, we prepared CLEAN images at seven energy bands between 3 keV and 20 keV with an eight-second integration. The light curves of three sources were analyzed after integrating the flux of each source region. We used the Fourier method to decompose each source light curve into rapidly varying and slowly varying components. The rapidly varying components show seven individual peaks which are well fitted with a sine function. Then we used the wavelet method to analyze the <span class="hlt">periods</span> in the rapidly varying component of each source. The results show that three sources display damped quasi-<span class="hlt">periodic</span> oscillations with a similar two-minute <span class="hlt">period</span>. The damped oscillations timescale varies between 2.5 to 6 minutes. Source S1 oscillates with the same phase as S3, but is almost in anti-phase with S2. Analyzing the flaring images in more detail, we found that these oscillation peaks are well consistent with the appearance of S3, which seems to split from or merge with S2 with a <span class="hlt">period</span> of two minutes. The flare images with a high cadence of one second at 3 - 6 keV show that source S3 appears with a rapid <span class="hlt">period</span> of 25 seconds. The two-minute oscillation shows the highest spectral power. Source S3 seems to shift its position along the flare loop with a mean speed of 130 km s-1, which is of the same order as the local sound speed. This connection between the oscillation peaks and emission enhancement appears to be an <span class="hlt">observational</span> constraint on the emission mechanism at 3 - 6 keV.</p> <div class="credits"> <p class="dwt_author">Ning, Zongjun</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">216</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/11295242"> <span id="translatedtitle">Inner magnetosphere variations after Solar Proton Events. <span class="hlt">Observations</span> on Mir space station in 1989–1994 time <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Measurements on board the Mir space station have been used to study the dose rate and the particle flux distribution in the inner magnetosphere. The measurements have been performed with the Bulgarian-Russian dosimeter-radiometer Liulin. The paper concentrates on the dynamics of the <span class="hlt">observed</span> “new” and “second” maxima which were created after Solar Proton Events (SPE) in the 1989–1994 time. The</p> <div class="credits"> <p class="dwt_author">Ts. P. Dachev; J. V. Semkova; Yu. N Matviichuk; B. T. Tomov; R. T. Koleva; P. T. Baynov; V. M. Petrov; V. V. Shurshakov; Yu. Ivanov</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">217</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24824766"> <span id="translatedtitle">Difference in production routes of water-soluble organic carbon in PM2.5 <span class="hlt">observed</span> during non-biomass and biomass burning <span class="hlt">periods</span> in Gwangju, Korea.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">4 h integrated PM2.5 samples were collected from an urban site of Gwangju, Korea, for five days and analyzed for organic carbon and elemental carbon (OC and EC), total water-soluble OC (WSOC), hydrophilic and hydrophobic WSOC fractions (WSOCHPI and WSOCHPO), oxalate, and inorganic ionic species (sodium (Na(+)), ammonium (NH4(+)), potassium (K(+)), calcium (Ca(2+)), magnesium (Mg(2+)), chloride (Cl(-)), nitrate (NO3(-)), and sulfate (SO4(2-))) to investigate the possible sources of water-soluble organic aerosols. Two types of sampling <span class="hlt">periods</span> were classified according to the regression relationship between black carbon (BC) concentrations measured at wavelengths of 370 nm (BC370nm) and 880 nm (BC880nm) using an aethalometer; the first <span class="hlt">period</span> was traffic emission influence ("non-biomass burning (BB) <span class="hlt">period</span>") and the second was biomass burning influence ("BB <span class="hlt">period</span>"). The slope of the regression equation (BC370nm/BC880nm) was 0.95 for the non-BB <span class="hlt">period</span> and 1.29 for the BB <span class="hlt">period</span>. However, no noticeable difference in the WSOC/OC ratio, which can be used to infer the extent of secondary organic aerosol (SOA) formation, was found between the non-BB (0.61, range = 0.43-0.75) and BB (0.61, range = 0.52-0.68) <span class="hlt">periods</span>, due to significant contribution of primary BB emissions to the WSOC. The concentrations of OC, WSOC and K(+), which were used as the BB emission markers, were 15.7 ?g C m(-3) (11.5-24.3), 9.4 ?g C m(-3) (7.0-12.7), and 1.2 ?g m(-3) (0.6-2.7), respectively, during the BB <span class="hlt">period</span>, and these results were approximately 1.7, 1.7, and 3.9 times higher than those during the non-BB <span class="hlt">period</span>. During the non-BB <span class="hlt">period</span>, good correlations among WSOC, SO4(2-) and oxalate, and poor correlations among WSOC, EC, and K(+) <span class="hlt">suggest</span> that SOA is probably an important source of WSOC (and WSOCHPI) concentration. For the WSOC fractions, better correlations among WSOCHPI, oxalate (R(2) = 0.52), and SO4(2-) (R(2) = 0.57) were found than among WSOCHPO, oxalate (R(2) = 0.23), and SO4(2-) (R(2) = 0.20), <span class="hlt">suggesting</span> that a significant proportion of the WSOCHPI fraction of OC could be produced through processes (gas-phase and heterogeneous oxidations) such as SOA formation. However, during the BB <span class="hlt">period</span>, the BB emission source accounted for the high correlations between total WSOC (and WSOC fractions) and other relevant atmospheric parameters (EC, Na(+), Cl(-), K(+), and oxalate), with higher correlations in WSOCHPI than in WSOCHPO. These results <span class="hlt">suggest</span> a significant contribution of BB emissions to WSOC. PMID:24824766</p> <div class="credits"> <p class="dwt_author">Yu, Geun-Hye; Cho, Sung-Yong; Bae, Min-Suk; Park, Seung-Shik</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">218</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.publish.csiro.au/?act=view_file&file_id=MU9840071.pdf"> <span id="translatedtitle"><span class="hlt">OBSERVATIONS</span> ON COLONY SIZE, BREEDING SUCCESS, RECRUITMENT AND INTER-COLONY DISPERSAL IN A TASMANIAN COLONY OF SHORT-TAILED SHEARWATERS PUFFINUS TENUIROSTRIS OVER A 30YEAR <span class="hlt">PERIOD</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">SUMMARY SERVENTY, D.L. and P.J. CURRY 1984. <span class="hlt">Observations</span> on colony size, breeding success, recruitment and inter- colony dispersal in a Tasmanian colony of Short-tailed Shearwaters Puffinus tenurrostrrs over a 30-year <span class="hlt">period</span>. Emu 84: 71-79. A programme to mark a small colony of Short-tailed Shearwaters, by means of monel leg-bands, was begun on Fisher Island during 1947-50 as part of a</p> <div class="credits"> <p class="dwt_author">D. L. SERVENTY; P. J. CURRY</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">219</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2005AGUFMSA43A1094W"> <span id="translatedtitle">Quasi-<span class="hlt">periodic</span> Variations of 2 to 4 Days in the Electron Density of the Post Sunset Equatorial Anomaly <span class="hlt">Observed</span> to be Synchronous on a Planetary Sale.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Quasi-<span class="hlt">periodic</span> variations are <span class="hlt">observed</span> in the F layer maximum electron density of the post sunset equatorial anomaly at its temporal maximum which occurs near 2100 LT. <span class="hlt">Periods</span> are 3-4 days in Oct-Jan and about 2 days in Mar-Apr; magnitudes are large, peak-to-valley ratios being between 2 and 5; conditions are solar maximum. <span class="hlt">Observations</span> are by ionospheric sounders in the American sector at magnetically conjugate locations in Northern and Southern hemispheres, and at Okinawa in the northern anomaly of Eastern Asia. The variations are synchronous in that the dates of each maximum and of each minimum coincide at all locations, day-to-day continuously for month-long <span class="hlt">periods</span>. This relation exists although measurements in the American sector are at 02 UT and those at Okinawa are at 12 UT. In addition, the magnetically conjugate variations are simultaneous, which is evidence that the variations are a product of pre-reversal ExB drift velocity. These variations are similar both in frequency and in their episodic nature to those <span class="hlt">observed</span> principally in the daytime anomaly where they are attributed to planetary scale oscillations in the neutral mesospheric zonal winds. If the variations reported here have a similar cause, it raises the possibility that the magnitude of the electron density of the anomaly - and therefore the conditions under which scintillation on trans-ionospheric RF signals can occur - can be forecast by two means: by the quasi-<span class="hlt">periodic</span> repetition of the variations; and by the <span class="hlt">observation</span> of planetary waves in the mesosphere by the TIMED satellite.</p> <div class="credits"> <p class="dwt_author">Whalen, J. A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">220</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://repository.tamu.edu/handle/1969.1/ETD-TAMU-1963-THESIS-M698"> <span id="translatedtitle">Investigation of radiation patterns in the 8-12 micron range as <span class="hlt">observed</span> by Tiros III over the Caribbean Sea during the <span class="hlt">period</span> 20-21 July 1961</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">INVESTIGATION OF RADIATION PATTERNS IN THE 8-12 MICRON RANGE AS <span class="hlt">OBSERVED</span> BY TIROS III OVER THE CARIBBEAN SEA DURING THE <span class="hlt">PERIOD</span> 20-21 JULY 1961 A Thesis By PAUL IRVIN MOHLER Captain, United States Air Force Submitted to the Graduate School... of the Agricultural and Mechanical College of Texas in partial fulfillment of the requirements for the degree of MASTER OF SCIENCE August 1963 Ma)or Sub]ect: METEOROLOGY INVESTIGATION OF RADIATION PATTERNS IN THE 8-12 MICRON RANGE AS <span class="hlt">OBSERVED</span> BY TIROS III OVER...</p> <div class="credits"> <p class="dwt_author">Mohler, Paul Irvin</p> <p class="dwt_publisher"></p> <p class="publishDate">1963-01-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" 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onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_13");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">221</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014JGRD..119.2990A"> <span id="translatedtitle">The low-level jet dust emission mechanism in the central Sahara: <span class="hlt">Observations</span> from Bordj-Badji Mokhtar during the June 2011 Fennec Intensive <span class="hlt">Observation</span> <span class="hlt">Period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This paper presents the first detailed analysis of low-level jets (LLJs) in the central Sahara from ground-based <span class="hlt">observations</span> at Bordj-Badji Mokhtar, Algeria, and addresses their operation as a dust emission mechanism. On LLJ mornings, composite wind speeds in the core (300 m aboveground level) reach 13.5 m s-1 at 0400. Surface temperatures increase from 0545 (30 min after sunrise), and jet decay begins around 0600. Ten meter winds lag those in the core by 5 h; peak 10 m wind speed, 7.5 m s-1, occurs at 0900. Only the deepest and strongest LLJs lead to dust emission. At 0600, these five LLJs have core wind speeds ?16 m s-1, below-core wind shear ? 0.6 m s-1/30 m, and wind shear between the core and 500 m above the core ?-1.8 m s-1. On these occasions, momentum mixes down from the LLJ after surface heating, leading to emission. On nondusty LLJ mornings, the convective boundary layer is 100 m shallower, and the LLJ is too weak to provide enough momentum to be mixed down for emission. LLJs are most frequently embedded in the monsoon flow or in the Harmattan; there is a clear association with the Saharan Heat Low. ERA-Interim reanalysis underestimates both Harmattan and monsoon LLJ core winds (by 4 m s-1 and 6 m s-1, respectively). The Met Office Africa Limited Area Model underestimates Harmattan LLJ core winds by only 0.2 m s-1. Monsoon LLJ core winds, however, are underestimated by 8.5 m s-1. Surface winds at 0900 are underestimated in both cases by up to 6 m s-1.</p> <div class="credits"> <p class="dwt_author">Allen, Christopher J. T.; Washington, Richard</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">222</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/20788215"> <span id="translatedtitle">An <span class="hlt">observational</span> study <span class="hlt">suggesting</span> clinical benefit for adjuvant postoperative chemoradiation in a population of over 500 cases after gastric resection with D2 nodal dissection for adenocarcinoma of the stomach</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Purpose: The role of adjuvant chemoradiotherapy (CRT) in D2-resected gastric-cancer patients has not been defined yet. We investigated the effect of postoperative chemoradiotherapy on the relapse rate and survival rate of patients with D2-resected gastric cancer. Methods and Materials: From August 1995 to April 2001, 544 patients received postoperative CRT after curative D2 resection. During the same <span class="hlt">period</span> of time, 446 patients received surgery without further adjuvant treatment. The adjuvant CRT consisted of 400 mg/m{sup 2} of fluorouracil plus 20 mg/m{sup 2} of leucovorin for 5 days, followed by 4,500 cGy of radiotherapy for 5 weeks, with fluorouracil and leucovorin on the first 4 and the last 3 days of radiotherapy. Two 5-day cycles of fluorouracil and leucovorin were given 4 weeks after the completion of radiotherapy. Results: The median duration of overall survival was significantly longer in the CRT group than in the comparison group (95.3 months vs. 62.6 months), which corresponds to a hazard ratio for death of 0.80 (p = 0.0200) or a reduction of 20% in the risk of death in the CRT group. The 5-year survival rates were consistently longer in the CRT group at Stages II, IIIA, IIIB, and IV than those in the comparison group. The CRT was associated with increases in the median duration of relapse-free survival (75.6 months vs. 52.7 months; hazard ratio for relapse, 0.80, p = 0.0160). Conclusion: Our results highly <span class="hlt">suggest</span> that the postoperative chemoradiotherapy in D2-resected gastric-cancer patients can prolong survival and decrease recurrence.</p> <div class="credits"> <p class="dwt_author">Kim, Sung [Department of Surgery, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Lim, Do Hoon [Department of Radiation Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Lee, Jeeyun [Division of Hematology-Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Kang, Won Ki [Division of Hematology-Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of)]. E-mail: wkkang@smc.samsung.co.kr; MacDonald, John S. [Gastrointestinal Oncology Service, Saint Vincent's Comprehensive Cancer Center, New York, NY (United States); Park, Chan Hyung [Center for the Improvement of Human Functioning International, Inc., Wichita, KS (United States); Park, Se Hoon [Division of Hematology-Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Lee, Se-Hoon [Division of Hematology-Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Kim, Kihyun [Division of Hematology-Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Park, Joon Oh; Kim, Won Seog; Jung, Chul Won; Park, Young Suk; Im, Young-Hyuck [Division of Hematology-Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Sohn, Tae Sung; Noh, Jae Hyung; Heo, Jin Seok; Kim, Yong Il [Department of Surgery, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Park, Chul Keun [Department of Pathology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of); Park, Keunchil [Division of Hematology-Oncology, Samsung Medical Center, Sungkyunkwan University School of Medicine, Seoul (Korea, Republic of)</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">223</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20040182332&hterms=Periodic+table&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3D%2528Periodic%2Btable%2529"> <span id="translatedtitle">Spectral Index and Quasi-<span class="hlt">Periodic</span> Oscillation Frequency Correlation in Black Hole Sources: <span class="hlt">Observational</span> Evidence of Two Phases and Phase Transition in Black Holes</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Recent studies have shown that strong correlations are <span class="hlt">observed</span> between the low frequencies (1-10 Hz) of quasi-<span class="hlt">periodic</span> oscillations (QPOs) and the spectral power law index of several black hole (BH) candidate sources, in low (hard) states, steep power law (soft) states, and transitions between these states. The <span class="hlt">observations</span> indicate that the X-ray spectra of such state (phases) show the presence of a power-law component and are sometimes related to simultaneous radio emission, indicating the probable presence of a jet. Strong QPOs (>20% rms) are present in the power density spectrum in the spectral range where the power-law component is dominant (i.e., 60%90%). This evidence contradicts the dominant, long-standing interpretation of QPOs as a signature of the thermal accretion disk. We present the data from the literature and our own data to illustrate the dominance of power-law index-QPO frequency correlations. We provide a model that identifies and explains the origin of the QPOs and how they are imprinted on the properties of the power-law flux component. We argue for the existence of a bounded compact coronal region that is a natural consequence of the adjustment of the Keplerian disk flow to the innermost sub-Keplerian boundary conditions near the central object and that ultimately leads to the formation of a transition layer (TL) between the adjustment radius and the innermost boundary. The model predicts two phases or states dictated by the photon upscattering produced in the TL: (1) a hard state, in which the TL is optically thin and very hot (kT approximately greater than 50 keV), producing photon upscattering via thermal Comptonization (the photon spectrum index Gamma approximates 1.7 for this state is dictated by gravitational energy release and Compton cooling in an optically thin shock near the adjustment radius), and (2) a soft state that is optically thick and relatively cold (kT approximately less than 5 keV the index for this state, Gamma approximates 2.8, is determined by soft-photon upscattering and photon trapping in a converging flow into the BH). In the TL model for the corona, the QPO frequency V(sub high) is related to the gravitational (close to Keplerian) frequency V(sub K) at the outer (adjustment) radius and v(sub low) is related to the TL's normal mode (magnetoacoustic) oscillation frequency v(sub MA) . The <span class="hlt">observed</span> correlations between index and low and high QPO frequencies are readily explained in terms of this model. We also <span class="hlt">suggest</span> a new method for evaluation of the BH mass using the index-frequency correlation.</p> <div class="credits"> <p class="dwt_author">Titarchuk, Lev; Fiorito, Ralph</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">224</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://dspace.mit.edu/handle/1721.1/41044"> <span id="translatedtitle"><span class="hlt">Suggestions</span> for Genetic A.I.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">This paper presents <span class="hlt">suggestions</span> for "Genetic A.I.": an attempt to model the genesis of intelligence in human infants, particularly as described by Piaget's theory of the Sensorimotor <span class="hlt">period</span>. The paper includes a synopsis ...</p> <div class="credits"> <p class="dwt_author">Drescher, Gary L.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">225</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24723741"> <span id="translatedtitle">Prognostic factors for long-term survival in patients with ampullary carcinoma: the results of a 15-year <span class="hlt">observation</span> <span class="hlt">period</span> after pancreaticoduodenectomy.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Introduction. Although ampullary carcinoma has the best prognosis among all periampullary carcinomas, its long-term survival remains low. Prognostic factors are only available for a <span class="hlt">period</span> of 10 years after pancreaticoduodenectomy. The aim of this retrospective study was to identify factors that influence the long-term patient survival over a 15-year <span class="hlt">observation</span> <span class="hlt">period</span>. Methods. From 1992 to 2007, 143 patients with ampullary carcinoma underwent pancreatic resection. 86 patients underwent pylorus-preserving pancreaticoduodenectomy (60%) and 57 patients underwent standard Kausch-Whipple pancreaticoduodenectomy (40%). Results. The overall 1-, 5-, 10-, and 15-year survival rates were 79%, 40%, 24%, and 10%, respectively. Within a mean <span class="hlt">observation</span> <span class="hlt">period</span> of 30 (0-205) months, 100 (69%) patients died. Survival analysis showed that positive lymph node involvement (P = 0.001), lymphatic vessel invasion (P = 0.0001), intraoperative administration of packed red blood cells (P = 0.03), an elevated CA 19-9 (P = 0.03), jaundice (P = 0.04), and an impaired patient condition (P = 0.01) are strong negative predictors for a reduced patient survival. Conclusions. Patients with ampullary carcinoma have distinctly better long-term survival than patients with pancreatic adenocarcinoma. Long-term survival depends strongly on lymphatic nodal and vessel involvement. Moreover, a preoperative elevated CA 19-9 proved to be a significant prognostic factor. Adjuvant therapy may be essential in patients with this risk constellation. PMID:24723741</p> <div class="credits"> <p class="dwt_author">Klein, Fritz; Jacob, Dietmar; Bahra, Marcus; Pelzer, Uwe; Puhl, Gero; Krannich, Alexander; Andreou, Andreas; Gül, Safak; Guckelberger, Olaf</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">226</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3958923"> <span id="translatedtitle">Prognostic Factors for Long-Term Survival in Patients with Ampullary Carcinoma: The Results of a 15-Year <span class="hlt">Observation</span> <span class="hlt">Period</span> after Pancreaticoduodenectomy</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Introduction. Although ampullary carcinoma has the best prognosis among all periampullary carcinomas, its long-term survival remains low. Prognostic factors are only available for a <span class="hlt">period</span> of 10 years after pancreaticoduodenectomy. The aim of this retrospective study was to identify factors that influence the long-term patient survival over a 15-year <span class="hlt">observation</span> <span class="hlt">period</span>. Methods. From 1992 to 2007, 143 patients with ampullary carcinoma underwent pancreatic resection. 86 patients underwent pylorus-preserving pancreaticoduodenectomy (60%) and 57 patients underwent standard Kausch-Whipple pancreaticoduodenectomy (40%). Results. The overall 1-, 5-, 10-, and 15-year survival rates were 79%, 40%, 24%, and 10%, respectively. Within a mean <span class="hlt">observation</span> <span class="hlt">period</span> of 30 (0–205) months, 100 (69%) patients died. Survival analysis showed that positive lymph node involvement (P = 0.001), lymphatic vessel invasion (P = 0.0001), intraoperative administration of packed red blood cells (P = 0.03), an elevated CA 19-9 (P = 0.03), jaundice (P = 0.04), and an impaired patient condition (P = 0.01) are strong negative predictors for a reduced patient survival. Conclusions. Patients with ampullary carcinoma have distinctly better long-term survival than patients with pancreatic adenocarcinoma. Long-term survival depends strongly on lymphatic nodal and vessel involvement. Moreover, a preoperative elevated CA 19-9 proved to be a significant prognostic factor. Adjuvant therapy may be essential in patients with this risk constellation. PMID:24723741</p> <div class="credits"> <p class="dwt_author">Jacob, Dietmar; Bahra, Marcus; Puhl, Gero; Krannich, Alexander; Andreou, Andreas; Gül, Safak; Guckelberger, Olaf</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">227</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4130246"> <span id="translatedtitle">Sensitive <span class="hlt">Periods</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">This chapter reviews sensitive <span class="hlt">periods</span> in human brain development based on the literature on children raised in institutions. Sensitive experiences occur when experiences are uniquely influential for the development of neural circuitry. Because in humans, we make inferences about sensitive <span class="hlt">periods</span> from evaluations of complex behaviors, we underestimate the occurrence of sensitive <span class="hlt">periods</span> at the level of neural circuitry. Although we are most interested in complex behaviors, such as IQ or attachment or externalizing problems, many different sensitive <span class="hlt">periods</span> at the level of circuits probably underlie these complex behaviors. Results from a number of studies <span class="hlt">suggest</span> that across most, but not all, domains of development, institutional rearing limited to the first 4–6 months of life is associated with no significant increase risk for long-term adverse effects relative to non-institutionalized children. Beyond that, evidence for sensitive <span class="hlt">periods</span> is less compelling, meaning that “the earlier the better” rule for enhanced caregiving is a reasonable conclusion at the current state of the science. PMID:25125708</p> <div class="credits"> <p class="dwt_author">Zeanah, Charles H.; Gunnar, Megan R.; McCall, Robert B.; Kreppner, Jana M.; Fox, Nathan A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">228</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/1311.6973.pdf"> <span id="translatedtitle">Swift X-ray and ultraviolet <span class="hlt">observations</span> of the shortest orbital <span class="hlt">period</span> double-degenerate system RX J0806.3+1527 (HM Cnc)</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">RX J0806.3+1527 (HM Cnc) is a pulsating X-ray source with 100 per cent modulation on a <span class="hlt">period</span> of 321.5 s (5.4 min). This <span class="hlt">period</span> reflects the orbital motion of a close binary system consisting of two interacting white dwarfs. Here we present a series of simultaneous X-ray (0.2-10 keV) and near-ultraviolet (2600 angstrom and 1928 angstrom) <span class="hlt">observations</span> carried out with the Swift satellite. In the near-ultraviolet the counterpart of RX J0806.3+1527 was detected at flux densities consistent with a blackbody with temperature 27E+3 K. We found that the emission at 2600 angstrom is modulated at the 321.5-s <span class="hlt">period</span>, with the peak ahead of the X-ray one by 0.28 cycles and coincident, within 0.05 cycles, with the optical. This phase-shift measurement confirms that the X-ray hot spot (located on the primary white dwarf) is at about 80-100 degrees from the direction connecting the two white dwarfs. Albeit at lower significance, the 321.5-s signature is present also in the 1928-angstrom data; at this wavelength, however, t...</p> <div class="credits"> <p class="dwt_author">Esposito, P; Dall'Osso, S; Covino, S</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">229</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19740014854&hterms=cahill&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dcahill"> <span id="translatedtitle">Explorer 45 (S 3-A) <span class="hlt">observations</span> of the magnetosphere and magnetopause during the 4-5 August 1972, magnetic storm <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The Explorer 45 satellite performed extensive field and particle measurements in the heart of the magnetosphere during the double magnetic storm <span class="hlt">period</span> of August 4-5, 1972. Both ground level magnetic records and the magnetic field deformations measured along the orbit by the satellite indicated the existence of only a moderate ring current. This was confirmed by the measurements of the total proton energy density less than those <span class="hlt">observed</span> during the December 1971 and June 1972 magnetic storms. The plasmapause in the noon quadrant was eroded continuously from the onset of the first storm at the beginning of August 4 to an altitude below L = 2.07 at about 18 hours on August 5. During the orbit containing the second sudden commencement a large amount of low frequency electric and magnetic field noise was encountered throughout the entire orbit. A noteworthy <span class="hlt">observation</span> during this orbit was the contraction of the magnetopause to distances inside the satellite at L = 5.2.</p> <div class="credits"> <p class="dwt_author">Hoffman, R. A.; Cahill, L. J., Jr.; Anderson, R. R.; Maynard, N. C.; Smith, P. H.; Fritz, T. A.; Williams, D. J.; Konradi, A.; Gurnett, D. A.</p> <p class="dwt_publisher"></p> <p class="publishDate">1974-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">230</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/5376390"> <span id="translatedtitle">Operation of a digital seismic network on Mount St. Helens volcano and <span class="hlt">observations</span> of long <span class="hlt">period</span> seismic events that originate under the volcano</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">A 9 station digital seismic array was operated on Mount St. Helens volcano in Washington State during 1981. One of the stations was placed inside the crater of the volcano, six were located on the flanks of the volcano within two km of the crater and two were approximately ten km from the crater. Four of the instruments recorded three components of motion and the remaining five recorded only the vertical component. A one day experiment was carried out during which the crater monitoring seismometer was complimented by the addition of two ink recording instruments. During the one day experiment six <span class="hlt">observers</span> recorded times of rockfall, felt-earthquake occurrences, and changes in steam emissions from the dome in the crater. Using information obtained during the one day experiment seismic events recorded by the digital instruments were classified as earthquakes, rockfalls, helicopter noise and a type of event that is unique to volcanoes which is called long <span class="hlt">period</span>. Waveforms of these long <span class="hlt">period</span> events have a duration of up to 30 seconds and a spectrum that is peaked at approximately 2 Hz. The frequency at which the peak in the spectrum occurs is nearly the same at all stations which means that the unique waveform of long <span class="hlt">period</span> events is due to a source effect, not a path effect. The peak frequency is fairly insensitive to the amplitude of the signal which means that the size of the source region is constant, independent of the signal amplitude. Long <span class="hlt">period</span> events were not felt and were accompanied by no visible changes inside the crater which lead to the conclusion that they are some sort of seismic disturbance generated inside the Volcano.</p> <div class="credits"> <p class="dwt_author">Fehler, M.; Chouet, B.</p> <p class="dwt_publisher"></p> <p class="publishDate">1982-09-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">231</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22039312"> <span id="translatedtitle">EXTREME-ULTRAVIOLET MULTI-WAVELENGTH <span class="hlt">OBSERVATIONS</span> OF QUASI-<span class="hlt">PERIODIC</span> PULSATIONS IN A SOLAR POST-FLARE CUSP-SHAPE LOOP WITH SDO/AIA</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We present extreme-ultraviolet multi-wavelength <span class="hlt">observations</span> with the SDO/AIA instruments of quasi-<span class="hlt">periodic</span> pulsations (QPPs) propagating along a cusp-shaped loop formed after an M2.2 flare on the Sun. Our motivation is to detect whether there were slow-mode magnetoacoustic waves propagating along its protruding flux tube. To this end, with fast Fourier transform we extract the short (<3 minutes) and long (>3 minutes) <span class="hlt">period</span> components of the QPPs from time-space diagrams of the tube slices. We find that velocity differences did exist among the short/long-<span class="hlt">period</span> components of different wavelengths, but only one event in the long-<span class="hlt">period</span> ones showed they were greater than the measurement errors (e.g., 65 km s{sup -1}), which were 330 km s{sup -1} detected in 171 A, 590 km s{sup -1} in 211 A, and 180 km s{sup -1} in 304 A. The intensity modulation in all wavelengths is found to be very large, e.g., {approx}60% of the emission trend for an event in the 171 A passband, which would be an order of magnitude higher than the perturbation of the plasma density in the slow-mode magnetoacoustic waves. Moreover, only the QPPs with upward velocities of 50-300 km s{sup -1} are found in the tube, and the downward ones of several tens of kilometers are never unambiguously detected. Therefore, most of the QPP events under study were likely the episodic outflows along the tube, and the one with a supersonic speed of 590 km s{sup -1} may be a kink wave.</p> <div class="credits"> <p class="dwt_author">Su, J. T. [Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Science, Beijing 100012 (China); Shen, Y. D.; Liu, Y. [National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011 (China)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-07-20</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">232</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/0706.3665v1"> <span id="translatedtitle">Multiwavelength optical <span class="hlt">observations</span> of chromospherically active binary systems V. FF UMa (2RE J0933+624): a system with orbital <span class="hlt">period</span> variation</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">This is the fifth paper in a series aimed at studying the chromospheres of active binary systems using several optical spectroscopic indicators to obtain or improve orbital solution and fundamental stellar parameters. We present here the study of FF UMa (2RE J0933+624), a recently discovered, X-ray/EUV selected, active binary with strong H_alpha emission. The objectives of this work are, to find orbital solutions and define stellar parameters from precise radial velocities and carry out an extensive study of the optical indicators of chromospheric activity. We obtained high resolution echelle spectroscopic <span class="hlt">observations</span> during five <span class="hlt">observing</span> runs from 1998 to 2004. We found radial velocities by cross correlation with radial velocity standard stars to achieve the best orbital solution. We also measured rotational velocity by cross-correlation techniques and have studied the kinematic by galactic space- velocity components (U, V, W) and Eggen criteria. Finally, we have determined the chromospheric contribution in optical spectroscopic indicators, from Ca II H & K to Ca II IRT lines, using the spectral subtraction technique. We have found that this system presents an orbital <span class="hlt">period</span> variation, higher than previously detected in other RS CVn systems. We determined an improved orbital solution, finding a circular orbit with a <span class="hlt">period</span> of 3.274 days. We derived the stellar parameters, confirming the subgiant nature of the primary component and obtained rotational velocities (vsini), of 33.57 km/s and 32.38 km/s for the primary and secondary components respectively. From our kinematic study, we can deduce its membership to the Castor moving group. Finally, the activity study has given us a better understanding of the possible mechanisms that produce the orbital <span class="hlt">period</span> variation.</p> <div class="credits"> <p class="dwt_author">M. C. Gálvez; D. Montes; M. J. Fernández-Figueroa; E. De Castro; M. Cornide</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-06-25</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">233</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014ApJ...795..114H"> <span id="translatedtitle">Quasi-<span class="hlt">periodic</span> Oscillations in Short Recurring Bursts of Magnetars SGR 1806-20 and SGR 1900+14 <span class="hlt">Observed</span> with RXTE</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Quasi-<span class="hlt">periodic</span> oscillations (QPOs) <span class="hlt">observed</span> in the giant flares of magnetars are of particular interest due to their potential to open up a window into the neutron star interior via neutron star asteroseismology. However, only three giant flares have been <span class="hlt">observed</span>. We therefore make use of the much larger data set of shorter, less energetic recurrent bursts. Here, we report on a search for QPOs in a large data set of bursts from the two most burst-active magnetars, SGR 1806-20 and SGR 1900+14, <span class="hlt">observed</span> with Rossi X-ray Timing Explorer. We find a single detection in an averaged periodogram comprising 30 bursts from SGR 1806-20, with a frequency of 57 Hz and a width of 5 Hz, remarkably similar to a giant flare QPO <span class="hlt">observed</span> from SGR 1900+14. This QPO fits naturally within the framework of global magneto-elastic torsional oscillations employed to explain giant flare QPOs. Additionally, we uncover a limit on the applicability of Fourier analysis for light curves with low background count rates and strong variability on short timescales. In this regime, standard Fourier methodology and more sophisticated Fourier analyses fail in equal parts by yielding an unacceptably large number of false-positive detections. This problem is not straightforward to solve in the Fourier domain. Instead, we show how simulations of light curves can offer a viable solution for QPO searches in these light curves.</p> <div class="credits"> <p class="dwt_author">Huppenkothen, D.; Heil, L. M.; Watts, A. L.; Gö?ü?, E.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">234</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2008JGRD..113.0C01M"> <span id="translatedtitle">Aerosol direct radiative forcing over Djougou (northern Benin) during the African Monsoon Multidisciplinary Analysis dry season experiment (Special <span class="hlt">Observation</span> <span class="hlt">Period</span>-0)</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The purpose of this work is to investigate the direct radiative forcing of aerosols over the supersite of Djougou (northern Benin) during the African Monsoon Multidisciplinary Analyses dry season experiment. We focus our simulations on the top of atmosphere, bottom of atmosphere, and atmosphere radiative forcings. During the dry season <span class="hlt">period</span>, Sun photometer measurements indicate a rather turbid atmosphere with a mean aerosol optical depth for the overall <span class="hlt">period</span> of 0.78 ± 0.24 (at 440 nm). The aerosol absorption coefficient estimated at the surface ranged between 2.3 and 37.3 Mm-1 (mean value 15.2 ± 10.6 Mm-1 at 520 nm) and the scattering coefficient between 44.5 and 232.3 Mm-1 (mean 145 ± 59 Mm-1 at 520 nm). This leads to a single scattering albedo of between 0.81 and 0.98 (at 520 nm) with a mean (and standard deviation) value of 0.91 ± 0.05, indicating moderately absorbing aerosols. In parallel, micropulse lidar measurements indicate the presence of two distinct aerosol layers, with a first one located between the surface and 1 km and a second one located above 1.5-4.0 km. On the basis of surface and aircraft <span class="hlt">observations</span>, sunphotometer measurements, lidar profiles, and Moderate Resolution Imagaing Spectroradiometer sensor an estimation of the daily clear sky direct radiative forcing has been estimated for the 17-24 January 2006 <span class="hlt">period</span>. Simulations indicate that aerosols reduce significantly the solar energy reaching the surface (mean ?FBOA = -61.5 W/m2) by reflection to space (mean ?FTOA = -18.4 W/m2) but predominantly by absorption of the solar radiation into the atmosphere (mean ?FATM = +43.1 W/m2). The mean heating rate at the surface and within the elevated biomass burning layer is considerably enhanced by 1.50 and 1.90 K day-1, respectively.</p> <div class="credits"> <p class="dwt_author">Mallet, M.; Pont, V.; Liousse, C.; Gomes, L.; Pelon, J.; Osborne, S.; Haywood, J.; Roger, J. C.; Dubuisson, P.; Mariscal, A.; Thouret, V.; Goloub, P.</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">235</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=2692861"> <span id="translatedtitle">Impact of infection control activities on the rate of needle stick injuries at a tertiary care hospital of Pakistan over a <span class="hlt">period</span> of six years: an <span class="hlt">observational</span> study</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Background Accidental exposure to blood and body fluids is frequent among health care workers. They are at high risk of nosocomial transmission of blood borne pathogens due to injuries caused by used sharps. We are reporting impact of surveillance and educational program on the rate of needle stick injuries among health care workers at a tertiary care hospital in Pakistan. Methods At Aga Khan University Hospital sharp injuries are reported to infection control office. To reduce these incidents a quality improvement project was inducted in the year 2005. Health care workers were educated; surveillance data from 2002 to 2007 was analyzed and compared with various risk factors. Results During study <span class="hlt">period</span> 1382 incidents were reported. Junior doctors sustained highest number of injuries (n = 394; 28.5%) followed by registered nurses (n = 283; 20.4%). Highest number of incidents was reported during blood collection (19%). An increasing trend was <span class="hlt">observed</span> in the pre intervention years (2002–04). However noticeable fall was noted in the post intervention <span class="hlt">period</span> that is in year 2006 and 2007. Major decline was noted among nurses (from 13 to 5 NSI/100 FTE/year). By relating and comparing the rates with various activities directly linked with the use of syringes a significant reduction in incidents were found including; hospital admissions (p-value 0.01), surgeries and procedures performed (p = 0.01), specimens collected in the laboratory (p = 0.001) and patients visits in clinics (p = 0.01). Conclusion We report significant reduction in needle stick injuries especially during post intervention study <span class="hlt">period</span>. This is being achieved by constant emphasis on improving awareness by regular educational sessions, implemented as a quality improvement project. PMID:19480683</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate">2009-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">236</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/22037134"> <span id="translatedtitle">YELLOW HYPERGIANTS SHOW LONG SECONDARY <span class="hlt">PERIODS</span>?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">There is <span class="hlt">observational</span> evidence that intermittent long secondary <span class="hlt">periods</span> of {approx}1000 days are present in the well-<span class="hlt">observed</span> yellow hypergiants {rho} Cas and HR 8752. The long secondary <span class="hlt">period</span> is interpreted here as the turnover time of giant convection cells in the convective envelope, as has been already <span class="hlt">suggested</span> in the case of red giants and supergiants of high luminosity. The <span class="hlt">observed</span> secondary <span class="hlt">periods</span> and surface radial velocities of {rho} Cas and HR 8752 agree with the theoretical predictions, within the expected errors. These results support a theoretical interpretation that now covers the entire initial mass range from 1 to 50 M{sub Sun} for luminous cool stars.</p> <div class="credits"> <p class="dwt_author">Stothers, Richard B. [NASA Goddard Institute for Space Studies, 2880 Broadway, New York, NY 10025 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">237</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19940017132&hterms=depression+scale&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Ddepression%2Bscale"> <span id="translatedtitle">A synoptic-scale overview of the TOGA COARE intensive <span class="hlt">observing</span> <span class="hlt">period</span> November 1992 to February 1993 based on analyses from US operational global data assimilation systems</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The operational global analyses from the two major U.S. numerical weather prediction centers, the Navy's Fleet Numerical Oceanography Center and the National Meteorological Center, are used to describe the synoptic-scale features of the 1 Nov. 1992 to 28 Feb. 1993 TOGA COARE intensive <span class="hlt">observing</span> <span class="hlt">period</span> (IOP). TOGA COARE is an international field experiment in which a large number of research scientists from the Goddard Laboratory for Atmospheres (Code 910) and the Laboratory for Hydrospheres (Code 970) participated. Two high-amplitude intraseasonal (30-60 day) oscillations passed through the TOGA COARE <span class="hlt">observational</span> network located in the equatorial western Pacific. Associated with the oscillations were two 6-10 day <span class="hlt">periods</span> of persistent westerly surface winds at the equator or 'westerly wind bursts.' These events are depicted through time series and time-longitude cross sections of divergence/velocity potential, surface winds, precipitation, ocean mixed-layer depth, and sea surface temperature. The high and low frequency components of the flow in which the intraseasonal oscillations were embedded are shown using seasonal, monthly, and 5-day averages of the surface, 850 and 200 mb winds, precipitation, and sea-level pressure, and a time-longitude cross section of tropical cyclone activity. Independent verification of precipitation comes from near real-time satellite estimates, and a reference climatology is given based on 9 years of ECMWF analyses. Daily 00 UTC analyses of surface winds and sea-level pressure for the entire western Pacific and Indian Ocean are provided to trace the evolution of individual synoptic events.</p> <div class="credits"> <p class="dwt_author">Fiorino, M.; Lord, S. J.; Lau, W. K.-M.; Phoebus, P. A.; Strey, C. G.</p> <p class="dwt_publisher"></p> <p class="publishDate">1993-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">238</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19960021096&hterms=green+cloud+computing&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dgreen%2Bcloud%2Bcomputing"> <span id="translatedtitle">Cloud Properties Derived From GOES-7 for Spring 1994 ARM Intensive <span class="hlt">Observing</span> <span class="hlt">Period</span> Using Version 1.0.0 of ARM Satellite Data Analysis Program</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">This document describes the initial formulation (Version 1.0.0) of the Atmospheric Radiation Measurement (ARM) program satellite data analysis procedures. Techniques are presented for calibrating geostationary satellite data with Sun synchronous satellite radiances and for converting narrowband radiances to top-of-the-atmosphere fluxes and albedos. A methodology is documented for combining geostationary visible and infrared radiances with surface-based temperature <span class="hlt">observations</span> to derive cloud amount, optical depth, height, thickness, temperature, and albedo. The analysis is limited to two grids centered over the ARM Southern Great Plains central facility in north-central Oklahoma. Daytime data taken during 5 Apr. - 1 May 1994, were analyzed on the 0.3 deg and 0.5 deg latitude-longitude grids that cover areas of 0.9 deg x 0.9 deg and 10 deg x 14 deg, respectively. Conditions ranging from scattered low cumulus to thin cirrus and thick cumulonimbus occurred during the study <span class="hlt">period</span>. Detailed comparisons with hourly surface <span class="hlt">observations</span> indicate that the mean cloudiness is within a few percent of the surface-derived sky cover. Formats of the results are also provided. The data can be accessed through the World Wide Web computer network.</p> <div class="credits"> <p class="dwt_author">Minnis, Patrick; Smith, William L., Jr.; Garber, Donald P.; Ayers, J. Kirk; Doelling, David R.</p> <p class="dwt_publisher"></p> <p class="publishDate">1995-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">239</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19760031346&hterms=cahill&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D60%26Ntt%3Dcahill"> <span id="translatedtitle">Explorer 45 /S3-A/ <span class="hlt">observations</span> of the magnetosphere and magnetopause during the August 4-6, 1972, magnetic storm <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The Explorer 45 (S3-A) satellite performed extensive field and particle measurements in the heart of the magnetosphere during the double magnetic storm <span class="hlt">period</span> of August 4-6, 1972. Both the ground level magnetic records and the magnetic field deformations measured along the orbit by the satellite indicated the existence of only a moderate ring current. This was confirmed by the measurements of the total proton energy density by the on-board particle detectors, which showed a maximum energy density less than the densities <span class="hlt">observed</span> during the December 1971 and June 1972 magnetic storms. The plasmapause in the noon quadrant was eroded continuously from the onset of the first storm at the beginning of August 4 to an altitude below L = 2.07 at about 1800 hours on August 5. Throughout the entire orbit during which the second sudden commencement occurred, a large amount of low-frequency electric and magnetic field noise was encountered. The most remarkable <span class="hlt">observation</span> during this orbit was the contraction of the magnetopause to distances inside the satellite location at L = 5.2.</p> <div class="credits"> <p class="dwt_author">Hoffman, R. A.; Maynard, N. C.; Smith, P. H.; Cahill, L. J., Jr.; Anderson, R. R.; Gurnett, D. A.; Fritz, T. A.; Williams, D. J.; Konradi, A.</p> <p class="dwt_publisher"></p> <p class="publishDate">1975-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">240</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013P%26SS...84...28A"> <span id="translatedtitle">The ~10 hour modulation of the relativistic electron spectrum as a result of the <span class="hlt">periodic</span> motion of the Jovian outer magnetosphere layer: Ulysses <span class="hlt">observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We analyze relativistic (E>3 MeV) electron <span class="hlt">observations</span> during the dayside inbound trajectory of Ulysses (day 33 to day 38, 1992) in the Jovian magnetosphere and we demonstrate that the continuous presence of a relativistic electron layer at higher north latitudes (Ulysses reached ~40° lat. during closest approach the planet). In particular, we evaluated the cross-B field anisotropy of relativistic (E>3 MeV) electrons intensity by the COSPIN/HET detector onboard Ulysses, and we found that between the times of plasma sheet crossings/approaches, when Ulysses was found far from the magnetodisc, at higher north latitudes, local increases in the relativistic electron intensity and intensity gradient in the northward direction were persistently <span class="hlt">observed</span>. We also found that (1) the well known ~10 h separated relativistic electron spectral index peaks (spectral softening) and (2) the detection of relativistic electron intensity gradient in the northward direction are related phenomena. We infer that phenomenon 1 and 2 are explained by the ~10 h <span class="hlt">periodic</span> upward-downward motion of the Jovian magnetosphere, and consequently of the outer magnetosphere relativistic electron layer. ?he above results extends earlier results for low energy electrons and energetic protons (Anagnostopoulos et al., 1998, 2001b) to relativistic electron phenomena, and provide strong evidence, for the first time, that the well known ~10 h rocking of the relativistic electron spectrum in the outer magnetosphere (the so called "clock phenomenon") is a spatial and not a temporal effect, as was earlier hypothesized (Simpson et al.,1992).</p> <div class="credits"> <p class="dwt_author">Anagnostopoulos, G. C.; Karanikola, I.; Marhavilas, P. K.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-08-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_11");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' 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class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_12");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' href="#">4</a> <a onClick='return showDiv("page_5");' href="#">5</a> <a onClick='return showDiv("page_6");' href="#">6</a> <a onClick='return showDiv("page_7");' href="#">7</a> <a onClick='return showDiv("page_8");' href="#">8</a> <a onClick='return showDiv("page_9");' href="#">9</a> <a onClick='return showDiv("page_10");' href="#">10</a> <a onClick='return showDiv("page_11");' href="#">11</a> <a onClick='return showDiv("page_12");' href="#">12</a> <a style="font-weight: bold;">13</a> <a onClick='return showDiv("page_14");' href="#">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a onClick='return showDiv("page_16");' href="#">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a onClick='return showDiv("page_21");' href="#">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_14");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">241</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2008ApJ...681..693O"> <span id="translatedtitle">Drift Effects and the Cosmic Ray Density Gradient in a Solar Rotation <span class="hlt">Period</span>: First <span class="hlt">Observation</span> with the Global Muon Detector Network (GMDN)</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We present for the first time hourly variations of the spatial density gradient of 50 GeV cosmic rays within a sample solar rotation <span class="hlt">period</span> in 2006. By inversely solving the diffusive flux equation, including the drift, we deduce the gradient from the anisotropy that is derived from the <span class="hlt">observation</span> made by the Global Muon Detector Network (GMDN). The anisotropy obtained by applying a new analysis method to the GMDN data is precise and free from atmospheric temperature effects on the muon count rate recorded by ground-based detectors. We find the derived north-south gradient perpendicular to the ecliptic plane is oriented toward the heliospheric current sheet (HCS; i.e., southward in the toward sector of the interplanetary magnetic field [IMF] and northward in the away sector). The orientation of the gradient component parallel to the ecliptic plane remains similar in both sectors, with an enhancement of its magnitude seen after the Earth crosses the HCS. These temporal features are interpreted in terms of a local maximum of the cosmic ray density at the HCS. This is consistent with the prediction of the drift model for the A<0 epoch. By comparing the <span class="hlt">observed</span> gradient with the numerical prediction of a simple drift model, we conclude that particle drifts in the large-scale magnetic field play an important role in organizing the density gradient, at least in the present A<0 epoch. We also found that corotating interaction regions did not have such a notable effect. <span class="hlt">Observations</span> with the GMDN provide us with a new tool for investigating cosmic-ray transport in the IMF.</p> <div class="credits"> <p class="dwt_author">Okazaki, Y.; Fushishita, A.; Narumi, T.; Kato, C.; Yasue, S.; Kuwabara, T.; Bieber, J. W.; Evenson, P.; Da Silva, M. R.; Dal Lago, A.; Schuch, N. J.; Fujii, Z.; Duldig, M. L.; Humble, J. E.; Sabbah, I.; Kóta, J.; Munakata, K.</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">242</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014ACP....14.7909K"> <span id="translatedtitle">Long-term MAX-DOAS network <span class="hlt">observations</span> of NO2 in Russia and Asia (MADRAS) during the <span class="hlt">period</span> 2007-2012: instrumentation, elucidation of climatology, and comparisons with OMI satellite <span class="hlt">observations</span> and global model simulations</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We conducted long-term network <span class="hlt">observations</span> using standardized Multi-Axis Differential optical absorption spectroscopy (MAX-DOAS) instruments in Russia and ASia (MADRAS) from 2007 onwards and made the first synthetic data analysis. At seven locations (Cape Hedo, Fukue and Yokosuka in Japan, Hefei in China, Gwangju in Korea, and Tomsk and Zvenigorod in Russia) with different levels of pollution, we obtained 80 927 retrievals of tropospheric NO2 vertical column density (TropoNO2VCD) and aerosol optical depth (AOD). In the technique, the optimal estimation of the TropoNO2VCD and its profile was performed using aerosol information derived from O4 absorbances simultaneously <span class="hlt">observed</span> at 460-490 nm. This large data set was used to analyze NO2 climatology systematically, including temporal variations from the seasonal to the diurnal scale. The results were compared with Ozone Monitoring Instrument (OMI) satellite <span class="hlt">observations</span> and global model simulations. Two NO2 retrievals of OMI satellite data (NASA ver. 2.1 and Dutch OMI NO2 (DOMINO) ver. 2.0) generally showed close correlations with those derived from MAX-DOAS <span class="hlt">observations</span>, but had low biases of up to ~50%. The bias was distinct when NO2 was abundantly present near the surface and when the AOD was high, <span class="hlt">suggesting</span> a possibility of incomplete accounting of NO2 near the surface under relatively high aerosol conditions for the satellite <span class="hlt">observations</span>. Except for constant biases, the satellite <span class="hlt">observations</span> showed nearly perfect seasonal agreement with MAX-DOAS <span class="hlt">observations</span>, <span class="hlt">suggesting</span> that the analysis of seasonal features of the satellite data were robust. Weekend reduction in the TropoNO2VCD found at Yokosuka and Gwangju was absent at Hefei, implying that the major sources had different weekly variation patterns. While the TropoNO2VCD generally decreased during the midday hours, it increased exceptionally at urban/suburban locations (Yokosuka, Gwangju, and Hefei) during winter. A global chemical transport model, MIROC-ESM-CHEM (Model for Interdisciplinary Research on Climate-Earth System Model-Chemistry), was validated for the first time with respect to background NO2 column densities during summer at Cape Hedo and Fukue in the clean marine atmosphere.</p> <div class="credits"> <p class="dwt_author">Kanaya, Y.; Irie, H.; Takashima, H.; Iwabuchi, H.; Akimoto, H.; Sudo, K.; Gu, M.; Chong, J.; Kim, Y. J.; Lee, H.; Li, A.; Si, F.; Xu, J.; Xie, P.-H.; Liu, W.-Q.; Dzhola, A.; Postylyakov, O.; Ivanov, V.; Grechko, E.; Terpugova, S.; Panchenko, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-08-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">243</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25748583"> <span id="translatedtitle">Field <span class="hlt">observation</span> of morpho-dynamic processes during storms at a Pacific beach, Japan: Role of long-<span class="hlt">period</span> waves in storm-induced berm erosion.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Many ultrasonic wave gages were placed with a small spacing across the swash zone to monitor either sand level or water level. Continuous monitoring conducted for a few years enabled the collection of data on the change in wave properties as well as swash-zone profiles. Data sets including two cases of large-scale berm erosion were analyzed. The results showed that 1) shoreline erosion started when high waves with significant power in long-<span class="hlt">period</span> (1 to 2 min.) waves reached the top of a well-developed berm with the help of rising tide; 2) the beach in the swash zone was eroded with higher elevation being more depressed, while the bottom elevation just outside the swash zone remained almost unchanged; and 3) erosion stopped in a few hours after the berm was completely eroded or the swash-zone slope became uniformly mild. These findings strongly <span class="hlt">suggest</span> that long waves play a dominant role in the swash-zone dynamics associated with these erosional events. PMID:25748583</p> <div class="credits"> <p class="dwt_author">Mizuguchi, Masaru; Seki, Katsumi</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">244</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://peggysue.as.utexas.edu/SIRTF/PAPERS/pap79.pub.pdf"> <span id="translatedtitle">Testing the Disk Regulation Paradigm with Spitzer <span class="hlt">Observations</span>. I. Rotation <span class="hlt">Periods</span> of Pre-Main-Sequence Stars in the IC 348 Cluster</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">We present 105 stellar rotation <span class="hlt">periods</span> in the young cluster IC 348, 75 of which are new detections, increasing the total number of known <span class="hlt">periods</span> in this cluster to 143. The <span class="hlt">period</span> distribution resembles that seen in the heart of the Orion Nebula cluster by Herbst and colleagues. Stars estimated to be less massive than 0.25 Msolar show a unimodal</p> <div class="credits"> <p class="dwt_author">Lucas Cieza; Nairn Baliber</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">245</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014NHESD...2..649M"> <span id="translatedtitle">Towards a new BOLAM-MOLOCH suite for the SIMM forecasting system: implementation of an optimised configuration for the HyMeX Special <span class="hlt">Observation</span> <span class="hlt">Periods</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">In this work, the performance of two versions of the Sistema Idro-Meteo-Mare (SIMM) forecasting system, aiming at predicting weather, waves and sea surge in the Mediterranean basin and, in particular, around the Italian coasts, are compared for two high-impact case studies corresponding to the Intense Operation <span class="hlt">Period</span> (IOP) 16 and 18 of the first monitoring campaign of the HYdrological cycle in Mediterranean EXperiment (HyMeX). The first SIMM version tested - currently operational - is based on the meteorological hydrostatic BOlogna Limited Area Model (BOLAM) one-way nested over two domains, the Mediterranean-embedded Costal WAve Forecasting system (Mc-WAF), and the Shallow water HYdrodynamic Finite Element Model (SHYFEM). The second version tested is the one initially implemented for the HyMeX monitoring campaigns, which is composed by an optimised new configuration of BOLAM defined over a wider, higher-resolution domain, the nonhydrostatic convection permitting model MOLOCH, the Mc-WAF component, and SHYFEM. Both SIMM versions are initialised with data from the European Centre for Medium-Range Weather Forecasts (ECMWF) Integrated Forecasting System (IFS). The accumulated precipitation obtained by applying all the above meteorological model chains at the two case studies is compared with <span class="hlt">observations</span>. In general, the precipitation forecast quality turns out to improve with increasing resolution, the best result being obtained with the MOLOCH model. Storm surge and tidal forecasts, obtained by forcing SHYFEM with the BOLAM and ECMWF IFS surface wind and atmospheric pressure fields, are compared with <span class="hlt">observations</span> of tidal elevation measured at the ISPRA "Punta della Salute" tide-gauge, located in the Lagoon of Venice. Results indicate that, for the IOP18, short-term forecasts obtained with BOLAM outperform the ECMWF IFS one, while the opposite seems apparently true for longer-term predictions.</p> <div class="credits"> <p class="dwt_author">Mariani, S.; Casaioli, M.; Malguzzi, P.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">246</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19900015536&hterms=level+rise&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D30%26Ntt%3Dlevel%2Brise"> <span id="translatedtitle">Summary of Sonic Boom Rise Times <span class="hlt">Observed</span> During FAA Community Response Studies over a 6-Month <span class="hlt">Period</span> in the Oklahoma City Area</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The sonic boom signature data acquired from about 1225 supersonic flights, over a 6-month <span class="hlt">period</span> in 1964 in the Oklahoma City area, was enhanced with the addition of data relating to rise times and total signature duration. These later parameters, not available at the time of publication of the original report on the Oklahoma City sonic boom exposures, are listed in tabular form along with overpressure, positive impulse, positive duration, and waveform category. Airplane operating information along with the surface weather <span class="hlt">observations</span> are also included. Sonic boom rise times include readings to the 1/2, 3/4, and maximum overpressure values. Rise time relative probabilities for various lateral locations from the ground track of 0, 5, and 10 miles are presented along with the variation of rise times with flight altitude. The tabulated signature data, along with corresponding airplane operating conditions and surface and upper level atmospheric information, are also available on electronic files to provide it in the format for more efficient and effective utilization.</p> <div class="credits"> <p class="dwt_author">Maglieri, Domenic J.; Sothcott, Victor E.</p> <p class="dwt_publisher"></p> <p class="publishDate">1990-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">247</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010ApJ...722..343D"> <span id="translatedtitle">X-ray, FUV, and UV <span class="hlt">Observations</span> of ? Centauri B: Determination of Long-term Magnetic Activity Cycle and Rotation <span class="hlt">Period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Over the last couple of decades we have been carrying out a study of stellar magnetic activity, dynamos, atmospheric physics, and spectral irradiances from a sample of solar-type G0-5 V stars with different ages. One of the major goals of this program is to study the evolution of the Sun's X-ray through NUV spectral irradiances with age. Of particular interest is the determination of the young Sun's elevated levels of high-energy fluxes because of the critical roles that X-ray (coronal) through FUV (transition region (TR), chromospheric) emissions play on the photochemical and photoionization evolution (and possible erosion) of early, young planetary atmospheres and ionospheres. Motivated by the current exoplanetary search missions (such as Kepler and CoRoT, along with the planned Space Interferometry Mission and Darwin/Terrestrial Planet Finder missions) that are hunting for Earth-size planets in the habitable zones (liquid water) of nearby main-sequence G-M stars, we are expanding our program to cooler, less luminous, but very importantly, much more numerous main-sequence K-type stars, such as ? Centauri B. The long life (2-3× longer than the Sun) and slow evolution of K stars provide nearly constant energy sources for possible hosted planets. This program parallels our "Sun in Time" program, but extends the study to stars with deeper convective zone depths. Presented here are X-ray (coronal; ROSAT, Chandra, XMM-Newton), UV (TR; International Ultraviolet Explorer (IUE)), NUV (chromospheric; IUE), and recently acquired FUV (TR/chromospheric; FUSE Cycles 7/8) <span class="hlt">observations</span> of the K1 V star ? Cen B (HD 128621; V = 1.33; (B - V) = +0.88; ? = 5.6 ± 0.6 Gyr). These combined high-energy measures provide a more complete look into the nature of ? Cen B's magnetic activity and X-ray-UV radiances. We find that ? Cen B has exhibited significant long-term variability in X-ray through NUV emission fluxes, indicating a solar-like long-term activity cycle of P cycle = 8.84 ± 0.4 years. In addition, analysis of the short-term rotational modulation of mean light due to the effects of magnetically active regions has yielded a well-determined rotation <span class="hlt">period</span> of P rotation = 36.2 ± 1.4 days. ? Cen B is the only old main-sequence K star with a reliably determined age and rotation <span class="hlt">period</span>, and for early K stars, as in the case of the Sun for G2 V stars, is an important calibrator for stellar age/rotation/activity relations.</p> <div class="credits"> <p class="dwt_author">DeWarf, L. E.; Datin, K. M.; Guinan, E. F.</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-10-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">248</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013EGUGA..15..705G"> <span id="translatedtitle">Inter-annual variability of aerosol optical depth over the tropical Atlantic Ocean based on MODIS-Aqua <span class="hlt">observations</span> over the <span class="hlt">period</span> 2002-2012</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The tropical Atlantic Ocean is affected by dust and biomass burning aerosol loads transported from the western parts of the Saharan desert and the sub-Sahel regions, respectively. The spatial and temporal patterns of this transport are determined by the aerosol emission rates, their deposition (wet and dry), by the latitudinal shift of the Intertropical Convergence Zone (ITCZ) and the prevailing wind fields. More specifically, in summer, Saharan dust aerosols are transported towards the Atlantic Ocean, even reaching the Gulf of Mexico, while in winter the Atlantic Ocean transport takes place in more southern latitudes, near the equator, sometimes reaching the northern parts of South America. In the later case, dust is mixed with biomass burning aerosols originating from agricultural activities in the sub-Sahel, associated with prevailing north-easterly airflow (Harmattan winds). Satellite <span class="hlt">observations</span> are the appropriate tool for describing this African aerosol export, which is important to atmospheric, oceanic and climate processes, offering the advantage of complete spatial coverage. In the present study, we use satellite measurements of aerosol optical depth at 550nm (AOD550nm), on a daily and monthly basis, derived from MODIS-Aqua platform, at 1ox1o spatial resolution (Level 3), for the <span class="hlt">period</span> 2002-2012. The primary objective is to determine the pixel-level and regional mean anomalies of AOD550nm over the entire study <span class="hlt">period</span>. The regime of the anomalies of African export is interpreted in relation to the aerosol source areas, precipitation, wind patterns and temporal variability of the North Atlantic Oscillation Index (NAOI). In order to ensure availability of AOD over the Sahara desert, MODIS-Aqua Deep Blue products are also used. As for precipitation, Global Precipitation Climatology Project (GPCP) data at 2.5ox2.5o are used. The wind fields are taken from the National Center for Environmental Prediction (NCEP). Apart from the regime of African aerosol export in the northern tropical Atlantic Ocean, it is also attempted to examine possible relationships between African dust export and NAO, with emphasis on identifying possible effects of the former to the later. This might be possible since aerosols through their radiative effects are known to affect atmospheric dynamics, for example modifying precipitation or the tracks and intensity of cyclones. Of course, such aerosol feedbacks on atmospheric dynamics and teleconnections are certainly complex and difficult to study, requiring the use of climate models, which is planned in a next step of the study.</p> <div class="credits"> <p class="dwt_author">Gkikas, Antonis; Hatzianastassiou, Nikolaos</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">249</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4015388"> <span id="translatedtitle">Deepening Sleep by Hypnotic <span class="hlt">Suggestion</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Study Objectives: Slow wave sleep (SWS) plays a critical role in body restoration and promotes brain plasticity; however, it markedly declines across the lifespan. Despite its importance, effective tools to increase SWS are rare. Here we tested whether a hypnotic <span class="hlt">suggestion</span> to “sleep deeper” extends the amount of SWS. Design: Within-subject, placebo-controlled crossover design. Setting: Sleep laboratory at the University of Zurich, Switzerland. Participants: Seventy healthy females 23.27 ± 3.17 y. Intervention: Participants listened to an auditory text with hypnotic <span class="hlt">suggestions</span> or a control tape before napping for 90 min while high-density electroencephalography was recorded. Measurements and Results: After participants listened to the hypnotic <span class="hlt">suggestion</span> to “sleep deeper” subsequent SWS was increased by 81% and time spent awake was reduced by 67% (with the amount of SWS or wake in the control condition set to 100%). Other sleep stages remained unaffected. Additionally, slow wave activity was significantly enhanced after hypnotic <span class="hlt">suggestions</span>. During the hypnotic tape, parietal theta power increases predicted the hypnosis-induced extension of SWS. Additional experiments confirmed that the beneficial effect of hypnotic <span class="hlt">suggestions</span> on SWS was specific to the hypnotic <span class="hlt">suggestion</span> and did not occur in low <span class="hlt">suggestible</span> participants. Conclusions: Our results demonstrate the effectiveness of hypnotic <span class="hlt">suggestions</span> to specifically increase the amount and duration of slow wave sleep (SWS) in a midday nap using objective measures of sleep in young, healthy, <span class="hlt">suggestible</span> females. Hypnotic <span class="hlt">suggestions</span> might be a successful tool with a lower risk of adverse side effects than pharmacological treatments to extend SWS also in clinical and elderly populations. Citation: Cordi MJ, Schlarb AA, Rasch B. Deepening sleep by hypnotic <span class="hlt">suggestion</span>. SLEEP 2014;37(6):1143-1152. PMID:24882909</p> <div class="credits"> <p class="dwt_author">Cordi, Maren J.; Schlarb, Angelika A.; Rasch, Björn</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">250</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014SPIE.9262E..0JL"> <span id="translatedtitle">Seasonal variation of aerosol vertical distributions in the middle and lower troposphere in Beijing and surrounding area during haze <span class="hlt">periods</span> based on CALIPSO <span class="hlt">observation</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The data from CALIPSO (Cloud-Aerosol Lidar and Infrared Pathfinder Satellite <span class="hlt">Observations</span>) satellite was used to analyze the aerosol micro-physical properties over Beijing and surrounding area during haze <span class="hlt">periods</span> from 2007 to 2008 in this paper. The results showed as follows. The values of TABC (total attenuated backscatter coefficient) for aerosols accounted for about 25% with varying altitudes. The aerosol scattering ability little changed from 0-4 km, showing that the aerosol layer evenly distribute. At different altitude ranges (0-1, 1-2, 2-3 and 3-4 km above ground level), values of TABC almost concentrate in the range of 2.5×10-3 -4.5×10-3 km-1.sr-1. In spring, summer and winter, aerosol scattering has the similar variation, with the maximum of TABC ranging from 3.5×10-3 km-1.sr-1 to 4.5×10-3 km-1.sr-1, while the maximum of TABC in autumn is from 1.5×10-3 km-1.sr-1 to 2.5×10-3 km-1.sr-1. Aerosol shape and size are characterized by VDR (volume depolarization ratio) and TACR (total attenuated color ratio). Aerosols with VDR greater than 10% were more than the ones with VDR less than 10% at the same altitude range. Notably, aerosols with smaller VDR (0-10%) appeared more frequently in autumn than those in the other three seasons. For each altitude range, aerosols with TACR ranging from 0-0.2 contributed much more than those with TACR ranging from 1.8-2.0. The size of aerosols in summer was the largest and that in autumn was the smallest in middle and lower troposphere.</p> <div class="credits"> <p class="dwt_author">Liu, Qiong; Ma, Xiaojun; Jin, Hongchun; Chen, Yonghang; Yu, Yang; Zhang, Hua; Cai, Changjie; Wang, Yuhui; Li, Hao</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-11-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">251</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3278338"> <span id="translatedtitle">Remission in schizophrenia: results of cross-sectional with 6-month follow-up <span class="hlt">period</span> and 1-year <span class="hlt">observational</span> therapeutic studies in an outpatient population</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Background A standardized definition of remission criteria in schizophrenia was proposed by the International group of NC Andreasen in 2005 (low symptom threshold for the eight core Positive and Negative Syndrome Scale (PANSS) symptoms for at least 6 consecutive months). Methods A cross-sectional study of remission rate, using a 6-month follow-up to assess symptomatic stability, was conducted in two healthcare districts (first and second) of an outpatient psychiatric service in Moscow. The key inclusion criteria were outpatients with an International Classification of Diseases, 10th edition (ICD-10) diagnosis of schizophrenia or schizoaffective disorder. Remission was assessed using modern criteria (severity and time criteria), PANSS and Global Assessment of Functioning (GAF). Patients who were stable but did not satisfied the symptomatic criteria were included in a further 1-year <span class="hlt">observational</span> study, with the first group (first district) receiving risperidone (long-acting, injectable) (RLAI) and the second group (second district) continuing to receiving routine treatment. Symptoms were assessed with PANSS, social functioning with the personal and social performance scale, compliance with rating of medication influences scale, and extrapyramidal side effects with the Simpson-Angus scale. Results Only 64 (31.5%) of 203 outpatients met the criteria for symptomatic remission in the cross-sectional study, but at the end of the 6-month follow-up <span class="hlt">period</span>, 158 (77.8%) were stable (irrespective of remission status). Among these only 53 (26.1%) patients fulfilled the remission criteria. The <span class="hlt">observational</span> study had 42 stable patients in the RLAI group and 35 in the routine treatment group: 19.0% in the RLAI group and 5.7% in the control group met remission criteria after 12 months of therapy. Furthermore, reduction of PANSS total and subscale scores, as well as improvement in social functioning, was more significant in the first group. Conclusions Only around one-quarter of our outpatient schizophrenic population met full remission criteria. Use of RLAI gave a better remission rate than achieved in standard care with routine treatment. Criteria for remission should take into account clinical course and functioning to support clinical care. PMID:22221826</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">252</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://lubbock.tamu.edu/files/2011/10/weedcontrolinforages_13.pdf"> <span id="translatedtitle"><span class="hlt">SUGGESTIONS</span> FOR WEED CONTROL IN</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">B-5038 10-98 <span class="hlt">SUGGESTIONS</span> FOR WEED CONTROL IN PASTURES AND FORAGES Texas Agricultural Extension;4 <span class="hlt">Suggestions</span> for Weed Control in Pastures and Forages Dr. Paul A. Baumann, Extension Weed Specialist Dr. David as a guide for controlling weeds in pasture and forages. Labeled rates and restrictions change constantly</p> <div class="credits"> <p class="dwt_author">Mukhtar, Saqib</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">253</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/1997JGR...10226225N"> <span id="translatedtitle">Short-<span class="hlt">period</span> fluctuations of the diurnal tide <span class="hlt">observed</span> with low-latitude MF and meteor radars during CADRE: Evidence for gravity wave/tidal interactions</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">MF and meteor radar data from four equatorial and subtropical sites (Hawaii, Christmas Island, Jakarta, and Adelaide) are used to examine diurnal tide amplitude and phase variability at mesosphere and lower thermosphere altitudes. All sites exhibit significant seasonal variability, with the largest amplitude fluctuations occurring at Hawaii and Adelaide. Shorter-term variability is found to occur primarily on timescales of ˜5 to 30 days. Amplitude and phase fluctuations are well correlated among different sites on occasion, but in general, the amplitude and phase coherences are low and <span class="hlt">suggest</span> significant local influences on the tidal structures. The temporal behavior of height variations of the diurnal tide amplitude and phase is also examined. Cross correlations and cross spectra of these tidal parameters, especially between the amplitude and phase, are examined closely. The tendency for phase maxima to lead amplitude maxima is consistent with tidal modulation of gravity wave propagation and momentum fluxes, with a corresponding feedback by the gravity wave momentum flux divergences on the <span class="hlt">observed</span> tidal structures. These results substantially extend previous more limited studies of gravity wave/tidal interactions and provide a statistical basis for the possible importance of this interaction and its influences on the diurnal tidal structure.</p> <div class="credits"> <p class="dwt_author">Nakamura, T.; Fritts, D. C.; Isler, J. R.; Tsuda, T.; Vincent, R. A.; Reid, I. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">1997-11-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">254</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20040079819&hterms=tmt&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D50%26Ntt%3Dtmt"> <span id="translatedtitle">Spectral Index and Quasi-<span class="hlt">Periodic</span> Oscillation Frequency Correlation in Black Hole (BH) Sources: <span class="hlt">Observational</span> Evidence of Two Phases and Phase Transition in BHs</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Recent studies have shown that strong correlations are <span class="hlt">observed</span> between the low frequencies (1-10 Hz) of quasiperiodic oscillations (QPOs) and the spectral power law index of several Black Hole (BH) candidate sources, in low hard states, steep power-law (soft) states and in transition between these states. The <span class="hlt">observations</span> indicate that the X-ray spectrum of such state (phases) show the presence of a power-law component and are sometimes related to simultaneous radio emission indicated the probable presence of a jet. Strong QPOs (less than 20% rms) are present in the power density spectrum in the spectral range where the power-law component is dominant ( i.e. 60-90% ). This evidence contradicts the dominant long standing interpretation of QPOs as a signature of the thermal accretion disk. We present the data from the literature and our own data to illustrate the dominance of power-law index-QPO frequency correlations. We provide a model, that identifies and explains the origin of the QPOs and how they are imprinted on the properties of power-law flux component. We argue the existence of a bounded compact coronal region which is a natural consequence of the adjustment of Keplerian disk flow to the innermost sub-Keplerian boundary conditions near the central object and that ultimately leads to the formation of a transition layer (TL) between the adjustment radius and the innermost boundary. The model predicts two phases or states dictated by the photon upscattering produced in the TL: (1) hard state, in which the TL is optically thin and very hot (kT approx. greater than 50 keV) producing photon upscattering via thermal Componization; the photon spectrum index Gamma appprox.1.5 for this state is dictated by gravitational energy release and Compton cooling in an optically thin shock near the adjustment radius; (2) a soft state which is optically thick and relatively cold (approx. less than 5 keV); the index for this state, Gamma approx. 2.8 is determined by soft-photon upscattering and photon trapping in converging flow into BH. In the TL model for corona the QPO frequency vnu(sub high) is related to the gravitational (close to Keplerian) frequency nu(sub K) at the outer (adjustment) radius and nu(sub low) is related to the TL s normal mode (magnetoacoustic) oscillation frequency nu(sub MA). The <span class="hlt">observed</span> correlations between index and low and high QPO frequencies are readily explained in terms of this model. We also <span class="hlt">suggest</span> a new method for evaluation of the BH mass using the index-frequency correlation.</p> <div class="credits"> <p class="dwt_author">Titarchuk, Lev; Fiorito, Ralph</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">255</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2006tmgm.meet..483T"> <span id="translatedtitle">Spectral Index and Quasi-<span class="hlt">Periodic</span> Oscillation Frequency Correlation in Black Hole (bh) Sources:. <span class="hlt">Observational</span> Evidence of Two Phases and Phase Transition in BHs</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Recent studies have shown that strong correlations are <span class="hlt">observed</span> between the low frequencies (1-10 Hz) of quasiperiodic oscillations (QPOs) and the spectral power law index of several Black Hole (BH) candidate sources, in low hard state, steep power-law (soft) state and in transition between these states. The <span class="hlt">observations</span> indicate that the X-ray spectrum of such state (phases) show the presence of a power-law component and are sometimes related to simultaneous radio emission indicated the probable presence of a jet. Strong QPOs (> 20% rms) are present in the power density spectrum in the spectral range where the power-law component is dominant (i.e. 60-90%). This evidence contradicts the dominant long standing interpretation of QPOs as a signature of the thermal accretion disk. We present the data from the literature and our own data to illustrate the dominance of power-law index-QPO frequency correlations. We provide a model, that identifies and explains the origin of the QPOs and how they are imprinted on the properties of power-law flux component. We argue the existence of a bounded compact coronal region which is a natural consequence of the adjustment of Keplerian disk flow to the innermost sub-Keplerian boundary conditions near the central object and that ultimately leads to the formation of a transition layer (TL) between the adjustment radius and the innermost boundary. The model predicts two phases or states dictated by the photon upscattering produced in the TL: (1) hard state, in which the TL is optically thin and very hot (kT ? 50 keV) producing photon upscattering via thermal Componization; the photon spectrum index ? ~ 1.7 for this state is dictated by gravitational energy release and Compton cooling in an optically thin shock near the adjustment radius; (2) a soft state which is optically thick and relatively cold (kT ? 5 keV); the index for this state, ? ~ 2.8 is determined by soft-photon upscattering and photon trapping in converging flow into BH. In the TL model for corona the QPO frequency ?high is related to the gravitational (close to Keplerian) frequency ?K at the outer (adjustment) radius and ?low is related to the TL's normal mode (magnetoacoustic) oscillation frequency ?MA. The <span class="hlt">observed</span> correlations between index and low and high QPO frequencies are readily explained in terms of this model. We also <span class="hlt">suggest</span> a new method for evaluation of the BH mass using the index-frequency correlation.</p> <div class="credits"> <p class="dwt_author">Titarchuck, Lev; Fiorito, Ralph</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-02-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">256</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013A%26A...557L..10N"> <span id="translatedtitle">Rotation <span class="hlt">periods</span> of 12 000 main-sequence Kepler stars: Dependence on stellar spectral type and comparison with v sin i <span class="hlt">observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Aims: We aim to measure the starspot rotation <span class="hlt">periods</span> of active stars in the Kepler field as a function of spectral type and to extend reliable rotation measurements from F-, G-, and K-type to M-type stars. Methods: Using the Lomb-Scargle periodogram we searched more than 150 000 stellar light curves for <span class="hlt">periodic</span> brightness variations. We analyzed <span class="hlt">periods</span> between 1 and 30 days in eight consecutive Kepler quarters, where 30 days is an estimated maximum for the validity of the PDC_MAP data correction pipeline. We selected stable rotation <span class="hlt">periods</span>, i.e., <span class="hlt">periods</span> that do not vary from the median by more than one day in at least six of the eight quarters. We averaged the <span class="hlt">periods</span> for each stellar spectral class according to B - V color and compared the results to archival vsini data, using stellar radii estimates from the Kepler Input Catalog. Results: We report on the stable starspot rotation <span class="hlt">periods</span> of 12 151 Kepler stars. We find good agreement between starspot velocities and vsini data for all F-, G- and early K-type stars. The 795 M-type stars in our sample have a median rotation <span class="hlt">period</span> of 15.4 days. We find an excess of M-type stars with <span class="hlt">periods</span> less than 7.5 days that are potentially fast-rotating and fully convective. Measuring photometric variability in multiple Kepler quarters appears to be a straightforward and reliable way to determine the rotation <span class="hlt">periods</span> of a large sample of active stars, including late-type stars. Table 1 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/557/L10</p> <div class="credits"> <p class="dwt_author">Nielsen, M. B.; Gizon, L.; Schunker, H.; Karoff, C.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-09-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">257</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://learningcenter.nsta.org/product_detail.aspx?id=10.2505/4/ss09_032_09_38"> <span id="translatedtitle">Current Research: Summer Reading <span class="hlt">Suggestions</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">To supplement your summer reading, NSTA's affiliates would like to <span class="hlt">suggest</span> some recent articles on education research. These articles cover a variety of topics that include diversity, technology, and science teacher retention. The abstracts of these impor</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate">2009-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">258</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/21464704"> <span id="translatedtitle">X-RAY, FUV, AND UV <span class="hlt">OBSERVATIONS</span> OF {alpha} CENTAURI B: DETERMINATION OF LONG-TERM MAGNETIC ACTIVITY CYCLE AND ROTATION <span class="hlt">PERIOD</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Over the last couple of decades we have been carrying out a study of stellar magnetic activity, dynamos, atmospheric physics, and spectral irradiances from a sample of solar-type G0-5 V stars with different ages. One of the major goals of this program is to study the evolution of the Sun's X-ray through NUV spectral irradiances with age. Of particular interest is the determination of the young Sun's elevated levels of high-energy fluxes because of the critical roles that X-ray (coronal) through FUV (transition region (TR), chromospheric) emissions play on the photochemical and photoionization evolution (and possible erosion) of early, young planetary atmospheres and ionospheres. Motivated by the current exoplanetary search missions (such as Kepler and CoRoT, along with the planned Space Interferometry Mission and Darwin/Terrestrial Planet Finder missions) that are hunting for Earth-size planets in the habitable zones (liquid water) of nearby main-sequence G-M stars, we are expanding our program to cooler, less luminous, but very importantly, much more numerous main-sequence K-type stars, such as {alpha} Centauri B. The long life (2-3x longer than the Sun) and slow evolution of K stars provide nearly constant energy sources for possible hosted planets. This program parallels our 'Sun in Time' program, but extends the study to stars with deeper convective zone depths. Presented here are X-ray (coronal; ROSAT, Chandra, XMM-Newton), UV (TR; International Ultraviolet Explorer (IUE)), NUV (chromospheric; IUE), and recently acquired FUV (TR/chromospheric; FUSE Cycles 7/8) <span class="hlt">observations</span> of the K1 V star {alpha} Cen B (HD 128621; V = 1.33; (B - V) = +0.88; {tau} = 5.6 {+-} 0.6 Gyr). These combined high-energy measures provide a more complete look into the nature of {alpha} Cen B's magnetic activity and X-ray-UV radiances. We find that {alpha} Cen B has exhibited significant long-term variability in X-ray through NUV emission fluxes, indicating a solar-like long-term activity cycle of P{sub cycle} = 8.84 {+-} 0.4 years. In addition, analysis of the short-term rotational modulation of mean light due to the effects of magnetically active regions has yielded a well-determined rotation <span class="hlt">period</span> of P{sub rotation} = 36.2 {+-} 1.4 days. {alpha} Cen B is the only old main-sequence K star with a reliably determined age and rotation <span class="hlt">period</span>, and for early K stars, as in the case of the Sun for G2 V stars, is an important calibrator for stellar age/rotation/activity relations.</p> <div class="credits"> <p class="dwt_author">DeWarf, L. E.; Guinan, E. F.; Datin, K. M., E-mail: Laurence.DeWarf@Villanova.ed [Department of Astronomy and Astrophysics, Villanova University, 800 Lancaster Avenue, Villanova, PA 19085 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-10-10</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">259</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010ffcd.confE.137S"> <span id="translatedtitle">Dynamics and evolution of tree populations and soil-vegetation relationships in Fogscapes: <span class="hlt">Observations</span> over a <span class="hlt">period</span> of 14 years at the experimental sites of Meija (Peru).</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The Fogscapes, i.e. fog-dependent landscapes, and the sub mountain drylands of the Pacific Coast from Ecuador to Northern Chile are amongst the most fragile regions of the planet. The so-called "Lomas" (i.e. Hills) ecosystems are characterised by pre-desertic flora and vegetation where the plant phenological pattern coincides with the fog season from June to December every year. The occurance of ENSO (El Niño Southern Oscillation) affects these ecosystems inducing, occasionally, a sudden change in the characteristics of the vegetation. Relics of low-density woodlands dominated by Caesalpinea spinosa and scattered trees of the same species (which during the fog season appear as savannah-like ecosystems) are still present but becoming increasingly rare due to past and present overgrazing In the experimental site of Las Cuchillas, located on the coastal hills close to Meija (Dept. Arequipa, South Peru) trees of native species (Caesalpinaea spinosa and Prosopis pallida) and exotic species (Acacia saligna, Casuarina equisetifolia, Parkinsonia aculeata) were planted in 1996, in order to look at the rehabilitation potential of the degraded "lomas" ecosystems. This paper deals with the results <span class="hlt">observed</span> over a <span class="hlt">period</span> of 14 years’ of tree growth patterns and the related results concerning the soil and habitat dynamics. Among indigenous species Caesalpinea spinosa shows the heighest rate of survival even if the height increment is low and the tree crowns tend to dry out at a height of approximately two metres, followed by the appearance of new shoots produced during the course of the seasons. The exotic Acacia saligna shows the maximum height, diameter and crown volume increments. The habitat conditions, both in term of diversity / frequency of plant and animal populations, and plant cover (LAI estimated by processing fish-eye lens images) have changed substantially over the years. A number of samples from the top mineral soil and random samples from the forest floor were collected both from the reforested test site and from the adjacent control areas were no trees had been planted. The samples were analysed for organic carbon and total nitrogen. Overall, the tree-covered soil retained much more of both elements than the non-forested areas, thus demonstrating the efficiency of the intervention carried out in terms of combatting the greenhouse effect. The various tree species planted, however, showed greatly variable capacity to promote carbon sequestration at soil level. The results referred to above are critical in understanding the plant population dynamics of pre-desertic ecosystems in response to climate change and in assessing the potential of reforestation programmes and landscape conservation strategies for the purposes of carbon sequestration.</p> <div class="credits"> <p class="dwt_author">Salbitano, F.; Calamini, G.; Certini, G.; Ortega, A.; Pierguidi, A.; Villasante, L.; Caceres, R.; Coaguila, D.; Delgado, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">260</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/6333944"> <span id="translatedtitle">Coping with paradoxes of risk communication: <span class="hlt">Observations</span> and <span class="hlt">suggestions</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The maturation of the field of risk communication has resulted in several manuals, a National Research Council review, a Society for Risk Analysis subgroup, and critics. Critics Pieter-Jan Stalen and Rob Coppock, and Harry Otway and Brian Wynne, have pointed out that much risk communication is impractical or paradoxical. In this letter, the author supports many of the criticisms of these critics, but also discusses errors and omissions in their viewpoints that he feels will inhibit progress in effective risk communication. Topics discussed are motivations for risk communication, the practicality of advice, the audience for risk communication, credibility, and whose interests are best served by risk communication. The purpose of this essay is therefore to spur further debate on the issue of risk communication. 13 refs.</p> <div class="credits"> <p class="dwt_author">Johnson, B.B. (New Jersey Dept. of Environmental Protection and Energy, Trenton (United States))</p> <p class="dwt_publisher"></p> <p class="publishDate">1993-06-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_12");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return 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<a onClick='return showDiv("page_11");' href="#">11</a> <a onClick='return showDiv("page_12");' href="#">12</a> <a onClick='return showDiv("page_13");' href="#">13</a> <a style="font-weight: bold;">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a onClick='return showDiv("page_16");' href="#">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a onClick='return showDiv("page_21");' href="#">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_15");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">261</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/8854372"> <span id="translatedtitle">Interrogative <span class="hlt">suggestibility</span> in opiate users.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">The present study investigated interrogative <span class="hlt">suggestibility</span> in opiate users. A group of patients undergoing a methadone detoxification programme in an in-patient drug treatment unit (Detox group, n = 21), and a group of residents who had come off drugs and were no longer suffering from withdrawal syndrome (Rehab group, n = 19) were compared on interrogative <span class="hlt">suggestibility</span> and various other psychological factors. Significant differences were found between the two groups, with the Detox group having more physical and psychological problems, and a higher total <span class="hlt">suggestibility</span> score in comparison with the Rehab group. These findings are discussed in relation to the context of police interrogations and the reliability of confessions made by suspects and witnesses dependent on opiates. PMID:8854372</p> <div class="credits"> <p class="dwt_author">Murakami, A; Edelmann, R J; Davis, P E</p> <p class="dwt_publisher"></p> <p class="publishDate">1996-09-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">262</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015EL....10956003T"> <span id="translatedtitle">Chiral doping effect in the B2 phase of a bent-core liquid crystal: The <span class="hlt">observation</span> of resonant X-ray satellite peaks assigned to the 5/10 layer <span class="hlt">periodic</span> structure</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We studied the details of a local layer structure in the B2 phase of bromo-containing bent-core liquid crystals mixed with a small amount of chiral molecules using microbeam resonant X-ray scattering. In this measurement, we detected the 1 ± 0.2 order satellite peaks, which <span class="hlt">suggest</span> that the B2 phase of the mixture has a long-range <span class="hlt">periodic</span> structure. Dielectric and electro-optic measurements indicate almost the same behavior as the antiferroelectric SmCAPA(B2) of pure bromo-containing bent-core liquid crystals, so that the B2 phase of the chiral mixture is also antiferroelectric, and it is concluded that the B2 phase of the chiral mixture forms a ten-layer <span class="hlt">periodic</span> structure. Such a long-range <span class="hlt">periodic</span> structure did not appear by mixing the racemate of the same compounds, which indicates the chiral effect on the long-range <span class="hlt">periodic</span> structure.</p> <div class="credits"> <p class="dwt_author">Takanishi, Yoichi; Ohtsuka, Youko; Takahashi, Yumiko; Kang, Sungmin; Iida, Atsuo</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-03-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">263</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=staple&pg=3&id=EJ891901"> <span id="translatedtitle">10 <span class="hlt">Suggestions</span> for Enhancing Lecturing</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Criticism of the lecture method remains a staple of discussion and writing in academia--and most of the time it's deserved! Those interested in improving this aspect of their teaching might wish to consider some or all of the following <span class="hlt">suggestions</span> for enhancing lectures. These include: (1) Lectures must start with a "grabber"; (2) Lectures must be…</p> <div class="credits"> <p class="dwt_author">Heitzmann, Ray</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">264</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.si.edu/Encyclopedia_SI/nmnh/ARCHAEOLOGY2007-ReadingList.pdf"> <span id="translatedtitle">ARCHAEOLOGY <span class="hlt">Suggested</span> Readings in Archaeology</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">ARCHAEOLOGY <span class="hlt">Suggested</span> Readings in Archaeology The following is a list of some of the major by those wishing more detailed information. Educators' Resources Archaeology in the Classroom. A Resource. Archaeological Institute of America. Archaeologists at Work: A Teacher's Guide to Classroom Archaeology. 2nd ed</p> <div class="credits"> <p class="dwt_author">Mathis, Wayne N.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">265</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://kuscholarworks.ku.edu/handle/1808/13613"> <span id="translatedtitle">Boolean Search <span class="hlt">Suggestions</span> in Primo</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">Poster presented at Ex Libris Users of North America (ELUNA) 2014 Meeting in Montreal, Canada April 29 - May 2, 2014. Discusses the development and assessment of a JavaScript add-on to Primo that provides Boolean search <span class="hlt">suggestions</span> based on search...</p> <div class="credits"> <p class="dwt_author">Hanrath, Scott</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-05-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">266</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=misdirection&id=EJ136430"> <span id="translatedtitle">Models: Caveats, Reflections, and <span class="hlt">Suggestions</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Noting that mathematical modeling is a relatively new phenomenon in higher education and that much can be learned from the misdirections and mistakes that characterize modeling in general, the author describes major criticisms of modeling and <span class="hlt">suggests</span> improvements, particularly in communication between modelers and potential model users. (JT)</p> <div class="credits"> <p class="dwt_author">Kirschling, Wayne R.</p> <p class="dwt_publisher"></p> <p class="publishDate">1976-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">267</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014PASJ...66S..18P"> <span id="translatedtitle">Hinode 7: Conference summary and future <span class="hlt">suggestions</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This conclusion to the seventh Hinode science meeting (2013 November in Takayama, Japan) attempts to summarise what we have learnt during the conference (mainly from the review talks) about new <span class="hlt">observations</span> from Hinode and about theories stimulated by them. <span class="hlt">Suggestions</span> for future study are also offered.</p> <div class="credits"> <p class="dwt_author">Priest, Eric</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">268</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://elibrary.unm.edu/sora/Wilson/v087n04/p0456-p0466.pdf"> <span id="translatedtitle"><span class="hlt">SUGGESTIONS</span> FOR CALCULATING NEST SUCCESS</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Reports of nesting success that do not take into account the time span of <span class="hlt">observation</span> for each nest usually understate losses, and sometimes the error can be very large. More than a decade ago I pointed out this problem and proposed a way of dealing with it (Mayfield 1960:192-204; 1961). Since that time many field students have used the method,</p> <div class="credits"> <p class="dwt_author">HAROLD F. MAYFIELD</p> <p class="dwt_publisher"></p> <p class="publishDate">1975-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">269</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=https://acswebcontent.acs.org/games/pt.html"> <span id="translatedtitle"><span class="hlt">Periodic</span> Table</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">Using the Macromedia Shockwave Player, this American Chemical Society website offers three interactive <span class="hlt">periodic</span> tables. Students can find the basic data on each element including its atomic radius, stable isotopes, melting point, and density in the first <span class="hlt">periodic</span> table tab. The website identifies different elemental groups by color. Users can view the electron configuration by selecting elements on the <span class="hlt">periodic</span> table in the second tab. The last tab offers plots of the elements' electronegativity, ionization energy, and other properties.</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">270</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20090015031&hterms=Promotion+publicity&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3DPromotion%2Bpublicity"> <span id="translatedtitle"><span class="hlt">Suggestions</span> for Popularizing Civil Aviation</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The public generally is taking very little interest in the progress of Civil Aviation, and the time has come to educate the public in aeronautics and to make them realize the far-reaching importance of air transport. Briefly, the whole problem resolves itself into discovering and applying means for bringing some of the many aspects and effects of civil aviation into the everyday lives of the public. The report <span class="hlt">suggests</span> three principal groups of methods: (1) Bring aviation into daily contact with the public. (2) Bring the public into daily contact with aviation. (3) General publicity.</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate">1926-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">271</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://earthobservatory.nasa.gov/Features/Zircon/"> <span id="translatedtitle">Ancient Crystals <span class="hlt">Suggest</span> Earlier Ocean</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">This report describes the findings of two scientists who studied the chemical makeup of crystals of zircon from rocks in Western Australia's Jack Hills. The zircon crystals are thought to be 4.5 billion years old, making them some of the oldest materials yet found on Earth. The ratios of oxygen isotopes found in the crystals <span class="hlt">suggest</span> that conditions during the Hadean Eon, the first 500 million years of Earth's history when the crystals were formed, were cooler and wetter than previously thought. Links to a glossary are embedded in the text.</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">272</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19800009695&hterms=1430&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3D1430"> <span id="translatedtitle">A sunspot <span class="hlt">periodicity</span> and the solar rotation</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">A least squares power spectrum analysis of daily sunspot numbers for the last 122 years yielded a statistically significant peak at 12.0715 plus or minus .002 days <span class="hlt">period</span>. This feature at 11.685 days (sidereal) of the sunspot spectrum is discussed in relation to the peak at 12.22 days (sidereal) which Dicke found in his oblateness data. The data is attributed to the Sun's core if the core rotates at either 12.0715 days or 24.1430 days <span class="hlt">period</span> (synodic). It is <span class="hlt">suggested</span> that spacecraft <span class="hlt">observations</span> combined with correlative analysis of solar surface features between eastern and western hemispheres could further reveal a basic core <span class="hlt">periodicity</span>. A Dicke type space oblateness experiment is discussed for providing better photospheric <span class="hlt">observations</span> than a ground instrument to determine the core <span class="hlt">periodicity</span>.</p> <div class="credits"> <p class="dwt_author">Knight, J. W.; Sturrock, P. A.; Schatten, K. H.</p> <p class="dwt_publisher"></p> <p class="publishDate">1980-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">273</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/6601206"> <span id="translatedtitle">Operation of a digital seismic network on Mount St. Helens volcano and <span class="hlt">observations</span> of long-<span class="hlt">period</span> seismic events that originate under the volcano</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">During the <span class="hlt">period</span> May through October 1981, a nine station digital seismic array was operated on the flanks of Mount St. Helens volcano in the state of Washington. The purpose was to obtain high quality digital seismic data from a dense seismic array operating near and in the summit crater of the volcano to facilitate study of near field seismic waveforms generated under the volcano. Our goal is to investigate the source mechanism of volcanic tremor and seismic activity associated with magma intrusion, dome growth and steam-ash emissions occurring within the crater of Mount St. Helens.</p> <div class="credits"> <p class="dwt_author">Fehler, M.; Chouet, B.</p> <p class="dwt_publisher"></p> <p class="publishDate">1982-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">274</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/759848"> <span id="translatedtitle">Long-<span class="hlt">Period</span> Solar Variability</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Terrestrial climate records and historical <span class="hlt">observations</span> of the Sun <span class="hlt">suggest</span> that the Sun undergoes aperiodic oscillations in radiative output and size over time <span class="hlt">periods</span> of centuries and millenia. Such behavior can be explained by the solar convective zone acting as a nonlinear oscillator, forced at the sunspot-cycle frequency by variations in heliomagnetic field strength. A forced variant of the Lorenz equations can generate a time series with the same characteristics as the solar and climate records. The timescales and magnitudes of oscillations that could be caused by this mechanism are consistent with what is known about the Sun and terrestrial climate.</p> <div class="credits"> <p class="dwt_author">GAUTHIER,JOHN H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2000-07-20</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">275</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/22774684"> <span id="translatedtitle">Building false memories without <span class="hlt">suggestions</span>.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">People can come to remember doing things they have never done. The question we asked in this study is whether people can systematically come to remember performing actions they never really did, in the absence of any <span class="hlt">suggestion</span> from the experimenter. People built LEGO vehicles, performing some steps but not others. For half the people, all the pieces needed to assemble each vehicle were laid out in order in front of them while they did the building; for the other half, the pieces were hidden from view. The next day, everyone returned for a surprise recognition test. People falsely and confidently remembered having carried out steps they did not; those who saw all the pieces while they built each vehicle were more likely to correctly remember performing steps they did perform but equally likely to falsely remember performing steps they did not. We explain our results using the source monitoring framework: People used the relationships between actions to internally generate the missing, related actions, later mistaking that information for genuine experience. PMID:22774684</p> <div class="credits"> <p class="dwt_author">Foster, Jeffrey L; Garry, Maryanne</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">276</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/1309.0100.pdf"> <span id="translatedtitle">Detecting multiple <span class="hlt">periodicities</span> in <span class="hlt">observational</span> data with the multi-frequency periodogram. II. Frequency Decomposer, a parallelized time-series analysis algorithm</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">This is a parallelized algorithm performing a decomposition of a noisy time series into a number of frequency components. The algorithm analyses all suspicious <span class="hlt">periodicities</span> that can be revealed, including the ones that look like an alias or noise at a glance, but later may prove to be a real variation. After selection of the initial candidates, the algorithm performs a complete pass through all their possible combinations and computes the rigorous multi-frequency statistical significance for each such frequency tuple. The largest combinations that still survived this thresholding procedure represent the outcome of the analysis. The parallel computing on a graphics processing unit (GPU) is implemented through CUDA and brings a significant performance increase. It is still possible to run FREDEC solely on CPU in the traditional single-threaded mode, when no suitable GPU device is available.</p> <div class="credits"> <p class="dwt_author">Baluev, Roman V</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">277</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013AtmEn..67..448C"> <span id="translatedtitle">Long-term <span class="hlt">observations</span> of saccharides in remote marine aerosols from the western North Pacific: A comparison between 1990-1993 and 2006-2009 <span class="hlt">periods</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Anhydrosugars (galactosan, mannosan and levoglucosan), sugars (xylose, fructose, glucose, sucrose and trehalose) and sugar alcohols (erythritol, arabitol, mannitol and inositol) were measured in the aerosol samples collected in a remote island (Chichi-Jima, Japan) in the western North Pacific from 1990 to 1993 and from 2006 to 2009. Total concentrations of anhydrosugars, the biomass burning tracers, were 0.01-5.57 ng m-3 (average 0.76 ng m-3) during 1990-1993 versus 0.01-7.19 ng m-3 (0.64 ng m-3) during 2006-2009. Their seasonal variations were characterized by winter/spring maxima and summer/fall minima. Such a seasonal pattern should be caused by the enhanced long-range atmospheric transport of biomass burning products and terrestrial organic matter (such as higher plant detritus and soil dust) from the Asian continent in winter/spring seasons, when the westerly or winter monsoon system prevails over the western North Pacific. Sugars and sugar alcohols showed different seasonal patterns. The monthly mean concentrations of erythritol, arabitol, mannitol, inositol, fructose, glucose and trehalose were found to be higher in spring/summer and lower in fall/winter during both 1990-1993 and 2006-2009 <span class="hlt">periods</span>, indicating an enhanced biogenic emission of aerosols in warm seasons. Interestingly, saccharides showed a gradual decrease in their concentrations from 1991 to 1993 and an increase from 2006 to 2009. In addition, the monthly averaged concentrations of sugars and sugar alcohols showed maxima in early summer during 1990-1993, which occurred about 1-2 months earlier than those during 2006-2009. Such a clear seasonal shift may be attributable to the changes in the strength of westerly and trade wind systems during two <span class="hlt">periods</span>.</p> <div class="credits"> <p class="dwt_author">Chen, Jing; Kawamura, Kimitaka; Liu, Cong-Qiang; Fu, Pingqing</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">278</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/5337865"> <span id="translatedtitle"><span class="hlt">Periods</span> found in heat measurements obtained by calorimetry</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">During a span of 640 days, a <span class="hlt">periodicity</span> of 1.5158 +- 0.0008 days was discovered in successive heater equilibria on Calorimeter No. 127. Measurements were taken at 12-h intervals, with occasional changes of exactly 3 or 6 h in the schedule of measurements. This schedule eliminated all other possible <span class="hlt">periods</span> except a <span class="hlt">period</span> of 0.150156 days. <span class="hlt">Periods</span> of 1.519125 and 1.511283 days were discovered in data on the excess length of day as obtained by the US Naval Observatory over a <span class="hlt">period</span> of 24 y. These two <span class="hlt">periods</span> could equally well represent <span class="hlt">periods</span> of 0.150189 and 0.150112 days, since measurements were obtained only once every 24 h. It is <span class="hlt">suggested</span> that <span class="hlt">periods</span> <span class="hlt">observed</span> in sensitive calorimeters and in length of day data may be related. 1 reference, 6 figures, 5 tables.</p> <div class="credits"> <p class="dwt_author">Jordan, K.C.</p> <p class="dwt_publisher"></p> <p class="publishDate">1984-02-28</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">279</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2006A%26A...455..255S"> <span id="translatedtitle">AD Mensae: a dwarf nova in the <span class="hlt">period</span> gap</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Aims.AD Men has been classified as a probable long-<span class="hlt">period</span> dwarf nova based on its long-term variability. Recent spectroscopic data instead <span class="hlt">suggested</span> a short-<span class="hlt">period</span> system. With the <span class="hlt">observations</span> presented here we aim to clarify its nature. Methods: .Time-resolved photometry and spectroscopy has been used to obtain information on the orbital <span class="hlt">period</span> of this system. Results: .The light curve shows the typical flickering and a clear hump-like <span class="hlt">periodic</span> modulation with an average amplitude of 0.3 mag and a <span class="hlt">period</span> of P=2.20(02) h. The radial velocity measurements of the H? emission line confirm this value as the orbital <span class="hlt">period</span>. Conclusions: .AD Men is thus located at the lower end of, but clearly inside, the gap of the <span class="hlt">period</span> distribution of cataclysmic variables, making it one of only 11 dwarf novae in this important <span class="hlt">period</span> range.</p> <div class="credits"> <p class="dwt_author">Schmidtobreick, L.; Tappert, C.</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-08-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">280</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://pubs.er.usgs.gov/publication/70047665"> <span id="translatedtitle">Annual water-level measurements in <span class="hlt">observation</span> wells, 1951-1955, and atlas of maps showing changes in water levels for various <span class="hlt">periods</span> from beginning of record through 1954, New Mexico</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p class="result-summary">This report tabulates the annual measurements of water level in the <span class="hlt">observation</span> wells in the various irrigated areas, primarily from 1951 through 1955. It summarizes changes in water level by discussion and with an atlas of nearly all the maps of change of water level for the <span class="hlt">period</span> of record to 1955 for each area in which <span class="hlt">observations</span> are being made. Included also are hydrographs for the <span class="hlt">period</span> of record through 1954 of several selected wells in the various areas irrigated from ground-water sources. The annual measurements of water level before 1951, seasonal measurements, and daily records of water levels in wells equipped with recording gages have been published in an annual series of U. S. Geological Survey water-supply papers.</p> <div class="credits"> <p class="dwt_author">Reeder, Harold O.</p> <p class="dwt_publisher"></p> <p class="publishDate">1959-01-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_13");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a 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src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">281</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/21448802"> <span id="translatedtitle">CONSTRAINTS ON LONG-<span class="hlt">PERIOD</span> PLANETS FROM AN L'- AND M-BAND SURVEY OF NEARBY SUN-LIKE STARS: <span class="hlt">OBSERVATIONS</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">We present the <span class="hlt">observational</span> results of an L'- and M-band adaptive optics imaging survey of 54 nearby, Sun-like stars for extrasolar planets, carried out using the Clio camera on the MMT. We have concentrated more strongly than all other planet-imaging surveys to date on very nearby F, G, and K stars, prioritizing stellar proximity higher than youth. Ours is also the first survey to include extensive <span class="hlt">observations</span> in the M band, which supplement the primary L' <span class="hlt">observations</span>. Models predict much better planet/star flux ratios at the L' and M bands than at more commonly used shorter wavelengths (i.e., the H band). We have carried out extensive blind simulations with fake planets inserted into the raw data to verify our sensitivity, and to establish a definitive relationship between source significance in {sigma} and survey completeness. We find 97% confident-detection completeness for 10{sigma} sources, but only 46% for 7{sigma} sources-raising concerns about the standard procedure of assuming high completeness at 5{sigma}, and demonstrating that blind sensitivity tests to establish the significance-completeness relation are an important analysis step for all planet-imaging surveys. We discovered a previously unknown {approx}0.15 M{sub sun} stellar companion to the F9 star GJ 3876, at a projected separation of about 80 AU. Twelve additional candidate faint companions are detected around other stars. Of these, 11 are confirmed to be background stars and one is a previously known brown dwarf. We obtained sensitivity to planetary-mass objects around almost all of our target stars, with sensitivity to objects below 3 M{sub Jup} in the best cases. Constraints on planet populations based on this null result are presented in our Modeling Results paper.</p> <div class="credits"> <p class="dwt_author">Heinze, A. N.; Hinz, Philip M.; Sivanandam, Suresh; Kenworthy, Matthew; Miller, Douglas [Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721 (United States); Meyer, Michael, E-mail: ariheinze@hotmail.co, E-mail: phinz@as.arizona.ed, E-mail: suresh@as.arizona.ed, E-mail: mkenworthy@as.arizona.ed, E-mail: dlmiller@as.arizona.ed, E-mail: mmeyer@phys.ethz.c [Department of Physics, Swiss Federal Institute of Technology (ETH-Zurich), ETH Honggerberg, CH-8093 Zurich (Switzerland)</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-05-10</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">282</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://repository.tamu.edu/handle/1969.1/ETD-TAMU-1963-THESIS-C889"> <span id="translatedtitle">An investigation of time changes in clouds <span class="hlt">observed</span> over the Gulf of Mexico and Caribbean Sea during the <span class="hlt">period</span> 18 - 23 July 1961</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">nsula BR H DURAS CamPBChe ara Cruz Y Peni Grand Caym4 '~a~ Swan 15(and CgXMMAI thnaslan HONDURAS + NICARAGUA Ipp 90 Bp Fig. 2. Geographical locator chart. 1. Surface <span class="hlt">observers</span> usually can see and thus report a hemispheric dome only... Figure Model of an easterly wave (after Riehlp 1954) Page 2. Geographical locator chart 14 Time cross-section at Swan Island from 0000 GCT, 16 July 1961 to 1200 GCT, 24 July 1961. Isopleths of relative humidity are shown...</p> <div class="credits"> <p class="dwt_author">Cramer, William Paul</p> <p class="dwt_publisher"></p> <p class="publishDate">1963-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">283</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25631747"> <span id="translatedtitle"><span class="hlt">Observations</span> on changes in abundance of questing Ixodes ricinus, castor bean tick, over a 35-year <span class="hlt">period</span> in the eastern part of its range (Russia, Tula region).</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Ixodes ricinus (Acari: Ixodidae) L. transmit a wide variety of pathogens to vertebrates including viruses, bacteria and protozoa. Understanding of the epidemiology of tick-borne infections requires basic knowledge of the regional and local factors influencing tick population dynamics. The present study describes the results of monitoring of a questing I. ricinus population, conducted over 35?years (1977-2011) in the eastern, poorly studied part of its range (Russia, Tula region). We have found that the multiannual average abundance of ticks is small and varies depending on the biotope and degree of urban transformation. Tick abundance for the first 14?years of <span class="hlt">observations</span> (1977-1990) was at the lower limit of the sensitivity of our methods throughout the study area (0.1-0.9 specimens per 1-km transect). In the following 21?years (1991-2011), a manifold increase in abundance was <span class="hlt">observed</span>, which reached 18.1?±?1.8 individuals per 1-km transect in moist floodplain terraces, and 4.8?±?0.9 in xerophylic hill woods. Long-term growth of tick abundance occurred in spite of a relatively constant abundance of small mammals and only minor fluctuations in the abundance of large wild animals. Climate and anthropogenic changes appear to be the main contributors to increased abundance of the tick. PMID:25631747</p> <div class="credits"> <p class="dwt_author">Korotkov, Yu; Kozlova, T; Kozlovskaya, L</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">284</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/21563073"> <span id="translatedtitle">Revisiting the Brazilian scenario of registry and protection of cultivars: an analysis of the <span class="hlt">period</span> from 1998 to 2010, its dynamics and legal <span class="hlt">observations</span>.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">During the last 20 years, the national production of grains has increased 156.1%; productivity increased 93.8% and there has been an increase of 29.1% in cultivated area. Currently, agribusiness is responsible for 40% of Brazilian exports. Nevertheless, there is little quantitative information on the main plant species of economic interest that have been registered and protected in the Agriculture, Fisheries and Food Supply Ministry (MAPA) by public and private companies, as well as by public-private partnerships. Consequently, we investigated the registry and protection of 27 species of economic interest, including the 15 that are the basis of the Brazilian diet, based on the information available on the site CultivarWeb, of MAPA, for the <span class="hlt">period</span> from 1998 to August 30, 2010. We also examined the legislation that regulates registration and protection procedures and its implications for plant breeding and plant product development. It was found that the private sector controls 73.1% of the registrations and 53.56% of the protections, while 10.73% of the protections were of material developed overseas. Public-private partnerships contributed little to the development of new cultivars, with 0.5% of the registries and 3.61% of the protections. We conclude that plant protection directed private investment to development of wheat and rice varieties, with the greatest public investments directed to corn and sorghum. After the Cultivar Protection Law was implemented, there was restriction of access to germplasm banks, which could inhibit advances in Brazilian plant breeding programs, indicating a need for revision of this legal barrier. PMID:21563073</p> <div class="credits"> <p class="dwt_author">Marinho, C D; Martins, F J O; Amaral, S C S; Amaral Júnior, A T; Gonçalves, L S A; de Mello, M P</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">285</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.rsc.org/chemsoc/visualelements/pages/pertable_fla.htm"> <span id="translatedtitle"><span class="hlt">Periodic</span> Table</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">This unique <span class="hlt">periodic</span> table presents the elements in an interesting visual display. Select an element, and find an image of the element, a description, history, and even an animation. Other chemical data is linked as a PDF file (requires Acrobat Reader).</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">286</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/22707043"> <span id="translatedtitle">A <span class="hlt">suggested</span> new bacteriophage genus: "Viunalikevirus".</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">We <span class="hlt">suggest</span> a bacteriophage genus, "Viunalikevirus", as a new genus within the family Myoviridae. To date, this genus includes seven sequenced members: Salmonella phages ViI, SFP10 and ?SH19; Escherichia phages CBA120 and PhaxI; Shigella phage phiSboM-AG3; and Dickeya phage LIMEstone1. Their shared myovirus morphology, with comparable head sizes and tail dimensions, and genome organization are considered distinguishing features. They appear to have conserved regulatory sequences, a horizontally acquired tRNA set and the probable substitution of an alternate base for thymine in the DNA. A close examination of the tail spike region in the DNA revealed four distinct tail spike proteins, an arrangement which might lead to the umbrella-like structures of the tails visible on electron micrographs. These properties set the <span class="hlt">suggested</span> genus apart from the recently ratified subfamily Tevenvirinae, although a significant evolutionary relationship can be <span class="hlt">observed</span>. PMID:22707043</p> <div class="credits"> <p class="dwt_author">Adriaenssens, Evelien M; Ackermann, Hans-Wolfgang; Anany, Hany; Blasdel, Bob; Connerton, Ian F; Goulding, David; Griffiths, Mansel W; Hooton, Steven P; Kutter, Elizabeth M; Kropinski, Andrew M; Lee, Ju-Hoon; Maes, Martine; Pickard, Derek; Ryu, Sangryeol; Sepehrizadeh, Zargham; Shahrbabak, S Sabouri; Toribio, Ana L; Lavigne, Rob</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-10-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">287</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.springerlink.com/index/x205v150h3412042.pdf"> <span id="translatedtitle"><span class="hlt">Periodicity</span> of DNA in exons</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">BACKGROUND: The <span class="hlt">periodic</span> pattern of DNA in exons is a known phenomenon. It was <span class="hlt">suggested</span> that one of the initial causes of <span class="hlt">periodicity</span> could be the universal (RNY)npattern (R = A or G, Y = C or U, N = any base) of ancient RNA. Two major questions were addressed in this paper. Firstly, the cause of DNA <span class="hlt">periodicity</span>, which</p> <div class="credits"> <p class="dwt_author">Stephen T Eskesen; Frank N Eskesen; Brian Kinghorn; Anatoly Ruvinsky</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">288</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19890012014&hterms=animal+extinction&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Danimal%2Bextinction"> <span id="translatedtitle"><span class="hlt">Periodicity</span> of extinction: A 1988 update</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The hypothesis that events of mass extinction recur <span class="hlt">periodically</span> at approximately 26 my intervals is an empirical claim based on analysis of data from the fossil record. The hypothesis has become closely linked with catastrophism because several events in the <span class="hlt">periodic</span> series are associated with evidence of extraterrestrial impacts, and terrestrial forcing mechanisms with long, <span class="hlt">periodic</span> recurrences are not easily conceived. Astronomical mechanisms that have been hypothesized include undetected solar companions and solar oscillation about the galactic plane, which induce comet showers and result in impacts on Earth at regular intervals. Because these mechanisms are speculative, they have been the subject of considerable controversy, as has the hypothesis of <span class="hlt">periodicity</span> of extinction. In response to criticisms and uncertainties, a data base was developed on times of extinction of marine animal genera. A time series is given and analyzed with 49 sample points for the per-genus extinction rate from the Late Permian to the Recent. An unexpected pattern in the data is the uniformity of magnitude of many of the <span class="hlt">periodic</span> extinction events. <span class="hlt">Observations</span> <span class="hlt">suggest</span> that the sequence of extinction events might be the result of two sets of mechanisms: a <span class="hlt">periodic</span> forcing that normally induces only moderate amounts of extinction, and independent incidents or catastrophes that, when coincident with the <span class="hlt">periodic</span> forcing, amplify its signal and produce major-mass extinctions.</p> <div class="credits"> <p class="dwt_author">Sepkowski, J. John, Jr.</p> <p class="dwt_publisher"></p> <p class="publishDate">1988-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">289</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://sprg.ssl.berkeley.edu/adminstuff/webpubs/1999_modulatedpc1.pdf"> <span id="translatedtitle">A MODULATED MULTIBAND Pc1 EVENT <span class="hlt">OBSERVED</span> BY POLAR/EFI AROUND THE PLASMAPAUSE</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">in amplitude, corresponding to classical Pc1 pearls. The repetition <span class="hlt">period</span> was the same on ground and in space. Moreover, the repetition <span class="hlt">period</span> of Pc1 pearls coincided with the <span class="hlt">period</span> of simultaneous Pc4 waves <span class="hlt">observed</span> by POLAR and on ground. The <span class="hlt">observations</span> <span class="hlt">suggest</span> that Pc1 pearls (EMIC waves in general) are modulated</p> <div class="credits"> <p class="dwt_author">California at Berkeley, University of</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">290</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19900037240&hterms=comet+strikes&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dcomet%2Bstrikes"> <span id="translatedtitle">Are <span class="hlt">periodic</span> bombardments real?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Consideration is given to the hypothesis that showers of comets or asteroids strike the earth every 26 m yrs, causing climatic castastrophes and mass extinctions (Raup and Sepkoski, 1984). Possible explanations for the alleged <span class="hlt">periodicity</span> are discussed, including the possibility that the sun has a small faint companion star and perturbations of the Oort cloud as the solar system passes through the Galactic plane. Also, the possible causes of the extinction at the K-T boundary are examined. The implications of these theories are noted and evidence <span class="hlt">suggesting</span> that impacts do not have <span class="hlt">periodicity</span> is presented.</p> <div class="credits"> <p class="dwt_author">Weissman, Paul R.</p> <p class="dwt_publisher"></p> <p class="publishDate">1990-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">291</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013GeoRL..40.2602C"> <span id="translatedtitle">California foreshock sequences <span class="hlt">suggest</span> aseismic triggering process</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Foreshocks are one of the few well-documented precursors to large earthquakes; therefore, understanding their nature is very important for earthquake prediction and hazard mitigation. However, the triggering role of foreshocks is not yet clear. It is possible that foreshocks are a self-triggering cascade of events that simply happen to trigger an unusually large aftershock; alternatively, foreshocks might originate from an external aseismic process that ultimately triggers the mainshock. In the former case, the foreshocks will have limited utility for forecasting. The latter case has been <span class="hlt">observed</span> for several individual large earthquakes; however, it remains unclear how common it is and how to distinguish foreshock sequences from other seismicity clusters that do not lead to large earthquakes. Here we analyze foreshocks of three M>7 mainshocks in southern California. These foreshock sequences appear similar to earthquake swarms, in that they do not start with their largest events and they exhibit spatial migration of seismicity. Analysis of source spectra shows that all three foreshock sequences feature lower average stress drops and depletion of high-frequency energy compared with the aftershocks of their corresponding mainshocks. Using a longer-term stress-drop catalog, we find that the average stress drop of the Landers and Hector Mine foreshock sequences is comparable to nearby swarms. Our <span class="hlt">observations</span> <span class="hlt">suggest</span> that these foreshock sequences are manifestations of aseismic transients occurring close to the mainshock hypocenters, possibly related to localized fault zone complexity, which have promoted the occurrence of both the foreshocks and the eventual mainshock.</p> <div class="credits"> <p class="dwt_author">Chen, Xiaowei; Shearer, Peter M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-06-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">292</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/38782500"> <span id="translatedtitle">Reinventing <span class="hlt">suggestion</span> systems for continuous improvement</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">This article reports an experiment to increase the effectiveness of a <span class="hlt">suggestion</span> system by deliberately applying principles of the kaizen and performance management. Design rules for <span class="hlt">suggestion</span> systems are derived from these theories. The <span class="hlt">suggestion</span> system that resulted differs from traditional <span class="hlt">suggestion</span> systems in a number of aspects. For example, in the new system, line managers have a role in</p> <div class="credits"> <p class="dwt_author">Roel W. Schuring; Harald Luijten</p> <p class="dwt_publisher"></p> <p class="publishDate">2001-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">293</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2006MAP....92..255R"> <span id="translatedtitle">Unstationary aspects of foehn in a large valley part I: operational setup, scientific objectives and analysis of the cases during the special <span class="hlt">observing</span> <span class="hlt">period</span> of the MAP subprogramme FORM</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The Rhine valley, which stretches from the main Alpine crest to the Lake of Constance, was chosen as the target area to study unstationary aspects of foehn during the Special <span class="hlt">Observing</span> <span class="hlt">Period</span> (SOP) of the Mesoscale Alpine Programme (MAP). This large valley is up to 10 km wide and has some of the highest foehn frequencies in the European Alps. The MAP subprogram FORM ( FOehn in the Rhine valley during MAP) was designed to investigate various aspects of the foehn including the interaction of foehn flow with the boundary layer and the processes that remove the cold air pool. The subprogram was also focused on improving the understanding and forecasting of foehn-related phenomena such as waves and turbulence. A large number of in-situ and remote sensing <span class="hlt">observing</span> systems were deployed to take measurements during the field phase of MAP. Among them were about 50 surface stations, up to 9 radiosonde stations, 2 wind profilers, 4 Doppler sodars, 2 scintillometers, 1 scanning and 1 backscatter lidar and different research aircraft. This paper gives an overview of the objectives of FORM, describes the target area and its instrumentation, and provides a detailed synoptic description of the 12 foehn cases <span class="hlt">observed</span> during the MAP SOP.</p> <div class="credits"> <p class="dwt_author">Richner, H.; Baumann-Stanzer, K.; Benech, B.; Berger, H.; Chimani, B.; Dorninger, M.; Drobinski, P.; Furger, M.; Gubser, S.; Gutermann, T.; Häberli, C.; Häller, E.; Lothon, M.; Mitev, V.; Ruffieux, D.; Seiz, G.; Steinacker, R.; Tschannett, S.; Vogt, S.; Werner, R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">294</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.nlm.nih.gov/medlineplus/news/fullstory_150619.html"> <span id="translatedtitle">Soda Habit May Prompt Early Puberty in Girls, Study <span class="hlt">Suggests</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://medlineplus.gov/">MedlinePLUS</a></p> <p class="result-summary">... in Girls, Study <span class="hlt">Suggests</span> Early menstruation a risk factor for depression and breast cancer, researchers say (*this news item will not be ... researchers noted. "Starting <span class="hlt">periods</span> early is a risk factor for ... breast cancer during adulthood. Thus, our findings have implications beyond ...</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">295</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://files.eric.ed.gov/fulltext/ED044989.pdf"> <span id="translatedtitle"><span class="hlt">Suggestions</span> for the Classical Shelves of a School Library.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">This bibliography is <span class="hlt">suggested</span> for use by students and teachers of Latin, Greek and ancient civilizations. Entries are compiled under the headings of: (1) bibliographies and journals including booklists, <span class="hlt">periodicals</span>, and books for teachers; (2) reference works in literature, mythology, history and antiquities, and language; (3) texts and…</p> <div class="credits"> <p class="dwt_author">Colebourn, R., Comp.; Cleeve, Marigold, Comp.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">296</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=locates+AND+additional+AND+articles&id=EJ401067"> <span id="translatedtitle">Animal Rights: Selected Resources and <span class="hlt">Suggestions</span> for Further Study.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Presents an annotated list of selected resources intended to serve as a guide to the growing amount of material on animal rights. <span class="hlt">Suggestions</span> to aid in additional research include subject headings used to find books, indexes used to locate <span class="hlt">periodical</span> articles, sources for locating organizations, and a selected list of animal rights organizations.…</p> <div class="credits"> <p class="dwt_author">Davidoff, Donald J.</p> <p class="dwt_publisher"></p> <p class="publishDate">1989-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">297</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015PhRvA..91a3631E"> <span id="translatedtitle">Excited-state quantum phase transitions and <span class="hlt">periodic</span> dynamics</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We investigate signatures of the excited-state quantum phase transition in the <span class="hlt">periodic</span> dynamics of the Lipkin-Meshkov-Glick model and the Tavis-Cummings model. In the thermodynamic limit, expectation values of <span class="hlt">observables</span> in eigenstates of the system can be calculated using classical trajectories. Motivated by this, we <span class="hlt">suggest</span> a method based on the time evolution of the finite-size system to find singularities in <span class="hlt">observables</span>, which arise due to the excited-state quantum phase transition.</p> <div class="credits"> <p class="dwt_author">Engelhardt, G.; Bastidas, V. M.; Kopylov, W.; Brandes, T.</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">298</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19820017198&hterms=plasma+research&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3D%2522plasma%2Bresearch%2522"> <span id="translatedtitle">Structure of the solar oscillation with <span class="hlt">period</span> near 160 minutes</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The solar oscillation with <span class="hlt">period</span> near 160 minutes is found to be unique in a spectrum computed over the range of <span class="hlt">periods</span> from about 71 to 278 minutes. A best estimate of the <span class="hlt">period</span> is 160.0095 + or - 0.001 minutes, which is different from 160 minutes (one ninth of a day) by a highly significant amount. The width of the peak is approximately equal to the limiting resolution that can be obtained from an <span class="hlt">observation</span> lasting 6 years, which <span class="hlt">suggests</span> that the damping time of the oscillations is considerably longer than 6 years. A <span class="hlt">suggestion</span> that this peak might be the result of a beating phenomenon between the five minute data averages and a solar oscillation with <span class="hlt">period</span> near five minutes is shown to be incorrect by recomputing a portion of the spectrum using 15 second data averages.</p> <div class="credits"> <p class="dwt_author">Scherrer, P. H.; Wilcox, J. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">1982-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">299</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=efffects&id=EJ321936"> <span id="translatedtitle">The Effects of <span class="hlt">Suggestibility</span> on Relaxation.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Selected undergraduates (N=32) on the basis of Creative Imagination Scale scores and randomly assigned high and low <span class="hlt">suggestibility</span> subjects to progressive relaxation (PR) and <span class="hlt">suggestions</span> of relaxation (SR) training modes. Results revealed a significant pre-post relaxation effect, and main efffects for both <span class="hlt">suggestibility</span> and training mode. (NRB)</p> <div class="credits"> <p class="dwt_author">Rickard, Henry C.; And Others</p> <p class="dwt_publisher"></p> <p class="publishDate">1985-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">300</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/astro-ph/0506757v1"> <span id="translatedtitle">Origin of long-<span class="hlt">period</span> Alfv{é}n waves in the solar wind</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We <span class="hlt">suggest</span> that the <span class="hlt">observed</span> long-<span class="hlt">period</span> Alfv{\\'e}n waves in the solar wind may be generated in the solar interior due to the pulsation of the Sun in the fundamental radial mode. The <span class="hlt">period</span> of this pulsation is about 1 hour. The pulsation causes a <span class="hlt">periodical</span> variation of density and large-scale magnetic field, this affecting the Alfv{\\'e}n speed in the solar interior. Consequently the Alfv{\\'e}n waves with the half frequency of pulsation (i.e. with the double <span class="hlt">period</span>) can be parametrically amplified in the interior below the convection zone due to the recently <span class="hlt">suggested</span> swing wave-wave interaction. Therefore the amplified Alfv{\\'e}n waves have <span class="hlt">periods</span> of several hours. The waves can propagate upwards through the convection zone to the solar atmosphere and cause the <span class="hlt">observed</span> long-<span class="hlt">period</span> Alfv{\\'e}n oscillations in the solar wind.</p> <div class="credits"> <p class="dwt_author">T. V. Zaqarashvili; G. Belvedere</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-06-30</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_14");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' 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onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">301</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19910038066&hterms=stellar+evolution&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3D%2528stellar%2Bevolution%2529"> <span id="translatedtitle">Stellar evolution and <span class="hlt">period</span> changes in RR Lyrae stars</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The <span class="hlt">observed</span> secular <span class="hlt">period</span> changes of RR Lyrae stars in five globular clusters have been compared with those predicted by synthetic models of the horizontal branch (HB). It is shown that most of the <span class="hlt">observed</span> number distributions of the <span class="hlt">period</span> change rate beta could be attributed to evolutionary effects, if the random <span class="hlt">observational</span> error is of order + or - 0.07 days/Myr in beta as <span class="hlt">suggested</span> by the <span class="hlt">observers</span>. The model calculations indicate that the mean rate of <span class="hlt">period</span> change in RR Lyrae stars in globular clusters depends sensitively on their HB type, as is the case for the <span class="hlt">period</span> shift at a given effective temperature. The distinct bias toward positive <span class="hlt">period</span> changes in M15 and Omega Cen is evidence that most HB stars in the Oosterhoff group II clusters pass through the instability strip from blue to red toward the end of their core helium burning phase. If confirmed by future <span class="hlt">observations</span>, this is strong support for the Lee et al. (1990) explanation of the Sandage (1957) <span class="hlt">period</span>-shift effect.</p> <div class="credits"> <p class="dwt_author">Lee, Young-Wook</p> <p class="dwt_publisher"></p> <p class="publishDate">1991-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">302</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19990028161&hterms=periodic&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D70%26Ntt%3Dperiodic"> <span id="translatedtitle">Quasi-<span class="hlt">periodic</span> compressive waves in polar plumes</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The <span class="hlt">observation</span> of polar plumes in the south polar coronal hole, carried out on 7 March 1996 by the Solar and Heliospheric Observatory (SOHO), are analyzed. These polar plumes are cool density structures that arise from morphologically unipolar magnetic footpoints. Data from the extreme ultraviolet imaging telescope show quasi-<span class="hlt">periodic</span> perturbations in the brightness of the Fe IX and X line emissions at 171 A from polar plumes. The perturbations have <span class="hlt">periods</span> of 10 to 15 min, and repeat for several cycles <span class="hlt">suggesting</span> that they are compressive waves propagating through the plume at or near the Alfven speed. Possible explanations for the <span class="hlt">observed</span> phenomenon are proposed.</p> <div class="credits"> <p class="dwt_author">DeForest, C. E.; Gurman, J. B.</p> <p class="dwt_publisher"></p> <p class="publishDate">1997-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">303</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/1583995"> <span id="translatedtitle">Detecting a hidden <span class="hlt">periodic</span> signal when its <span class="hlt">period</span> is unknown</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">A simple method is presented for detecting an unknown <span class="hlt">periodic</span> signal in additive noise. The <span class="hlt">period</span> is unknown, but the amplitudes of the fundamental and the first M - 1 harmonics are known to be nonzero. One application is the detection of a torpedo by a submarine sonar system from the <span class="hlt">observed</span> acoustic line spectrum generated by the torpedo's blade</p> <div class="credits"> <p class="dwt_author">M. Hinich</p> <p class="dwt_publisher"></p> <p class="publishDate">1982-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">304</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/21144772"> <span id="translatedtitle">The influence of <span class="hlt">suggestibility</span> on memory.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">We provide a translation of Binet and Henri's pioneering 1894 paper on the influence of <span class="hlt">suggestibility</span> on memory. Alfred Binet (1857-1911) is famous as the author who created the IQ test that bears his name, but he is almost unknown as the psychological investigator who generated numerous original experiments and fascinating results in the study of memory. His experiments published in 1894 manipulated <span class="hlt">suggestibility</span> in several ways to determine effects on remembering. Three particular modes of <span class="hlt">suggestion</span> were employed to induce false recognitions: (1) indirect <span class="hlt">suggestion</span> by a preconceived idea; (2) direct <span class="hlt">suggestion</span>; and (3) collective <span class="hlt">suggestion</span>. In the commentary we <span class="hlt">suggest</span> that Binet and Henri's (1894) paper written over 115 years ago is still highly relevant even today. In particular, Binet's legacy lives on in modern research on misinformation effects in memory, in studies of conformity, and in experiments on the social contagion of memory. PMID:21144772</p> <div class="credits"> <p class="dwt_author">Nicolas, Serge; Collins, Thérèse; Gounden, Yannick; Roediger, Henry L</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">305</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/20645418"> <span id="translatedtitle">Host-mediated induction of alpha-amylases by larvae of the Mexican bean weevil Zabrotes subfasciatus (Coleoptera: Chrysomelidae: Bruchinae) is irreversible and <span class="hlt">observed</span> from the initiation of the feeding <span class="hlt">period</span>.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Larvae of Zabrotes subfasciatus secrete alpha-amylases that are insensitive to the alpha-amylase inhibitor found in seeds of Phaseolus vulgaris. By analyzing amylase activities during larval development on P. vulgaris, we detected activity of the constitutive amylase and the two inducible amylase isoforms at all stages. When larvae were transferred from the non alpha-amylase inhibitor containing seeds of Vigna unguiculata to P. vulgaris, the inducible alpha-amylases were expressed at the same level as in control larvae fed on P. vulgaris. Interestingly, when larvae were transferred from seeds of P. vulgaris to those of V. unguiculata, inducible alpha-amylases continued to be expressed at a level similar to that found in control larvae fed P. vulgaris continuously. When 10-day-old larvae were removed from seeds of V. unguiculata and transferred into capsules containing flour of P. vulgaris cotyledons, and thus maintained until completing 17 days (age when the larvae stopped feeding), we could detect higher activity of the inducible alpha-amylases. However, when larvae of the same age were transferred from P. vulgaris into capsules containing flour of V. unguiculata, the inducible alpha-amylases remained up-regulated. These results <span class="hlt">suggest</span> that the larvae of Z. subfasciatus have the ability to induce insensitive amylases early in their development. A short <span class="hlt">period</span> of feeding on P. vulgaris cotyledon flour was sufficient to irreversibly induce the inducible alpha-amylase isoforms. Incubations of brush border membrane vesicles with the alpha-amylase inhibitor 1 from P. vulgaris <span class="hlt">suggest</span> that the inhibitor is recognized by putative receptors found in the midgut microvillar membranes. PMID:20645418</p> <div class="credits"> <p class="dwt_author">Bifano, Thaís D; Samuels, Richard I; Alexandre, Daniel; Silva, Carlos P</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-08-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">306</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012IAUS..282..123S"> <span id="translatedtitle">The Orbital <span class="hlt">Period</span> Distribution of Cataclysmic Variables Found by the SDSS</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The orbital <span class="hlt">period</span> is one of the most accessible <span class="hlt">observables</span> of a cataclysmic variable. It has been a concern for many years that the orbital <span class="hlt">period</span> distribution of the known systems does not match that predicted by evolutionary theory. The sample of objects discovered by the Sloan Digital Sky Survey has changed this: it shows the long-expected predominance of short-<span class="hlt">period</span> objects termed the `<span class="hlt">period</span> spike'. The minimum <span class="hlt">period</span> remains in conflict with theory, <span class="hlt">suggesting</span> that the angular momentum loss mechanisms are stronger than predicted.</p> <div class="credits"> <p class="dwt_author">Southworth, John; Gänsicke, Boris T.; Breedt, Elmé</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">307</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25365130"> <span id="translatedtitle">Hypnotizability, not <span class="hlt">suggestion</span>, influences false memory development.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Hypnotizability influences the development of false memories. In Experiment 1, participants heard a positive or negative <span class="hlt">suggestion</span> regarding hypnosis and then listened to 8 Deese-Roediger-McDermott (DRM) false memory paradigm lists in a hypnotic state. Neither hypnosis nor prehypnotic <span class="hlt">suggestion</span> affected memory. Highly hypnotizable participants were more accurate in recall and recognition. In Experiment 2, <span class="hlt">suggestions</span> were delivered in the form of feedback. Participants heard a positive or negative <span class="hlt">suggestion</span> about their performance prior to either the encoding or retrieval of 8 DRM lists. Neither accurate nor false memories were affected by the <span class="hlt">suggestion</span>. Highly hypnotizable individuals recognized fewer critical lures if they received a negative <span class="hlt">suggestion</span> about their performance. These results highlight the unusual role of hypnotizability in the creation of false memories. PMID:25365130</p> <div class="credits"> <p class="dwt_author">Dasse, Michelle N; Elkins, Gary R; Weaver, Charles A</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">308</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://serc.carleton.edu/sp/mnstep/activities/26404.html"> <span id="translatedtitle">Group and <span class="hlt">periodic</span> properties lab</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">Students will <span class="hlt">observe</span> and perform experiments with the elements sodium, potassium, calcium, magnesium, sulfur and phosphorus. Conclusions will be made about trends down groups, across <span class="hlt">periods</span> and relating to acidity/basicity of metal oxides vs. nonmetal oxides</p> <div class="credits"> <p class="dwt_author">Dan Shaffer</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">309</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://pubs.er.usgs.gov/publication/pp175018"> <span id="translatedtitle">Radar interferometry <span class="hlt">observations</span> of surface displacements during pre- and coeruptive <span class="hlt">periods</span> at Mount St. Helens, Washington, 1992-2005: Chapter 18 in A volcano rekindled: the renewed eruption of Mount St. Helens, 2004-2006</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p class="result-summary">We analyzed hundreds of interferograms of Mount St. Helens produced from radar images acquired by the ERS-1/2, ENVISAT, and RADARSAT satellites during the 1992-2004 preeruptive and 2004-2005 coeruptive <span class="hlt">periods</span> for signs of deformation associated with magmatic activity at depth. Individual interferograms were often contaminated by atmospheric delay anomalies; therefore, we employed stacking to amplify any deformation patterns that might exist while minimizing random noise. Preeruptive interferograms show no signs of volcanowide deformation between 1992 and the onset of eruptive activity in 2004. Several patches of subsidence in the 1980 debris-avalanche deposit were identified, however, and are thought to be caused by viscoelastic relaxation of loosely consolidated substrate, consolidation of water-saturated sediment, or melting of buried ice. Coeruptive interferometric stacks are dominated by atmospheric noise, probably because individual interferograms span only short time intervals in 2004 and 2005. Nevertheless, we are confident that at least one of the seven coeruptive stacks we constructed is reliable at about the 1-cm level. This stack <span class="hlt">suggests</span> deflation of Mount St. Helens driven by contraction of a source beneath the volcano.</p> <div class="credits"> <p class="dwt_author">Poland, Michael; Lu, Zhong</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">310</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014A%26A...563L...4N"> <span id="translatedtitle">Convection, granulation, and <span class="hlt">period</span> jitter in classical Cepheids</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Analyses of recent <span class="hlt">observations</span> of the sole classical Cepheid in the Kepler field, V1154 Cygni, found random changes of about 30 min in the pulsation <span class="hlt">period</span>. These <span class="hlt">period</span> changes challenge standard theories of pulsation and evolution because the <span class="hlt">period</span> change is non-secular, and explaining this <span class="hlt">period</span> jitter is necessary for understanding stellar evolution and the role of Cepheids as precise standard candles. We <span class="hlt">suggest</span> that convection and convective hot spots can explain the <span class="hlt">observed</span> <span class="hlt">period</span> jitter. Convective hot spots alter the timing of flux maximum and minimum in the Cepheid light curve, hence change the measured pulsation <span class="hlt">period</span>. We present a model of random hot spots that generate a localized flux excess that perturbs the Cepheid light curve and consequently the pulsation <span class="hlt">period</span>, which is consistent with the <span class="hlt">observed</span> jitter. This result demonstrates how important understanding convection is for modeling Cepheid stellar structure and evolution, how convection determines the red edge of the instability strip, and just how sensitive Cepheid light curves are to atmospheric physics.</p> <div class="credits"> <p class="dwt_author">Neilson, Hilding R.; Ignace, Richard</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-03-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">311</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ftp.ecgs.lu/pdf/jlg91/JLG91_JYGuo_FA.pdf"> <span id="translatedtitle">The folding-averaging algorithm applied to precisely determine <span class="hlt">periodical</span> signals from time series with application to the detection of free oscillations using super-conducting gravimeter <span class="hlt">observation</span> data</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The folding-averaging algorithm is applied to precisely determining <span class="hlt">periodical</span> signals which may be present in a time series. The basic principle is to rebuild for every test <span class="hlt">period</span> a new short time series by cutting the the original times series to shorter ones of which the length is equal to the test <span class="hlt">period</span>, and then stacking the short time series</p> <div class="credits"> <p class="dwt_author">J. Y. Guo; H. Greiner-Mai; L. Ballani; J. Neumeyer; O. Dierks; C. K. Shum</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">312</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3622029"> <span id="translatedtitle"><span class="hlt">Periodic</span> bursts of Jovian non-Io decametric radio emission</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">During the years 2000–2011 the radio instruments onboard Cassini, Wind and STEREO spacecraft have recorded a large amount of the Jovian decametric radio emission (DAM). In this paper we report on the analysis of the new type of Jovian <span class="hlt">periodic</span> radio bursts recently revealed in the decametric frequency range. These bursts, which are non-Io component of DAM, are characterized by a strong <span class="hlt">periodic</span> reoccurrence over several Jovian days with a <span class="hlt">period</span> ?1.5% longer than the rotation rate of the planet's magnetosphere (System III). The bursts are typically <span class="hlt">observed</span> between 4 and 12 MHz and their occurrence probability has been found to be significantly higher in the sector of Jovian Central Meridian Longitude between 300° and 60° (via 360°). The stereoscopic multispacecraft <span class="hlt">observations</span> have shown that the radio sources of the <span class="hlt">periodic</span> bursts radiate in a non-axisymmetric hollow cone-like pattern and sub-corotate with Jupiter remaining active during several planet's rotations. The occurrence of the <span class="hlt">periodic</span> non-Io DAM bursts is strongly correlated with pulses of the solar wind ram pressure at Jupiter. Moreover the <span class="hlt">periodic</span> bursts exhibit a tendency to occur in groups every ?25 days. The polarization measurements have shown that the <span class="hlt">periodic</span> bursts are right hand polarized radio emission associated with the Northern magnetic hemisphere of Jupiter. We <span class="hlt">suggest</span> that <span class="hlt">periodic</span> non-Io DAM bursts may be connected with the interchange instability in Io plasma torus triggered by the solar wind. PMID:23585696</p> <div class="credits"> <p class="dwt_author">Panchenko, M.; Rucker, H.O.; Farrell, W.M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">313</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23585696"> <span id="translatedtitle"><span class="hlt">Periodic</span> bursts of Jovian non-Io decametric radio emission.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">During the years 2000-2011 the radio instruments onboard Cassini, Wind and STEREO spacecraft have recorded a large amount of the Jovian decametric radio emission (DAM). In this paper we report on the analysis of the new type of Jovian <span class="hlt">periodic</span> radio bursts recently revealed in the decametric frequency range. These bursts, which are non-Io component of DAM, are characterized by a strong <span class="hlt">periodic</span> reoccurrence over several Jovian days with a <span class="hlt">period</span> [Formula: see text] longer than the rotation rate of the planet's magnetosphere (System III). The bursts are typically <span class="hlt">observed</span> between 4 and 12 MHz and their occurrence probability has been found to be significantly higher in the sector of Jovian Central Meridian Longitude between 300° and 60° (via 360°). The stereoscopic multispacecraft <span class="hlt">observations</span> have shown that the radio sources of the <span class="hlt">periodic</span> bursts radiate in a non-axisymmetric hollow cone-like pattern and sub-corotate with Jupiter remaining active during several planet's rotations. The occurrence of the <span class="hlt">periodic</span> non-Io DAM bursts is strongly correlated with pulses of the solar wind ram pressure at Jupiter. Moreover the <span class="hlt">periodic</span> bursts exhibit a tendency to occur in groups every [Formula: see text] days. The polarization measurements have shown that the <span class="hlt">periodic</span> bursts are right hand polarized radio emission associated with the Northern magnetic hemisphere of Jupiter. We <span class="hlt">suggest</span> that <span class="hlt">periodic</span> non-Io DAM bursts may be connected with the interchange instability in Io plasma torus triggered by the solar wind. PMID:23585696</p> <div class="credits"> <p class="dwt_author">Panchenko, M; Rucker, H O; Farrell, W M</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">314</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20140010436&hterms=south+barrow&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3Dsouth%2Bbarrow"> <span id="translatedtitle"><span class="hlt">Periodic</span> Bursts of Jovian Non-Io Decametric Radio Emission</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">During the years 2000-2011 the radio instruments onboard Cassini, Wind and STEREO spacecraft have Recorded a large amount of the Jovian decametric radio emission (DAM). In this paper we report on the analysis of the new type of Jovian <span class="hlt">periodic</span> radio bursts recently revealed in the decametric frequency range. These bursts, which are non-Io component of DAM, are characterized by a strong <span class="hlt">periodic</span> reoccurrence over several Jovian days with a <span class="hlt">period</span> approx. = 1:5% longer than the rotation rate of the planet's magnetosphere (System III). The bursts are typically <span class="hlt">observed</span> between 4 and 12 MHz and their occurrence probability has been found to be significantly higher in the sector of Jovian Central Meridian Longitude between 300 deg. and 60 deg. (via 360 deg.). The stereoscopic multispacecraft <span class="hlt">observations</span> have shown that the radio sources of the <span class="hlt">periodic</span> bursts radiate in a non-axisymmetric hollow cone-like pattern and sub-corotate with Jupiter remaining active during several planet's rotations. The occurrence of the <span class="hlt">periodic</span> non-Io DAM bursts is strongly correlated with pulses of the solar wind ram pressure at Jupiter. Moreover the <span class="hlt">periodic</span> bursts exhibit a tendency to occur in groups every approx. 25 days. The polarization measurements have shown that the <span class="hlt">periodic</span> bursts are right hand polarized radio emission associated with the Northern magnetic hemisphere of Jupiter. We <span class="hlt">suggest</span> that <span class="hlt">periodic</span> non-Io DAM bursts may be connected with the interchange instability in Io plasma torus triggered by the solar wind.</p> <div class="credits"> <p class="dwt_author">Panchenko, M.; Rucker, H O.; Farrell, W. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">315</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=20090001918&hterms=relationships+statistics&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3D%2528relationships%2Bstatistics%2529"> <span id="translatedtitle">On the <span class="hlt">Period</span>-Amplitude and Amplitude-<span class="hlt">Period</span> Relationships</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Examined are <span class="hlt">Period</span>-Amplitude and Amplitude-<span class="hlt">Period</span> relationships based on the cyclic behavior of the 12-month moving averages of monthly mean sunspot numbers for cycles 0.23, both in terms of Fisher's exact tests for 2x2 contingency tables and linear regression analyses. Concerning the <span class="hlt">Period</span>-Amplitude relationship (same cycle), because cycle 23's maximum amplitude is known to be 120.8, the inferred regressions (90-percent prediction intervals) <span class="hlt">suggest</span> that its <span class="hlt">period</span> will be 131 +/- 24 months (using all cycles) or 131 +/- 18 months (ignoring cycles 2 and 4, which have the extremes of <span class="hlt">period</span>, 108 and 164 months, respectively). Because cycle 23 has already persisted for 142 months (May 1996 through February 2008), based on the latter prediction, it should end before September 2008. Concerning the Amplitude-<span class="hlt">Period</span> relationship (following cycle maximum amplitude versus preceding cycle <span class="hlt">period</span>), because cycle 23's <span class="hlt">period</span> is known to be at least 142 months, the inferred regressions (90-percent prediction intervals) <span class="hlt">suggest</span> that cycle 24's maximum amplitude will be about less than or equal to 96.1 +/- 55.0 (using all cycle pairs) or less than or equal to 91.0 +/- 36.7 (ignoring statistical outlier cycle pairs). Hence, cycle 24's maximum amplitude is expected to be less than 151, perhaps even less than 128, unless cycle pair 23/24 proves to be a statistical outlier.</p> <div class="credits"> <p class="dwt_author">Wilson, Robert M.; Hathaway, David H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">316</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=3794044"> <span id="translatedtitle">Placebo-<span class="hlt">Suggestion</span> Modulates Conflict Resolution in the Stroop Task</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Here, we ask whether placebo-<span class="hlt">suggestion</span> (without any form of hypnotic induction) can modulate the resolution of cognitive conflict. Naïve participants performed a Stroop Task while wearing an EEG cap described as a “brain wave” machine. In Experiment 1, participants were made to believe that the EEG cap would either enhance or decrease their color perception and performance on the Stroop task. In Experiment 2, participants were explicitly asked to imagine that their color perception and performance would be enhanced or decreased (non-hypnotic imaginative <span class="hlt">suggestion</span>). We <span class="hlt">observed</span> effects of placebo-<span class="hlt">suggestion</span> on Stroop interference on accuracy: interference was decreased with positive <span class="hlt">suggestion</span> and increased with negative <span class="hlt">suggestion</span> compared to baseline. Intra-individual variability was also increased under negative <span class="hlt">suggestion</span> compared to baseline. Compliance with the instruction to imagine a modulation of performance, on the other hand, did not influence accuracy and only had a negative impact on response latencies and on intra-individual variability, especially in the congruent condition of the Stroop Task. Taken together, these results demonstrate that expectations induced by a placebo-<span class="hlt">suggestion</span> can modulate our ability to resolve cognitive conflict, either facilitating or impairing response accuracy depending on the <span class="hlt">suggestion’s</span> contents. Our results also demonstrate a dissociation between placebo-<span class="hlt">suggestion</span> and non-hypnotic imaginative <span class="hlt">suggestion</span>. PMID:24130735</p> <div class="credits"> <p class="dwt_author">Caspar, Emilie A.; Gevers, Wim; Cleeremans, Axel</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">317</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/12088333"> <span id="translatedtitle">The "big five" and hypnotic <span class="hlt">suggestibility</span>.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">A recent approach to personality measurement argues that the essential personality traits are encompassed by 5 basic factors: openness/intellect, conscientiousness, neuroticism, agreeableness, and extraversion. This study used the Big Five Inventory to test the hypothesis that 1 or more of the 5 factors underlie hypnotic <span class="hlt">suggestibility</span>. No meaningful relationships between hypnotic <span class="hlt">suggestibility</span> and any of the 5 factors were found. PMID:12088333</p> <div class="credits"> <p class="dwt_author">Nordenstrom, Benita K; Council, James R; Meier, Brian P</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">318</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/2820534"> <span id="translatedtitle">Cerebral Mechanisms of Hypnotic Induction and <span class="hlt">Suggestion</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The neural mechanisms underlying hypnotic states and responses to hypnotic <span class="hlt">suggestions</span> remain largely unknown and, to date, have been studied only with indirect methods. Here, the effects of hypnosis and <span class="hlt">suggestions</span> to alter pain perception were investigated in hypnotizable subjects by using positron emission tomography (PET) measures of regional cerebral blood flow (rCBF) and electroencephalographic (EEG) measures of brain electrical</p> <div class="credits"> <p class="dwt_author">Pierre Rainville; Robert K. Hofbauer; TomᚠPaus; Gary H. Duncan; M. Catherine Bushnell; Donald D. Price</p> <p class="dwt_publisher"></p> <p class="publishDate">1999-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">319</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.chem.cmu.edu/groups/yaron/pdf/twosuggestions-jce.pdf"> <span id="translatedtitle">Two <span class="hlt">Suggestions</span> for Improving Chemical Equilibrium Instruction</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">Two <span class="hlt">Suggestions</span> for Improving Chemical Equilibrium Instruction Journal: Journal of Chemical to the Journal of Chemical Education #12;ed-20XX-XXXXXX Two <span class="hlt">Suggestions</span> for Improving Chemical Equilibrium Chemical Equilibrium Instruction David Yaron*1, Jodi L. Davenport2, James Greeno3, Michael Karabinos1</p> <div class="credits"> <p class="dwt_author">Yaron, David</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">320</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25660206"> <span id="translatedtitle">Improving sleep and cognition by hypnotic <span class="hlt">suggestion</span> in the elderly.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Sleep quality markedly declines across the human lifespan. Particularly the amount of slow-wave sleep (SWS) decreases with age and this decrease is paralleled by a loss of cognitive functioning in the elderly. Here we show in healthy elderly females that the amount of SWS can be extended by a hypnotic <span class="hlt">suggestion</span> "to sleep deeper" before sleep. In a placebo-controlled cross-over design, participants listened to hypnotic <span class="hlt">suggestions</span> or a control tape before a midday nap while high density electroencephalography was recorded. After the hypnotic <span class="hlt">suggestion</span>, we <span class="hlt">observed</span> a 57% increase in SWS in females <span class="hlt">suggestible</span> to hypnosis as compared to the control condition. Furthermore, left frontal slow-wave activity (SWA), characteristic for SWS, was significantly increased, followed by a significant improvement in prefrontal cognitive functioning after sleep. Our results <span class="hlt">suggest</span> that hypnotic <span class="hlt">suggestions</span> might be a successful alternative for widely-used sleep-enhancing medication to extend SWS and improve cognition in the elderly. PMID:25660206</p> <div class="credits"> <p class="dwt_author">Cordi, Maren Jasmin; Hirsiger, Sarah; Mérillat, Susan; Rasch, Björn</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-03-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_15");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return 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class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_16");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' href="#">3</a> <a onClick='return showDiv("page_4");' href="#">4</a> <a onClick='return showDiv("page_5");' href="#">5</a> <a onClick='return showDiv("page_6");' href="#">6</a> <a onClick='return showDiv("page_7");' href="#">7</a> <a onClick='return showDiv("page_8");' href="#">8</a> <a onClick='return 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title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">321</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/24130735"> <span id="translatedtitle">Placebo-<span class="hlt">suggestion</span> modulates conflict resolution in the Stroop Task.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Here, we ask whether placebo-<span class="hlt">suggestion</span> (without any form of hypnotic induction) can modulate the resolution of cognitive conflict. Naïve participants performed a Stroop Task while wearing an EEG cap described as a "brain wave" machine. In Experiment 1, participants were made to believe that the EEG cap would either enhance or decrease their color perception and performance on the Stroop task. In Experiment 2, participants were explicitly asked to imagine that their color perception and performance would be enhanced or decreased (non-hypnotic imaginative <span class="hlt">suggestion</span>). We <span class="hlt">observed</span> effects of placebo-<span class="hlt">suggestion</span> on Stroop interference on accuracy: interference was decreased with positive <span class="hlt">suggestion</span> and increased with negative <span class="hlt">suggestion</span> compared to baseline. Intra-individual variability was also increased under negative <span class="hlt">suggestion</span> compared to baseline. Compliance with the instruction to imagine a modulation of performance, on the other hand, did not influence accuracy and only had a negative impact on response latencies and on intra-individual variability, especially in the congruent condition of the Stroop Task. Taken together, these results demonstrate that expectations induced by a placebo-<span class="hlt">suggestion</span> can modulate our ability to resolve cognitive conflict, either facilitating or impairing response accuracy depending on the <span class="hlt">suggestion</span>'s contents. Our results also demonstrate a dissociation between placebo-<span class="hlt">suggestion</span> and non-hypnotic imaginative <span class="hlt">suggestion</span>. PMID:24130735</p> <div class="credits"> <p class="dwt_author">Magalhães De Saldanha da Gama, Pedro A; Slama, Hichem; Caspar, Emilie A; Gevers, Wim; Cleeremans, Axel</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">322</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.nlm.nih.gov/medlineplus/news/fullstory_151231.html"> <span id="translatedtitle">Nuts May Lengthen Your Life, Study <span class="hlt">Suggests</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://medlineplus.gov/">MedlinePLUS</a></p> <p class="result-summary">... MONDAY, March 2, 2015 (HealthDay) -- Eating nuts, including peanuts and peanut butter, may help you live longer, a new ... nutrition and health research <span class="hlt">suggests</span> that nut and peanut consumption can be considered a healthy lifestyle choice," ...</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">323</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/21452814"> <span id="translatedtitle">AN INTERPRETATION OF THE ORBITAL <span class="hlt">PERIOD</span> DIFFERENCE BETWEEN HOT JUPITERS AND GIANT PLANETS ON LONG-<span class="hlt">PERIOD</span> ORBITS</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">It is believed that a hot Jupiter (giant planet with a short <span class="hlt">period</span> less than 10 days) forms in the outer region of a protoplanetary disk, then migrates inward to an orbit with a short <span class="hlt">period</span> around 3 days, and stops there by a final stopping mechanism. The prominent problem is why hot Jupiters migrate inward to short-<span class="hlt">period</span> orbits, while other extrasolar giant planets and Jovian planets in our solar system exist on long-<span class="hlt">period</span> orbits. Here we show that this difference in orbital <span class="hlt">periods</span> is caused by two populations of protoplanetary disks. One population experiences gravitational instability during some <span class="hlt">periods</span> of their lifetime (GI disks), while the other does not (No-GI disks). In GI disks, planets can quickly migrate inward to short-<span class="hlt">period</span> orbits to become hot Jupiters. In No-GI disks, the migration is so slow that planets can exist on long-<span class="hlt">period</span> orbits. Protoplanetary disks are classified into the two populations because of the differences in properties of molecular cloud cores, from which disks from. We specifically compare our theory with <span class="hlt">observations</span>. Our theory is supported by <span class="hlt">observations</span> of extrasolar planets. We analyze the current status of our solar system and find that our solar nebula belongs to the population with a low migration rate. This is consistent with the <span class="hlt">observation</span> that Jupiter and Saturn are indeed on long-<span class="hlt">period</span> orbits. Our results further <span class="hlt">suggest</span> that, in the future <span class="hlt">observations</span>, a hot Jupiter cannot be found around a star with mass below a critical mass (0.14-0.28 M {sub sun}).</p> <div class="credits"> <p class="dwt_author">Jin Liping, E-mail: jinlp@jlu.edu.c [College of Physics, Jilin University, Changchun, Jilin 130021 (China)</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-09-10</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">324</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25246673"> <span id="translatedtitle">Hydrodynamics of <span class="hlt">periodic</span> breathers.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">We report the first experimental <span class="hlt">observation</span> of <span class="hlt">periodic</span> breathers in water waves. One of them is Kuznetsov-Ma soliton and another one is Akhmediev breather. Each of them is a localized solution of the nonlinear Schrödinger equation (NLS) on a constant background. The difference is in localization which is either in time or in space. The experiments conducted in a water wave flume show results that are in good agreement with the NLS theory. Basic features of the breathers that include the maximal amplitudes and spectra are consistent with the theoretical predictions. PMID:25246673</p> <div class="credits"> <p class="dwt_author">Chabchoub, A; Kibler, B; Dudley, J M; Akhmediev, N</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-10-28</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">325</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2012MPBu...39..148P"> <span id="translatedtitle">Rotation <span class="hlt">Period</span> Determination for 5143 Heracles</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The Earth crossing minor planet 5143 Heracles made in late 2011 its closest approach to Earth since discovery. A consortium of <span class="hlt">observers</span> found a synodic rotation <span class="hlt">period</span> near 2.706 hours and amplitude increasing from 0.08 ±0.02 magnitudes at phase angle 20 degrees to 0.18 ±0.03 magnitudes at phase angle 87 degrees, with 3 unequal maxima and minima per cycle. Magnitude parameters H = 14.10 ±0.04 and G = 0.08 ±0.02 are found, and the color index V-R = 0.42 ±0.07. For an asteroid of taxonomic class Q, a <span class="hlt">suggested</span> albedo pv = 0.20 ±0.05 yields estimated diameter D = 4.5 ±0.7 km. Three possible binary events were recorded, but these are insufficient for binary detection to be secure. Retrograde rotation is <span class="hlt">suggested</span>.</p> <div class="credits"> <p class="dwt_author">Pilcher, Frederick; Briggs, John W.; Franco, Lorenzo; Inasaridze, Raguli Ya.; Krugly, Yurij N.; Molotiv, Igor E.; Klinglesmith, Daniel A., III; Pollock, Joe; Pravec, Petr</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-07-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">326</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25472881"> <span id="translatedtitle">Anxiety disorders and physical comorbidity: increased prevalence but reduced relevance of specific risk factors for hospital-based mortality during a 12.5-year <span class="hlt">observation</span> <span class="hlt">period</span> in general hospital admissions.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Anxiety disorders (AD) are associated with an increase in physical comorbidities, but the effects of these diseases on hospital-based mortality are unclear. Consequently, we investigated whether the burden of physical comorbidity and its relevance on hospital-based mortality differed between individuals with and without AD during a 12.5-year <span class="hlt">observation</span> <span class="hlt">period</span> in general hospital admissions. During 1 January 2000 and 30 June 2012, 11,481 AD individuals were admitted to seven General Manchester Hospitals. All comorbidities with a prevalence ?1 % were compared with those of 114,810 randomly selected and group-matched hospital controls of the same age and gender, regardless of priority of diagnoses or specialized treatments. Comorbidities that increased the risk of hospital-based mortality (but not mortality outside of the hospital) were identified using multivariate logistic regression analyses. AD individuals compared to controls had a substantial excess comorbidity, but a reduced hospital-based mortality rate. Twenty-two physical comorbidities were increased in AD individuals compared with controls, which included cardiovascular diseases and their risk factors. The most frequent physical comorbidities in AD individuals were hypertension, asthma, cataract, and ischaemic heart disease. Risk factors for hospital-based mortality in AD individuals were lung cancer, alcoholic liver disease, respiratory failure, heart failure, pneumonia, bronchitis, non-specific dementia, breast cancer, COPD, gallbladder calculus, atrial fibrillation, and angina. The impact of atrial fibrillation, angina, and gallbladder calculus on hospital-based mortality was higher in AD individuals than in controls. In contrast, other mortality risk factors had an equal or lower impact on hospital-based mortality in sample comparisons. Therefore AD individuals have a higher burden of physical comorbidity that is associated with a reduced risk of general hospital-based mortality. Atrial fibrillation, angina, and gallbladder calculus are major risk factors for general hospital-based mortality in AD individuals. PMID:25472881</p> <div class="credits"> <p class="dwt_author">Schoepf, Dieter; Heun, Reinhard</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">327</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://repository.tamu.edu/handle/1969.1/87194"> <span id="translatedtitle"><span class="hlt">Suggestions</span> for Weed Control in Corn</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary"><span class="hlt">Suggestions</span> for Weed Control in Corn 2-02 E E-525 <span class="hlt">Suggestions</span> for W eed Contr ol in Cor n P aul A. B aumann, P h.D. P r ofessor and E xtension W eed S pecialist T exas Cooperativ e E xtension The T exas A&M U niv ersity S y stem T able P age... T able P age 1 W inter w eed contr ol ............................................................................5 4 P ostemergence and post-dir ect ed herbicides ..................................14 2 P r eplant herbicides for postemergence contr ol...</p> <div class="credits"> <p class="dwt_author">Baumann, Paul A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-02-19</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">328</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/52861597"> <span id="translatedtitle">Is the <span class="hlt">periodicity</span> in the distribution of quasar redshifts evidence for the universe being multiply-connected?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary"><span class="hlt">Observational</span> evidence is cited as proof that the universe is compactified, i.e., a topologically flat space. It is <span class="hlt">suggested</span> that quasars are 'ghost' images that can appear in a universe with positive curvature (a sphere). A <span class="hlt">periodicity</span> has been statistically detected for the redshifts of quasars, which may indicate the existence of a large-scale <span class="hlt">periodic</span> perturbation in the mass distribution</p> <div class="credits"> <p class="dwt_author">L.-Z. Fang; H. Sato</p> <p class="dwt_publisher"></p> <p class="publishDate">1983-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">329</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=black+AND+holes&id=EJ879604"> <span id="translatedtitle">Technology Is Power: <span class="hlt">Suggestions</span> for Beginning Teachers</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Shanklin knows it can be hard for new teachers to incorporate all they know about technology with the realities of a classroom. She <span class="hlt">suggests</span> setting incremental, monthly technology goals; investing in equipment; assessing students' grasp of the technology at their disposal and their use of it in classroom projects; searching purposefully for…</p> <div class="credits"> <p class="dwt_author">Shanklin, Nancy</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">330</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=black+AND+holes&pg=5&id=EJ068448"> <span id="translatedtitle">Physics Courses--Some <span class="hlt">Suggested</span> Case Studies</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">To communicate the relevance and excitement of science activity to students, the use of more imaginative, and even openly speculative, case studies in physics courses is <span class="hlt">suggested</span>. Some useful examples are Magnetic Monopoles, Constants, Black Holes, Antimatter, Zero Mass Particles, Tachyons, and the Bootstrap Hypothesis. (DF)</p> <div class="credits"> <p class="dwt_author">Swetman, T. P.</p> <p class="dwt_publisher"></p> <p class="publishDate">1972-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">331</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=%22Research+Article%22&id=EJ1040522"> <span id="translatedtitle"><span class="hlt">Suggestions</span> for Structuring a Research Article</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Researchers often experience difficulty as they attempt to prepare journal articles that describe their work. The purpose of this article is to provide researchers in the field of education with a series of <span class="hlt">suggestions</span> as to how to clearly structure each section of a research manuscript that they intend to submit for publication in a scholarly…</p> <div class="credits"> <p class="dwt_author">Klein, James D.; Reiser, Robert A.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">332</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://cogsci.indiana.edu/pub/nichols.rhythm.pdf"> <span id="translatedtitle">LYRIC-BASED RHYTHM <span class="hlt">SUGGESTION</span> Eric Nichols</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">and Cognition ABSTRACT Which comes first--the lyrics or the music? Here we consider the lyrics-first approach with lyrics it can serve as compositional advice. Books on songwriting and music composition often <span class="hlt">suggest</span> rule applicable to music with lyrics. The Linguistic Stress Rule states: "Prefer to align strong beats</p> <div class="credits"> <p class="dwt_author">Indiana University</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">333</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/13302541"> <span id="translatedtitle">Social group <span class="hlt">suggestion</span> from user image collections</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Photo-sharing services have attracted millions of people and helped construct massive social networks on the Web. A popular trend is that users share their image collections within social groups, which greatly promotes the interactions between users and expands their social networks. Existing systems have difficulties in generating satisfactory social group <span class="hlt">suggestions</span> because the images are classified independently and their relationship</p> <div class="credits"> <p class="dwt_author">Jie Yu; Xin Jin; Jiawei Han; Jiebo Luo</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">334</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/43547652"> <span id="translatedtitle">Training in community policing : A <span class="hlt">suggested</span> curriculum</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The widespread acceptance of community policing necessitates the need for training of recruits into its philosophy and practices. We provide a <span class="hlt">suggested</span> curriculum for such training after describing its three basic premises. This is followed by discussions of the rationale for the curriculum, and a promising training method that can be used in its implementation. All of the above are</p> <div class="credits"> <p class="dwt_author">Michael J. Palmiotto; Michael L. Birzer; N. Prabha Unnithan</p> <p class="dwt_publisher"></p> <p class="publishDate">2000-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">335</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/37029524"> <span id="translatedtitle">On the mechanism of <span class="hlt">suggestion</span> and hypnosis</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The nature of hypnosis is not adequately explained by conditioned responses or conditioned attitudes. The writer agrees with R. W. White that the hypnotized subject must be motivated, but not necessarily to behave like a hypnotized person. She postulates, rather, that <span class="hlt">suggestions</span> are effective only if the subject actively strives to imagine himself in the situation described by the operator.</p> <div class="credits"> <p class="dwt_author">M. B. Arnold</p> <p class="dwt_publisher"></p> <p class="publishDate">1946-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">336</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.cse.ohio-state.edu/~lai/2331/greedy.pdf"> <span id="translatedtitle">Minimum Spanning Trees <span class="hlt">Suggested</span> Reading: Chapter 23.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">Minimum Spanning Trees CSE 680 <span class="hlt">Suggested</span> Reading: Chapter 23. 1 Greedy Method Optimization Problem best at this moment 1 #12;2 Minimum Spanning Trees · Spanning tree: A spanning tree of a connected = (V, E), find a span- ning tree of minimum cost. · Assume V = {1, 2, . . . , n}. 2 #12;3 Prim</p> <div class="credits"> <p class="dwt_author">Lai, Ten-Hwang "Steve"</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">337</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.cse.ohio-state.edu/~lai/2331/6.greedy.pdf"> <span id="translatedtitle">Minimum Spanning Trees <span class="hlt">Suggested</span> Reading: Chapter 23.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">Minimum Spanning Trees CSE 2331 <span class="hlt">Suggested</span> Reading: Chapter 23. 1 Greedy Method Optimization Problem best at this moment 1 #12;2 Minimum Spanning Trees · Spanning tree: A spanning tree of a connected = (V, E), find a span- ning tree of minimum cost. · Assume V = {1, 2, . . . , n}. 2 #12;3 Prim</p> <div class="credits"> <p class="dwt_author">Lai, Ten-Hwang "Steve"</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">338</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.uaf.edu/files/summer/JRN-F049-F01-Field-Photography-Gear-List.pdf"> <span id="translatedtitle"><span class="hlt">Suggested</span> Gear List Tent (could be shared)</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary"><span class="hlt">Suggested</span> Gear List Tent (could be shared) Sleeping bag Sleeping pad Pillow Clothing: Bring layers. Hiking shoes Sun hat Wool/fleece cap Wool/fleece gloves Jacket (fleece jacket could fit under rain gear) Heavy rain gear, including pants Rubber boots/hip waders Neoprene gloves Sandals Toiletries: small towel</p> <div class="credits"> <p class="dwt_author">Sikes, Derek S.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">339</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/57485260"> <span id="translatedtitle">Does Neuroimaging of <span class="hlt">Suggestion</span> Elucidate Hypnotic Trance?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Contemporary studies in the cognitive neuroscience of attention and <span class="hlt">suggestion</span> shed new light on the underlying neural mechanisms that operationalize these effects. Without adhering to important caveats inherent to imaging of the living human brain, however, findings from brain imaging studies may enthrall more than explain. Scholars, practitioners, professionals, and consumers must realize that the influence words exert on focal</p> <div class="credits"> <p class="dwt_author">Amir Raz</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">340</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=corporate+AND+law&pg=5&id=EJ178875"> <span id="translatedtitle">Accounting: <span class="hlt">Suggested</span> Content for Postsecondary Tax Course</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Surveys of community college graduates and of certified public accountants were made to determine employment relevance of the accounting curriculum. The article <span class="hlt">suggests</span> topics from the study data which should be included in taxation courses, e.g., income tax accounting, corporate taxation accounting, and tax law. (MF)</p> <div class="credits"> <p class="dwt_author">King, Patricia H.; Morgan, Samuel D.</p> <p class="dwt_publisher"></p> <p class="publishDate">1978-01-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_16");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a 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src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">341</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://files.eric.ed.gov/fulltext/ED313168.pdf"> <span id="translatedtitle">Family Living: <span class="hlt">Suggestions</span> for Effective Parenting.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary"><span class="hlt">Suggestions</span> for effective parenting of preschool children are provided in 33 brief articles on children's feelings concerning self-esteem; fear; adopted children; the birth of a sibling; death; depression; and coping with stress, trauma, and divorce. Children's behavior is discussed in articles on toddlers' eating habits, punishment and…</p> <div class="credits"> <p class="dwt_author">Katz, Lilian G.; And Others</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">342</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=science+AND+research+AND+topic&pg=3&id=EJ1018315"> <span id="translatedtitle">Current Research: 2013 Summer Reading <span class="hlt">Suggestions</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">To supplement the summer reading of National Science Teachers Association (NSTA) members, the NSTA Committee on Research in Science Education <span class="hlt">suggested</span> a list of science education research articles that were published in the journals of NSTA's affiliates in 2012. These articles covered a variety of topics that include learning about…</p> <div class="credits"> <p class="dwt_author">Journal of College Science Teaching, 2013</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">343</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25054188"> <span id="translatedtitle">Enhancing business intelligence by means of <span class="hlt">suggestive</span> reviews.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Appropriate identification and classification of online reviews to satisfy the needs of current and potential users pose a critical challenge for the business environment. This paper focuses on a specific kind of reviews: the <span class="hlt">suggestive</span> type. <span class="hlt">Suggestions</span> have a significant influence on both consumers' choices and designers' understanding and, hence, they are key for tasks such as brand positioning and social media marketing. The proposed approach consists of three main steps: (1) classify comparative and <span class="hlt">suggestive</span> sentences; (2) categorize <span class="hlt">suggestive</span> sentences into different types, either explicit or implicit locutions; (3) perform sentiment analysis on the classified reviews. A range of supervised machine learning approaches and feature sets are evaluated to tackle the problem of <span class="hlt">suggestive</span> opinion mining. Experimental results for all three tasks are obtained on a dataset of mobile phone reviews and demonstrate that extending a bag-of-words representation with <span class="hlt">suggestive</span> and comparative patterns is ideal for distinguishing <span class="hlt">suggestive</span> sentences. In particular, it is <span class="hlt">observed</span> that classifying <span class="hlt">suggestive</span> sentences into implicit and explicit locutions works best when using a mixed sequential rule feature representation. Sentiment analysis achieves maximum performance when employing additional preprocessing in the form of negation handling and target masking, combined with sentiment lexicons. PMID:25054188</p> <div class="credits"> <p class="dwt_author">Qazi, Atika; Raj, Ram Gopal; Tahir, Muhammad; Cambria, Erik; Syed, Karim Bux Shah</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">344</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.pubmedcentral.nih.gov/articlerender.fcgi?tool=pmcentrez&artid=4099162"> <span id="translatedtitle">Enhancing Business Intelligence by Means of <span class="hlt">Suggestive</span> Reviews</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pmc">PubMed Central</a></p> <p class="result-summary">Appropriate identification and classification of online reviews to satisfy the needs of current and potential users pose a critical challenge for the business environment. This paper focuses on a specific kind of reviews: the <span class="hlt">suggestive</span> type. <span class="hlt">Suggestions</span> have a significant influence on both consumers' choices and designers' understanding and, hence, they are key for tasks such as brand positioning and social media marketing. The proposed approach consists of three main steps: (1) classify comparative and <span class="hlt">suggestive</span> sentences; (2) categorize <span class="hlt">suggestive</span> sentences into different types, either explicit or implicit locutions; (3) perform sentiment analysis on the classified reviews. A range of supervised machine learning approaches and feature sets are evaluated to tackle the problem of <span class="hlt">suggestive</span> opinion mining. Experimental results for all three tasks are obtained on a dataset of mobile phone reviews and demonstrate that extending a bag-of-words representation with <span class="hlt">suggestive</span> and comparative patterns is ideal for distinguishing <span class="hlt">suggestive</span> sentences. In particular, it is <span class="hlt">observed</span> that classifying <span class="hlt">suggestive</span> sentences into implicit and explicit locutions works best when using a mixed sequential rule feature representation. Sentiment analysis achieves maximum performance when employing additional preprocessing in the form of negation handling and target masking, combined with sentiment lexicons. PMID:25054188</p> <div class="credits"> <p class="dwt_author">Qazi, Atika</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">345</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/6769616"> <span id="translatedtitle"><span class="hlt">Periodic</span> Comet Machholz and its idiosyncrasies</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The dynamics and physical characteristics of Comet P/Machholz are analyzed. The discovery of the comet (Machholz, 1986) is discussed, including the <span class="hlt">observational</span> conditions and the theory that the comet is inactive over extensive <span class="hlt">periods</span> of time. Consideration is given to <span class="hlt">observations</span> of the two tails of Comet P/Machholz (Emerson, 1986), the brightness variations and light curve of the comet, and nuclear photometry of the comet (Green, 1987). It is <span class="hlt">suggested</span> that the increase in activity beginning one day after perihelion was triggered by a discrete source within 15 deg of the rotation pole that became sunlit after perihelion. Also, the possibility that Comet P/Machholz is associated with a meteor stream is examined. 45 refs.</p> <div class="credits"> <p class="dwt_author">Sekanina, Z. (JPL, Pasadena, CA (USA))</p> <p class="dwt_publisher"></p> <p class="publishDate">1990-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">346</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/20736607"> <span id="translatedtitle"><span class="hlt">Periodically</span> oscillating plasma sphere</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The <span class="hlt">periodically</span> oscillating plasma sphere, or POPS, is a novel fusion concept first proposed by D. C. Barnes and R. A. Nebel [Fusion Technol. 38, 28 (1998)]. POPS utilizes the self-similar collapse of an oscillating ion cloud in a spherical harmonic oscillator potential well formed by electron injection. Once the ions have been phase-locked, their coherent motion simultaneously produces very high densities and temperatures during the collapse phase of the oscillation. A requirement for POPS is that the electron injection produces a stable harmonic oscillator potential. This has been demonstrated in a gridded inertial electrostatic confinement device and verified by particle simulation. Also, the POPS oscillation has been confirmed experimentally through <span class="hlt">observation</span> that the ions in the potential well exhibit resonance behavior when driven at the POPS frequency. Excellent agreement between the <span class="hlt">observed</span> POPS frequencies and the theoretical predictions has been <span class="hlt">observed</span> for a wide range of potential well depths and three different ion species. Practical applications of POPS require large plasma compressions. These large compressions have been <span class="hlt">observed</span> in particle simulations, although space charge neutralization remains a major issue.</p> <div class="credits"> <p class="dwt_author">Park, J.; Nebel, R.A.; Stange, S.; Murali, S. Krupakar [Los Alamos National Laboratory, Los Alamos, New Mexico 87544 (United States); University of Wisconsin, Madison, Wisconsin 53706 (United States)</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-05-15</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">347</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://pubs.er.usgs.gov/publication/70036652"> <span id="translatedtitle"><span class="hlt">Suggested</span> notation conventions for rotational seismology</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p class="result-summary">We note substantial inconsistency among authors discussing rotational motions <span class="hlt">observed</span> with inertial seismic sensors (and much more so in the broader topic of rotational phenomena). Working from physics and other precedents, we propose standard terminology and a preferred reference frame for inertial sensors (Fig. 1) that may be consistently used in discussions of both finite and infinitesimal <span class="hlt">observed</span> rotational and translational motions in seismology and earthquake engineering. The scope of this article is limited to <span class="hlt">observations</span> because there are significant differences in the analysis of finite and infinitesimal rotations, though such discussions should remain compatible with those presented here where possible. We recommend the general use of the notation conventions presented in this tutorial, and we recommend that any deviations or alternatives be explicitly defined.</p> <div class="credits"> <p class="dwt_author">Evans, J.R.</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">348</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23093907"> <span id="translatedtitle">Mentoring in biostatistics: some <span class="hlt">suggestions</span> for reform.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Mentoring is routinely used as a tool to facilitate acquisition of skills by new professionals in fields like medicine, nursing, surgery, and business. While mentoring has been proposed as an effective strategy for knowledge and skills transfer in biostatistics and related fields, there is still much to be done to facilitate adoption by stakeholders, including academia and employers of biostatisticians. This is especially troubling given that biostatisticians play a key role in the success or otherwise of clinical research conducted for evidence-based decisions. In this paper, we offer <span class="hlt">suggestions</span> on how mentoring can be applied in practice to advance the statistical training of future biostatisticians. In particular, we propose steps that academic statistics departments, professional statistical societies, and statistics organizations can take to advance the mentoring of young biostatisticians. Our <span class="hlt">suggestions</span> also cover what mentors and mentees can do to facilitate a successful mentoring relationship. PMID:23093907</p> <div class="credits"> <p class="dwt_author">Odueyungbo, Adefowope; Thabane, Lehana</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">349</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://repository.tamu.edu/handle/1969.1/87684"> <span id="translatedtitle"><span class="hlt">Suggestions</span> For Weed Control In Cotton</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">Acetyl CoA carboxylase inhibitor 2 lb/gal Syngenta Goal ? 2 XL oxyfluoren Protox inhibitor 1.6 lb/gal Dow AgroSciences Gramoxone ? Max paraquat Photosystem I electron diverter 3.0 lb/gal Syngenta Harmony Extra ? thifensulfuron-methyl Acetolactate... by David Nace, page 20 photograph by Scott Bauer, both of the U.S. Department of Agriculture <span class="hlt">Suggestions</span> for in Cotton Tables 1. Winter Weed Control Treatments ...............................................6 2. Preplant...</p> <div class="credits"> <p class="dwt_author">Baumann, Paul A.; Lemon, Robert G.</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-07-03</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">350</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://math.ucsb.edu/ugrad/pdf/UpdatedSuggestedPlanofStudyBSMath.pdf"> <span id="translatedtitle"><span class="hlt">Suggested</span> Plan of Study BS Mathematics</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">: Math 118A Math 118B 118C or elective UD elective 147A or elective *Computer Science 8 or 16<span class="hlt">Suggested</span> Plan of Study BS Mathematics 10/21/14 Fall Winter Spring Summer? Frosh year: Math 3A Math 3B Math 4A CMPSC* Physics 1, 6A or 21 Soph. year: Math 4B Math 6A Math 6B Math 8** Math 108A*** Math</p> <div class="credits"> <p class="dwt_author">Akhmedov, Azer</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">351</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://math.ucsb.edu/ugrad/pdf/UpdatedSuggestedPlanofStudyMTHSC.pdf"> <span id="translatedtitle"><span class="hlt">Suggested</span> Plan of Study BS Mathematical Sciences</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">elective Sr. year: Math 118A Math 118B 118C or UD elective UD elective 122A *Computer Science 8 or 16<span class="hlt">Suggested</span> Plan of Study BS Mathematical Sciences 10/21/14 Fall Winter Spring Summer? Frosh year: Math 3A Math 3B Math 4A CMPSC* Physics 1, 6A or 21 Soph. year: Math 4B Math 6B Math 108A*** Math 6A</p> <div class="credits"> <p class="dwt_author">Akhmedov, Azer</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">352</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/39885006"> <span id="translatedtitle">Describing Baseline Conditions: <span class="hlt">Suggestions</span> for Study Reports</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Experimental research involves comparing two or more conditions. One of those conditions in single subject research is often\\u000a the baseline. Adequate description of the baseline conditions is necessary for evaluating the effects of independent variables,\\u000a drawing generalizations from studies, and providing information for subsequent replication studies. <span class="hlt">Suggestions</span> are made about\\u000a the types of information to include when describing baseline conditions</p> <div class="credits"> <p class="dwt_author">Mark Wolery; Brian Reichow; Leslie Rogers</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">353</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014ASPC..490...63M"> <span id="translatedtitle">The Multiple <span class="hlt">Periods</span> and the Magnetic Nature of CP Puppis</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Fast cadence time resolved spectra taken at the CTIO-4 m telescope with the RC-spectrograph during 2 consecutive nights revealed a long term modulation of the binary radial velocity. Chandra hard X-ray spectra taken with the HETGS instrument showed features typically <span class="hlt">observed</span> in magnetic white dwarfs. Here, we present the new data and <span class="hlt">suggest</span> that CP Pup is possibly a long orbital <span class="hlt">period</span> intermediate polar.</p> <div class="credits"> <p class="dwt_author">Mason, E.; Bianchini, A.; Orio, M.; Williams, R. E.; Mukai, K.; de Marino, D.; Abbot, T. M. C.; di Mille, F.</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">354</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011PhRvE..83d1919K"> <span id="translatedtitle">Ergodicity convergence test <span class="hlt">suggests</span> telomere motion obeys fractional dynamics</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Anomalous diffusion, <span class="hlt">observed</span> in many biological processes, is a generalized description of a wide variety of processes, all obeying the same law of mean-square displacement. Identifying the basic mechanisms of these <span class="hlt">observations</span> is important for deducing the nature of the biophysical systems measured. We implement a previously <span class="hlt">suggested</span> method for distinguishing between fractional Langevin dynamics, fractional Brownian motion, and continuous time random walk based on the ergodic nature of the data. We apply the method together with the recently <span class="hlt">suggested</span> P-variation test and the displacement correlation to the lately measured dynamics of telomeres in the nucleus of mammalian cells and find strong evidence that the telomeres motion obeys fractional dynamics. The ergodic dynamics are <span class="hlt">observed</span> experimentally to fit fractional Brownian or Langevin dynamics.</p> <div class="credits"> <p class="dwt_author">Kepten, E.; Bronshtein, I.; Garini, Y.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-04-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">355</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ninds.nih.gov/disorders/periodic_paralysis/periodic_paralysis.htm"> <span id="translatedtitle">Familial <span class="hlt">Periodic</span> Paralyses</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://medlineplus.gov/">MedlinePLUS</a></p> <p class="result-summary">NINDS Familial <span class="hlt">Periodic</span> Paralyses Information Page Synonym(s): <span class="hlt">Periodic</span> Paralyses Table of Contents (click to jump to sections) What are Familial <span class="hlt">Periodic</span> Paralyses? Is there any treatment? What is the prognosis? What research is ...</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">356</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ia.usu.edu/viewproject.php?project=ia:5338"> <span id="translatedtitle">So Many <span class="hlt">Periodic</span> Tables!</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary"><span class="hlt">Periodic</span> tables come in a variety of shapes and formats. Some <span class="hlt">periodic</span> tables have a flair of creativity! Take a look at these different versions of <span class="hlt">Periodic</span> Tables at the following websites. You will be asked to reflect on the theme of <span class="hlt">periodicity</span> after exploring these websites. 1. Some <span class="hlt">Periodic</span> Tables provide a wealth of information about each element. Compare 2 different elements on the following <span class="hlt">Periodic</span> Tables. <span class="hlt">Periodic</span> Table Alive WebElements 2. <span class="hlt">Periodic</span> Tables can be organized in unique and unusual 2-dimensional and 3-dimensional formats. Analyse the organization of <span class="hlt">periodicity</span> in some of the following <span class="hlt">Periodic</span> Tables. Presentation Forms of the <span class="hlt">Periodic</span> Table Universal <span class="hlt">Periodic</span> Table 3. Sometimes the designer ...</p> <div class="credits"> <p class="dwt_author">Mrs. Suggs</p> <p class="dwt_publisher"></p> <p class="publishDate">2007-11-30</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">357</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/10833724"> <span id="translatedtitle"><span class="hlt">Suggesting</span> strategies improves creative visual synthesis.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">An experiment assessed whether a figural or an interpretative strategy can enhance creative visual synthesis. 45 undergraduates were presented a set of simple figures and asked to imagine combining them to obtain a whole pattern corresponding to a creative product. In the figurative condition participants were instructed to combine figures in unusual ways; in the interpretative condition they were induced to look for unusual meanings embedded in the combinations; in the control condition no strategy was <span class="hlt">suggested</span>. Results showed that certain strategies induced a more flexible visual synthesis. PMID:10833724</p> <div class="credits"> <p class="dwt_author">Antonietti, A; Martini, E</p> <p class="dwt_publisher"></p> <p class="publishDate">2000-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">358</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/48570368"> <span id="translatedtitle"><span class="hlt">Suggestion</span> of Complex Monitoring of Undermined Territory</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">\\u000a Underground mining of coal deposits in Ostrava-Karvina region causes movements and deformations on the surface where a subsidence\\u000a depression starts to develop. Real displays of undermining can be only found out by repeated in situ measurements; geodetic\\u000a and geophysical methods can be used. Photogrammetry enables to <span class="hlt">observe</span> the whole subsidence depression and to create digital\\u000a terrain model. GPS is used</p> <div class="credits"> <p class="dwt_author">Hana Doležalová</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">359</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/15841294"> <span id="translatedtitle">[<span class="hlt">Suggestions</span> for buying medical equipment in hospitals].</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">TO THE EDITOR: Both in Greece and in other European countries there are plans to buy more medical equipment. If the whole procedure is not effective, it may result to a large deficit in the hospital budget. The total hospital deficit now in Greece is about 2.5 billion euros. It is <span class="hlt">suggested</span> that in every hospital, the Authorized Committee for Medical Equipment Purchasing, should include the following: One Director of a Medical Department related to the equipment to be bought and another Director of a Medical Department, unrelated. One accountant. One legal advisor specialized in hospital affairs. One economical advisor specialized in banking who will be able to <span class="hlt">suggest</span> leasing or other means of financing the purchase of the relevant equipment. A cost accounting analysis described by a detailed report, should be provided to secure that the equipment to be bought should be cost-effective and leaving a reasonable surplus after not more than 10 years from the time it is installed. Finally, the possibility of using one expensive equipment to cover the needs of more than one hospitals either by moving the equipment (i.e. the PET/CT camera by a large vehicle) or by transferring the patients to a central hospital, may be provided by the above Authorized Committee. PMID:15841294</p> <div class="credits"> <p class="dwt_author">Trontzos, Christos</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">360</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/1021193"> <span id="translatedtitle">Dinosaur Peptides <span class="hlt">Suggest</span> Mechanisms of Protein Survival</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Eleven collagen peptide sequences recovered from chemical extracts of dinosaur bones were mapped onto molecular models of the vertebrate collagen fibril derived from extant taxa. The dinosaur peptides localized to fibril regions protected by the close packing of collagen molecules, and contained few acidic amino acids. Four peptides mapped to collagen regions crucial for cell-collagen interactions and tissue development. Dinosaur peptides were not represented in more exposed parts of the collagen fibril or regions mediating intermolecular cross-linking. Thus functionally significant regions of collagen fibrils that are physically shielded within the fibril may be preferentially preserved in fossils. These results show empirically that structure-function relationships at the molecular level could contribute to selective preservation in fossilized vertebrate remains across geological time, <span class="hlt">suggest</span> a 'preservation motif', and bolster current concepts linking collagen structure to biological function. This non-random distribution supports the hypothesis that the peptides are produced by the extinct organisms and <span class="hlt">suggests</span> a chemical mechanism for survival.</p> <div class="credits"> <p class="dwt_author">San Antonio, James D.; Schweitzer, Mary H.; Jensen, Shane T.; Kalluri, Raghu; Buckley, Michael; Orgel, Joseph P.R.O. (Harvard-Med); (IIT); (NCSU); (UPENN); (Manchester); (Orthovita)</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-09-16</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_17");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return showDiv("page_1");' href="#">1</a> <a onClick='return showDiv("page_2");' href="#">2</a> <a onClick='return showDiv("page_3");' 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src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">361</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.msss.com/mars_images/moc/june2000/"> <span id="translatedtitle">Recent Images <span class="hlt">Suggesting</span> Liquid Water on Mars</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">Recently, the press reported that the Mars Orbiter Camera (MOC) had captured compelling images of gullies and slope failures that might be associated with the presence of liquid water on Mars. Now you can see these famous images at Malin Space Science Systems' MOC Website. These sharp, beautiful, color images (.jpeg, .gif) are featured on pages containing descriptions of how such physical features are formed on earth. The images are available in two sizes (small = 360K, large = 690K). Highlights include the "gully landform" compared to channel and apron features on Mount Saint Helens on Earth, a 3-D image (3-D glasses required) of a "weeping" alcove in an impact crater, and clues <span class="hlt">suggesting</span> that the suspected liquid water on Mars is relatively young.</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">362</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/5036542"> <span id="translatedtitle">Elastic wave scattering methods: assessments and <span class="hlt">suggestions</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">The author was asked by the meeting organizers to review and assess the developments over the past ten or so years in elastic wave scattering methods and to <span class="hlt">suggest</span> areas of future research opportunities. He highlights the developments, focusing on what he feels were distinct steps forward in our theoretical understanding of how elastic waves interact with flaws. For references and illustrative figures, he decided to use as his principal source the proceedings of the various annual Reviews of Progress in Quantitative Nondestructive Evaluation (NDE). These meetings have been the main forum not only for presenting results of theoretical research but also for demonstrating the relevance of the theoretical research for the design and interpretation of experiment. In his opinion a quantitative NDE is possible only if this relevance exists, and his major objective is to discuss and illustrate the degree to which relevance has developed.</p> <div class="credits"> <p class="dwt_author">Gubernatis, J.E.</p> <p class="dwt_publisher"></p> <p class="publishDate">1985-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">363</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25554800"> <span id="translatedtitle"><span class="hlt">Periodic</span> breathing in healthy humans at exercise in hypoxia.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary"><span class="hlt">Periodic</span> breathing is frequent in heart failure or ventilatory disorders during sleep, and common during sleep at high altitude, but has been rarely studied in wakefulness and during exercise. A retrospective analysis of ventilation from hypoxia exercise tests was realized in 82 healthy subjects separated into two groups with either high or low ventilatory response to hypoxia at exercise (HVRe). A fast Fourier transform spectral analysis of the breath-by-breath ventilation (V?e) signal, O2 saturation, and end-tidal PCO2 evidenced a <span class="hlt">periodic</span> pattern with a <span class="hlt">period</span> of 11.1 to 12.0 s. The peak power of the V?e spectrum was higher in the high HVRe group (P < 0.001). A prospective study (25 subjects) was performed to evaluate the influence of cardiorespiratory factors on the amplitude and <span class="hlt">period</span> of oscillations in various conditions of exercise (20 to 40% maximal aerobic power) and hypoxia (0 to 4,000 m altitude). The <span class="hlt">period</span> of V?e was shorter at exercise (vs. rest, P < 0.001) and hypoxia (vs. normoxia, P < 0.001), and inversely related with cardiac output and V?e (P < 0.001). V?e peak power was higher at exercise (P < 0.001) and hypoxia (P < 0.001), and was positively related with cardiac output and V?e (P < 0.001). V?e peak power in hypoxia was positively related with the ventilatory response to CO2 (HCVR). This novel <span class="hlt">observation</span> <span class="hlt">suggests</span> that healthy subjects demonstrate a spontaneous <span class="hlt">periodic</span> breathing, not clearly <span class="hlt">observable</span> at rest and in normoxia, but triggered by hypoxic exercise. The <span class="hlt">periodic</span> pattern is enhanced in subjects with high HVRe and high HCVR, <span class="hlt">suggesting</span> that oxygen and CO2 play synergistic roles in the modulation of these oscillations. PMID:25554800</p> <div class="credits"> <p class="dwt_author">Hermand, Eric; Pichon, Aurélien; Lhuissier, François J; Richalet, Jean-Paul</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">364</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/23045690"> <span id="translatedtitle">Critical <span class="hlt">period</span> for acoustic preference in mice.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Preference behaviors are often established during early life, but the underlying neural circuit mechanisms remain unknown. Adapting a unique nesting behavior assay, we confirmed a "critical <span class="hlt">period</span>" for developing music preference in C57BL/6 mice. Early music exposure between postnatal days 15 and 24 reversed their innate bias for silent shelter, which typically could not be altered in adulthood. Instead, exposing adult mice treated acutely with valproic acid or carrying a targeted deletion of the Nogo receptor (NgR(-/-)) unmasked a strong plasticity of preference consistent with a reopening of the critical <span class="hlt">period</span> as seen in other systems. Imaging of cFos expression revealed a prominent neuronal activation in response to the exposed music in the prelimbic and infralimbic medial prefrontal cortex only under conditions of open plasticity. Neither behavioral changes nor selective medial prefrontal cortex activation was <span class="hlt">observed</span> in response to pure tone exposure, indicating a music-specific effect. Open-field center crossings were increased concomitant with shifts in music preference, <span class="hlt">suggesting</span> a potential anxiolytic effect. Thus, music may offer both a unique window into the emotional state of mice and a potentially efficient assay for molecular "brakes" on critical <span class="hlt">period</span> plasticity common to sensory and higher order brain areas. PMID:23045690</p> <div class="credits"> <p class="dwt_author">Yang, Eun-Jin; Lin, Eric W; Hensch, Takao K</p> <p class="dwt_publisher"></p> <p class="publishDate">2012-10-16</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">365</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19910018813&hterms=audrey&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Daudrey"> <span id="translatedtitle"><span class="hlt">Suggested</span> criteria for evaluating systems engineering methodologies</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Systems engineering is the application of mathematical and scientific principles to practical ends in the life-cycle of a system. A methodology for systems engineering is a carefully developed, relatively complex procedure or process for applying these mathematical and scientific principles. There are many systems engineering methodologies (or possibly many versions of a few methodologies) currently in use in government and industry. These methodologies are usually designed to meet the needs of a particular organization. It has been <span class="hlt">observed</span>, however, that many technical and non-technical problems arise when inadequate systems engineering methodologies are applied by organizations to their systems development projects. Various criteria for evaluating systems engineering methodologies are discussed. Such criteria are developed to assist methodology-users in identifying and selecting methodologies that best fit the needs of the organization.</p> <div class="credits"> <p class="dwt_author">Gates, Audrey; Paul, Arthur S.; Gill, Tepper L.</p> <p class="dwt_publisher"></p> <p class="publishDate">1989-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">366</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=yield&pg=4&id=EJ862631"> <span id="translatedtitle"><span class="hlt">Suggestibility</span> under Pressure: Theory of Mind, Executive Function, and <span class="hlt">Suggestibility</span> in Preschoolers</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Eighty preschoolers, ages 3 to 5 years old, completed a 4-phase study in which they experienced a live event and received a pressured, <span class="hlt">suggestive</span> interview about the event a week later. Children were also administered batteries of theory of mind and executive function tasks, as well as the Video <span class="hlt">Suggestibility</span> Scale for Children (VSSC), which…</p> <div class="credits"> <p class="dwt_author">Karpinski, Aryn C.; Scullin, Matthew H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">367</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010Ap%26SS.330..243D"> <span id="translatedtitle">A cyclical <span class="hlt">period</span> variation detected in the updated orbital <span class="hlt">period</span> analysis of TV Columbae</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Two CCD photometries of the intermediate polar TV Columbae are made for obtaining two updated eclipse timings with high precision. There is an interval time ˜17 yr since the last mid-eclipse time <span class="hlt">observed</span> in 1991. Thus, the new mid-eclipse times might offer an opportunity to check the previous orbital ephemerides. A calculation indicates that the orbital ephemeris derived by Augusteijn et al. (Astron. Astrophys. Suppl. Ser. 107:219, 1994) should be corrected. Based on the proper linear ephemeris (Hellier in Mon. Not. R. Astron. Soc. 264:132, 1993), the new orbital <span class="hlt">period</span> analysis <span class="hlt">suggests</span> a cyclical <span class="hlt">period</span> variation in the O-C diagram of TV Columbae. Using Applegate’s mechanism to explain the <span class="hlt">periodic</span> oscillation in the O-C diagram, the required energy is larger than the energy that a M0-type star can afford over a complete variation <span class="hlt">period</span> of ˜31.0(±3.0) yr. Thus, the light travel-time effect indicates that the tertiary component in TV Columbae may be a dwarf with a low mass, which is near the lower mass limit of ˜0.08 M ? as long as the inclination of the third body is high enough.</p> <div class="credits"> <p class="dwt_author">Dai, Zhibin; Qian, Shengbang; Fernández Lajús, Eduardo; Baume, G. L.</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">368</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2013AGUFM.S22A..05S"> <span id="translatedtitle">Failures and <span class="hlt">suggestions</span> in Earthquake forecasting and prediction</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Seismologists have had poor success in earthquake prediction. However, wide ranging <span class="hlt">observations</span> from earlier great earthquakes show that precursory data can exist. In particular, two aspects seem promising. In agreement with simple physical modeling, b-values decrease in highly loaded fault zones for years before failure. Potentially more usefully, in high stress regions, breakdown of dilatant patches leading to failure can yield expelled water-related <span class="hlt">observations</span>. The volume increase (dilatancy) caused by high shear stresses decreases the pore pressure. Eventually, water flows back in restoring the pore pressure, promoting failure and expelling the extra water. Of course, in a generally stressed region there may be many small patches that fail, such as <span class="hlt">observed</span> before the 1975 Haicheng earthquake. Only a few days before the major event will most of the dilatancy breakdown occur in the fault zone itself such as for the Tangshan, 1976 destructive event. <span class="hlt">Observations</span> of 'water release' effects have been <span class="hlt">observed</span> before the 1923 great Kanto earthquake, the 1984 Yamasaki event, the 1975 Haicheng and the 1976 Tangshan earthquakes and also the 1995 Kobe earthquake. While there are obvious difficulties in water release <span class="hlt">observations</span>, not least because there is currently no <span class="hlt">observational</span> network anywhere, historical data does <span class="hlt">suggest</span> some promise if we broaden our approach to this difficult subject.</p> <div class="credits"> <p class="dwt_author">Sacks, S. I.</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-12-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">369</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015MPBu...42..149W"> <span id="translatedtitle">Rotational <span class="hlt">Period</span> of 10042 Budstewart</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">We report photometric <span class="hlt">observations</span> of the main-belt asteroid 10042 Budstewart made on five nights in 2014 September and October. We obtain a well-determined synodic rotation <span class="hlt">period</span> of 3.695 ± 0.002 h and amplitude of 0.33 ± 0.02 mag.</p> <div class="credits"> <p class="dwt_author">Warell, Johan; Klinglesmith, Daniel A., III; DeHart, Austin</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">370</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/133892"> <span id="translatedtitle">Evidence <span class="hlt">suggesting</span> possible SCA1 gene involvement in schizophrenia</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Several findings <span class="hlt">suggest</span> a possible role for the SCA1 gene on chromosome 6p in some cases of schizophrenia. First, linkage analyses in Irish pedigrees provided LOD scores up to 3.0 for one model tested using microsatellites closely linked to SCA1. Reanalysis of these data using affected sibpair methods yielded a significant result (p = 0.01) for one marker. An attempt to replicate this linkage finding was made using 44 NIMH families (206 individuals, 80 affected) and 12 Utah families (120 individuals, 49 affected). LOD scores were negative in these new families, even allowing for heterogeneity, as were results using affected sibpair methods. However, one Utah family provided a LOD score of 1.3. We also screened the SCA1 trinucleotide repeat to search for expansions characteristic of this disorder in these families and in 38 additional unrelated schizophrenics. We found 1 schizophrenic with 41 repeats, which is substantially larger than the maximum size of 36 repeats <span class="hlt">observed</span> in previous studies of several hundred controls. We are now assessing whether the distribution of SCA1 repeats differs significantly in schizophrenia versus controls. Recent reports <span class="hlt">suggest</span> possible anticipation in schizophrenia (also characteristic of SCA1) and a few cases of psychiatric symptoms <span class="hlt">suggesting</span> schizophrenia have been <span class="hlt">observed</span> in the highly related disorder DRPLA (SCA2), which is also based on trinucleotide repeat expansion. These findings <span class="hlt">suggest</span> that further investigations of this gene and chromosome region may be a priority.</p> <div class="credits"> <p class="dwt_author">Diehl, S.R.; Wange, S.; Sun, C. [NIDR, Bethesda, MD (United States)] [and others</p> <p class="dwt_publisher"></p> <p class="publishDate">1994-09-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">371</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2015MPBu...42...90P"> <span id="translatedtitle">Rotation <span class="hlt">Period</span> Determination for 1110 Jaroslawa</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">On the basis of more than two months of photometric <span class="hlt">observations</span> we find for 1110 Jaroslawa synodic rotation <span class="hlt">period</span> near 97.4 hours and amplitude near 0.65 magnitudes. We find evidence of changes in amplitude and synodic <span class="hlt">period</span> with changing phase angle and phase angle bisector, but were not able to obtain sufficient <span class="hlt">observations</span> to document these completely.</p> <div class="credits"> <p class="dwt_author">Pilcher, Frederick; Ferrero, Andrea; Klinglesmith, Daniel A., III; Hanowell, Jesse</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">372</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/10127910"> <span id="translatedtitle">Employee <span class="hlt">suggestion</span> programs: the rewards of involvement.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Successful ESPs are the products of a great deal of effort by managers, administrators, teams, individuals, and reviewers, who are all striving to achieve the goals of increased profitability and enhanced employee involvement. A review of the literature indicates that there are several prescriptions that will increase the likelihood of a successful ESP (see the box). Today's American business prophets sound ceaseless calls to arms in the name of "world class performance," "global competitiveness," "total quality management," and a variety of other buzz terms. A burgeoning industry has evolved that promises, through speeches, teleconferences, seminars, and consulting contracts, to teach American organizations how to achieve excellence. In the face of a sputtering economy and unrelenting competitive pressure, today's managers must translate these laudatory ideals into hands-on reality without sacrificing the firm's profit margin to experimentation. If any idea can help an organization achieve improvement through a workable program, then that idea and that program deserve real consideration. An ESP represents an opportunity to tap the intelligence and resourcefulness of an organization's employees, and by doing so, reap significant cost savings. Those companies and managers that have an ESP program uniformly list economic advantages first when describing the benefits of their employee <span class="hlt">suggestion</span> programs. But there is another deeper and longer term benefit inherent in an ESP. These programs allow employees to become involved in their organization; they drive deaccession to lower levels, they give employees more responsibility, they foster creative approaches to work, and they encourage creativity in pursuit of company goals.(ABSTRACT TRUNCATED AT 250 WORDS) PMID:10127910</p> <div class="credits"> <p class="dwt_author">Mishra, J M; McKendall, M</p> <p class="dwt_publisher"></p> <p class="publishDate">1993-09-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">373</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/22238861"> <span id="translatedtitle">The effect of women's <span class="hlt">suggestive</span> clothing on men's behavior and judgment: a field study.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Numerous studies have shown that men overestimate the sexual intent of women based on their clothing style; however, this hypothesis has not been assessed empirically in a natural setting. This small field study measured the time it took for men to approach two female confederates sitting in a tavern, one wearing <span class="hlt">suggestive</span> clothes and one wearing more conservative clothes. The behavior of 108 men was <span class="hlt">observed</span> over 54 <span class="hlt">periods</span> on 16 different nights in two different taverns. The time it took for the men to approach after initial eye contact was significantly shorter in the <span class="hlt">suggestive</span> clothing condition. The men were also asked by male confederates to rate the likelihood of having a date with the women, and having sex on the first date. The men rated their chances to have a date and to have sex significantly higher in the <span class="hlt">suggestive</span> clothing condition. Results are discussed with respect to men's possible misinterpretation that women's clothing indicates sexual interest, and the risks associated with the misinterpretation. PMID:22238861</p> <div class="credits"> <p class="dwt_author">Guéguen, Nicolas</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-10-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">374</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19950025912&hterms=red+cedar&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D20%26Ntt%3Dred%2Bcedar"> <span id="translatedtitle">Relativistic timescale analysis <span class="hlt">suggests</span> lunar theory revision</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The SI second of the atomic clock was calibrated to match the Ephemeris Time (ET) second in a mutual four year effort between the National Physical Laboratory (NPL) and the United States Naval Observatory (USNO). The ephemeris time is 'clocked' by <span class="hlt">observing</span> the elapsed time it takes the Moon to cross two positions (usually occultation of stars relative to a position on Earth) and dividing that time span into the predicted seconds according to the lunar equations of motion. The last revision of the equations of motion was the Improved Lunar Ephemeris (ILE), which was based on E. W. Brown's lunar theory. Brown classically derived the lunar equations from a purely Newtonian gravity with no relativistic compensations. However, ET is very theory dependent and is affected by relativity, which was not included in the ILE. To investigate the relativistic effects, a new, noninertial metric for a gravitated, translationally accelerated and rotating reference frame has three sets of contributions, namely (1) Earth's velocity, (2) the static solar gravity field and (3) the centripetal acceleration from Earth's orbit. This last term can be characterized as a pseudogravitational acceleration. This metric predicts a time dilation calculated to be -0.787481 seconds in one year. The effect of this dilation would make the ET timescale run slower than had been originally determined. Interestingly, this value is within 2 percent of the average leap second insertion rate, which is the result of the divergence between International Atomic Time (TAI) and Earth's rotational time called Universal Time (UT or UTI). Because the predictions themselves are significant, regardless of the comparison to TAI and UT, the authors will be rederiving the lunar ephemeris model in the manner of Brown with the relativistic time dilation effects from the new metric to determine a revised, relativistic ephemeris timescale that could be used to determine UT free of leap second adjustments.</p> <div class="credits"> <p class="dwt_author">Deines, Steven D.; Williams, Carol A.</p> <p class="dwt_publisher"></p> <p class="publishDate">1995-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">375</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/25594911"> <span id="translatedtitle">Hypnosis, hypnotic <span class="hlt">suggestibility</span>, memory, and involvement in films.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Our research extends studies that have examined the relation between hypnotic <span class="hlt">suggestibility</span> and experiential involvement and the role of an hypnotic induction in enhancing experiential involvement (e.g., absorption) in engaging tasks. Researchers have reported increased involvement in reading (Baum & Lynn, 1981) and music-listening (Snodgrass & Lynn, 1989) tasks during hypnosis. We predicted a similar effect for film viewing: greater experiential involvement in an emotional (The Champ) versus a non-emotional (Scenes of Toronto) film. We tested 121 participants who completed measures of absorption and trait dissociation and the Harvard Group Scale of Hypnotic Susceptibility and then viewed the two films after either an hypnotic induction or a non-hypnotic task (i.e., anagrams). Experiential involvement varied as a function of hypnotic <span class="hlt">suggestibility</span> and film clip. Highly <span class="hlt">suggestible</span> participants reported more state depersonalization than less <span class="hlt">suggestible</span> participants, and depersonalization was associated with negative affect; however, we <span class="hlt">observed</span> no significant correlation between hypnotic <span class="hlt">suggestibility</span> and trait dissociation. Although hypnosis had no effect on memory commission or omission errors, contrary to the hypothesis that hypnosis facilitates absorption in emotionally engaging tasks, the emotional film was associated with more commission and omission errors compared with the non-emotional film. PMID:25594911</p> <div class="credits"> <p class="dwt_author">Maxwell, Reed; Lynn, Steven Jay; Condon, Liam</p> <p class="dwt_publisher"></p> <p class="publishDate">2015-05-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">376</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/biblio/6596860"> <span id="translatedtitle">Latent <span class="hlt">period</span> in clinical radiation myelopathy</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Seventy-seven papers containing data on more than 300 cases of radiation myelopathy have been analyzed. The data <span class="hlt">suggest</span> that the latent <span class="hlt">periods</span> are similar in the cervical and thoracic levels of the spinal cord and are bimodally distributed. Myelopathy of lumbar cord apparently has a shorter latent <span class="hlt">period</span>. As in controlled animal experiments, the latent <span class="hlt">period</span> decreases with increasing dose. Furthermore, the variation in latent <span class="hlt">periods</span> also decreases with dose. It is also seen that retreated patients and pediatric or adolescent patients have greatly reduced latent <span class="hlt">periods</span>. The implications of these findings as they compare with the animal data are discussed.</p> <div class="credits"> <p class="dwt_author">Schultheiss, T.E.; Higgins, E.M.; El-Mahdi, A.M.</p> <p class="dwt_publisher"></p> <p class="publishDate">1984-07-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">377</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19910016743&hterms=Conglomerate&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D40%26Ntt%3DConglomerate"> <span id="translatedtitle">Short-<span class="hlt">period</span> comets</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The spacecraft flybys of Comet Halley in 1986 confirmed Whipple's icy conglomerate hypothesis for cometary nuclei and showed that comets are far richer in volatiles than any other class of solar system bodies. Water is the most abundant volatile, comprising roughly 80 percent of the gas flowing out from the nucleus. Carbon monoxide is next with a content of 15 percent relative to water, though with approximately half of that coming from an extended source in the cometary coma, i.e., hydrocarbon dust grains. The detection of large numbers of hydrocarbon CHON grains was one of the more significant discoveries of the Halley flybys, as was the ground-based <span class="hlt">observation</span> that CN occurs in jets, again indicating an extended source. Evidence was also found for more complex hydrocarbons. Estimates of the total dust-to-gas ratio for Halley range as high as 2:1, indicating that a substantial fraction of the volatile material may be tied up in solid hydrocarbons rather than ices. The role of clathrates in trapping more volatile ices is not yet understood. If Halley can be taken to be representative of all short-<span class="hlt">period</span> comets, then the short-<span class="hlt">period</span> comets may provide a significant source of volatiles in near-earth space. This resource is more difficult to reach dynamically than the near-earth asteriods, but the high volatile content may justify the additional effort necessary. In addition, there is considerable evidence that at least some fraction of the near-earth asteriods are extinct cometary nuclei which have evolved into asteroid orbits, and which may contain significant volatiles buried beneath an insulating lag-deposit crust of nonvolatiles. Knowledge of comets will be greatly enhanced in the near future by the Comet Rendezvous Flyby mission now under development by NASA, and by the proposed Rosetta mission.</p> <div class="credits"> <p class="dwt_author">Weissman, Paul R.; Campins, Humberto</p> <p class="dwt_publisher"></p> <p class="publishDate">1991-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">378</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://prevention.cancer.gov/programs-resources/groups/b/software/screening"> <span id="translatedtitle"><span class="hlt">Periodic</span> Screening Evaluation</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.cancer.gov">Cancer.gov</a></p> <p class="result-summary">Statistical Software <span class="hlt">Periodic</span> Screening Evaluation (Written by Stuart G. Baker) New Approach (Simplified Approximation): See Baker SG. Evaluating <span class="hlt">periodic</span> cancer screening without a randomized control group: a simplified design and analysis. In: Duffy</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">379</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.agu.org/journals/jz/v067/i005/JZ067i005p02066/JZ067i005p02066.pdf"> <span id="translatedtitle">Correlation of Short-<span class="hlt">Period</span> Fluctuations of the Earth's Magnetic Field and Instantaneous Frequency Measurements</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Rapid fluctuations of the instantaneous re- ceived frequency of stable HF CW transmissions have been <span class="hlt">observed</span> during <span class="hlt">periods</span> of geomag- netic disturbances by Watts and Davies (1960) and by Fenwick and Villard (1960). A possible correlation of these fluctuations to magnetic field changes has been <span class="hlt">suggested</span> by Fenwick and Villard (1960); Chan, Villard, and Dueo (1961); and Kanellakos and Villard</p> <div class="credits"> <p class="dwt_author">K. L. Chan; D. P. Kanellakos; O. G. Villard</p> <p class="dwt_publisher"></p> <p class="publishDate">1962-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">380</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/0809.0046v1"> <span id="translatedtitle">Time-<span class="hlt">periodic</span> universes</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">In this letter we construct a new time-<span class="hlt">periodic</span> solution of the vacuum Einstein's field equations whose Riemann curvature norm takes the infinity at some points. We show that this solution is intrinsically time-<span class="hlt">periodic</span> and describes a time-<span class="hlt">periodic</span> universe with the "black hole". New physical phenomena are investigated and new singularities are analyzed for this universal model.</p> <div class="credits"> <p class="dwt_author">De-Xing Kong; Kefeng Liu; Ming Shen</p> <p class="dwt_publisher"></p> <p class="publishDate">2008-08-30</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_18");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.previous.18x20.png" alt="Previous Page" /></a> <span id="PageLinks" class="pageLinks"> <span> <a onClick='return 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showDiv("page_21");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">381</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=atom&pg=2&id=EJ1028694"> <span id="translatedtitle">The <span class="hlt">Periodic</span> Pyramid</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">The chemical elements present in the modern <span class="hlt">periodic</span> table are arranged in terms of atomic numbers and chemical <span class="hlt">periodicity</span>. <span class="hlt">Periodicity</span> arises from quantum mechanical limitations on how many electrons can occupy various shells and subshells of an atom. The shell model of the atom predicts that a maximum of 2, 8, 18, and 32 electrons can occupy…</p> <div class="credits"> <p class="dwt_author">Hennigan, Jennifer N.; Grubbs, W. Tandy</p> <p class="dwt_publisher"></p> <p class="publishDate">2013-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">382</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://arxiv.org/pdf/astro-ph/0611482v1"> <span id="translatedtitle">Analysis of the eclipsing binaries in the LMC discovered by OGLE: <span class="hlt">Period</span> distribution and frequency of the short-<span class="hlt">period</span> binaries</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">We review the results of our analysis of the OGLE LMC eclipsing binaries (Mazeh, Tamuz & North 2006), using EBAS -- Eclipsing Binary Automated Solver, an automated algorithm to fit lightcurves of eclipsing binaries (Tamuz, Mazeh & North 2006). After being corrected for <span class="hlt">observational</span> selection effects, the set of detected eclipsing binaries yielded the <span class="hlt">period</span> distribution and the frequency of all LMC short-<span class="hlt">period</span> binaries, and not just the eclipsing systems. Somewhat surprisingly, the <span class="hlt">period</span> distribution is consistent with a flat distribution in log P between 2 and 10 days. The total number of binaries with <span class="hlt">periods</span> shorter than 10 days in the LMC was estimated to be about 5000. This figure led us to <span class="hlt">suggest</span> that (0.7 +- 0.4)% of the main-sequence A- and B-type stars are found in binaries with <span class="hlt">periods</span> shorter than 10 days. This frequency is substantially smaller than the fraction of binaries found by small Galactic radial-velocity surveys of B stars.</p> <div class="credits"> <p class="dwt_author">Tsevi Mazeh; Omer Tamuz; Pierre North</p> <p class="dwt_publisher"></p> <p class="publishDate">2006-11-15</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">383</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/44278460"> <span id="translatedtitle">Identifying anthropogenic sources of nitrogen oxide emissions from calculations of Lagrangian trajectories and the <span class="hlt">observational</span> data from a tall tower in Siberia during the spring-summer <span class="hlt">period</span> of 2007</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">The task of identifying climatically significant regional anthropogenic emissions and estimating their contribution to the\\u000a variability of nitrogen oxides <span class="hlt">observed</span> at a monitoring station is considered on the basis of NO and NO2 surface concentrations measured at the Zotino background <span class="hlt">observation</span> station (60°26? N, 89°24? E, Krasnoyarsk Territory).\\u000a The approach used is based on an estimation of the conditional probability</p> <div class="credits"> <p class="dwt_author">A. V. Vivchar; K. B. Moiseenko; R. A. Shumskii; A. I. Skorokhod</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">384</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=Periodization+AND+training+AND+cycling&id=EJ663778"> <span id="translatedtitle"><span class="hlt">Periodization</span> Research and an Example Application.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">Describes <span class="hlt">periodization</span> in strength training (the cycling of specificity, intensity, and volume of training to achieve peak levels of performance for the most important conditions), <span class="hlt">suggesting</span> that well-designed <span class="hlt">periodized</span> programs will allow superior performance at the appropriate time, reduction in overtraining potential, systematic control over…</p> <div class="credits"> <p class="dwt_author">Graham, John</p> <p class="dwt_publisher"></p> <p class="publishDate">2002-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">385</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.ncbi.nlm.nih.gov/pubmed/9671803"> <span id="translatedtitle">Clines of nuclear DNA markers <span class="hlt">suggest</span> a largely neolithic ancestry of the European gene pool.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.ncbi.nlm.nih.gov/entrez/query.fcgi?DB=pubmed">PubMed</a></p> <p class="result-summary">Comparisons between archaeological findings and allele frequencies at protein loci <span class="hlt">suggest</span> that most genes of current Europeans descend from populations that have been expanding in Europe in the last 10, 000 years, in the Neolithic <span class="hlt">period</span>. Recent mitochondrial data have been interpreted as indicating a much older, Paleolithic ancestry. In a spatial autocorrelation study at seven hypervariable loci in Europe (four microsatellites, two larger, tandem-repeat loci, and a sequence polymorphism) broad clinal patterns of DNA variation were recognized. The <span class="hlt">observed</span> clines closely match those described at the protein level, in agreement with a possible Near Eastern origin for the ancestral population. Separation times between populations were estimated on the basis of a stepwise mutation model. Even assuming low mutation rates and long generation times, we found no evidence for population splits older than 10,000 years, with the predictable exception of Saami (Lapps). The simplest interpretation of these results is that the current nuclear gene pool largely reflects the westward and northward expansion of a Neolithic group. This conclusion is now supported by purely genetic evidence on the levels and patterns of microsatellite diversity, rather than by correlations of biological and nonbiological data. We argue that many mitochondrial lineages whose origin has been traced back to the Paleolithic <span class="hlt">period</span> probably reached Europe at a later time. PMID:9671803</p> <div class="credits"> <p class="dwt_author">Chikhi, L; Destro-Bisol, G; Bertorelle, G; Pascali, V; Barbujani, G</p> <p class="dwt_publisher"></p> <p class="publishDate">1998-07-21</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">386</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/10137483"> <span id="translatedtitle">Radial and nonradial <span class="hlt">periods</span> and growth rates of an AI Velorum model</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Walraven, Walraven, and Balona recently discovered several new <span class="hlt">periodicities</span> in addition to the well-known fundamental and first overtone <span class="hlt">periods</span> of the high-amplitude {delta} Scuti star AI Velorum. Linear nonadiabatic pulsation calculations were performed for an AI Velorum model of mass 1.96 M{sub {circle_dot}}, 24.05 L{sub {circle_dot}}, and T{sub eff}7566 K for the radial and low-degree nonradial modes to help verify the tentative identifications made by Walraven, et al. Comparison of the calculated <span class="hlt">periods</span> with the <span class="hlt">observations</span> <span class="hlt">suggests</span> some alternatives to the identifications proposed by Walraven, et al.</p> <div class="credits"> <p class="dwt_author">Guzik, J.A.</p> <p class="dwt_publisher"></p> <p class="publishDate">1992-05-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">387</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.osti.gov/scitech/servlets/purl/5448318"> <span id="translatedtitle">Radial and nonradial <span class="hlt">periods</span> and growth rates of an AI Velorum model</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/scitech">SciTech Connect</a></p> <p class="result-summary">Walraven, Walraven, and Balona recently discovered several new <span class="hlt">periodicities</span> in addition to the well-known fundamental and first overtone <span class="hlt">periods</span> of the high-amplitude {delta} Scuti star AI Velorum. Linear nonadiabatic pulsation calculations were performed for an AI Velorum model of mass 1.96 M{sub {circle dot}}, 24.05 L{sub {circle dot}}, and T{sub eff}7566 K for the radial and low-degree nonradial modes to help verify the tentative identifications made by Walraven, et al. Comparison of the calculated <span class="hlt">periods</span> with the <span class="hlt">observations</span> <span class="hlt">suggests</span> some alternatives to the identifications proposed by Walraven, et al.</p> <div class="credits"> <p class="dwt_author">Guzik, J.A.</p> <p class="dwt_publisher"></p> <p class="publishDate">1992-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">388</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19830029065&hterms=composite+circular+cylindrical&qs=Ntx%3Dmode%2Bmatchall%26Ntk%3DAll%26N%3D0%26No%3D10%26Ntt%3Dcomposite%2Bcircular%2Bcylindrical"> <span id="translatedtitle">On composites with <span class="hlt">periodic</span> structure</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">The overall moduli of a composite with an isotropic elastic matrix containing <span class="hlt">periodically</span> distributed (anisotropic) inclusions or voids, can be expressed in terms of several infinite series which only depend on the geometry of the inclusions or voids, and hence can be computed once and for all for given geometries. For solids with <span class="hlt">periodic</span> structures these infinite series play exactly the same role as does Eshelby's tensor for a single inclusion or void in an unbounded elastic medium. For spherical and circular-cylindrical geometries, the required infinite series are calculated and the results are tabulated. These are then used to estimate the overall elastic moduli when either the overall strains or the overall stresses are prescribed, obtaining the same results. These results are compared with other estimates and with experimental data. It is found that the model of composites with <span class="hlt">periodic</span> structure yields estimates in excellent agreement with the experimental <span class="hlt">observations</span>.</p> <div class="credits"> <p class="dwt_author">Nemat-Nasser, S.; Iwakuma, T.; Hejazi, M.</p> <p class="dwt_publisher"></p> <p class="publishDate">1982-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">389</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ntrs.nasa.gov/search.jsp?R=19780013080&hterms=types+stains&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchall%26Ntt%3Dtypes%2Bstains"> <span id="translatedtitle">Infrared <span class="hlt">Observations</span> of Late Type Stars</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://ntrs.nasa.gov/search.jsp">NASA Technical Reports Server (NTRS)</a></p> <p class="result-summary">Substantive mass loss resulting in appreciable circumstellar dust envelopes is common in late-type stars. The evolutionary history and physical state of a cool star determine the chemistry within the outer stellar atmosphere mirrored by the molecular and particulate material present in the envelope. The <span class="hlt">observational</span> consequences of this debris determined by moderate spectral resolution infrared spectrophotometry are reviewed. Significant information is provided by <span class="hlt">observations</span> of the emergent energy flux of both the cool stellar photosphere and of the circumstellar dust envelope. The <span class="hlt">observation</span> <span class="hlt">suggests</span> that mass-loss occurs to some degree throughout late stellar evolutionary phases and that occasional <span class="hlt">periods</span> of high mass loss are not uncommon.</p> <div class="credits"> <p class="dwt_author">Merrill, K. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">1977-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">390</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2010PhDT.........1V"> <span id="translatedtitle"><span class="hlt">Periodic</span> solar wind density structures</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">This dissertation addresses a specific aspect of the Sun-Earth connection: we show that coronal activity creates <span class="hlt">periodic</span> density structures in the solar wind which convect radially outward and interact with Earth's magnetosphere. First, we analyze 11 years (1995-2005) of in situ solar wind density <span class="hlt">observations</span> from the Wind spacecraft and find that <span class="hlt">periodic</span> density structures occur at particular sets of radial length-scales more often than others. This indicates that these density fluctuations, which have radial length-scales of hundreds of megameters, cannot be attributed entirely to turbulence. Next, we analyze their effect on Earth's magnetosphere. Though these structures are not waves in the solar wind rest frame, they appear at discrete frequencies in Earth's reference frame. They compress the magnetosphere as they convect past, driving global magnetospheric oscillations at the same discrete frequencies as the <span class="hlt">periodic</span> density structures. Last, we investigate source regions and mechanisms of the <span class="hlt">periodic</span> solar wind density structures. We analyze the alpha particle to proton abundance ratio during events of <span class="hlt">periodic</span> density structures. In many events, the proton and alpha density fluctuations are anti- correlated, which strongly argues for either temporally or spatially varying coronal source plasma. We examine white light images of the solar wind taken with SECCHI HI1 on the STEREO spacecraft and find <span class="hlt">periodic</span> density structures as near to the Sun as 15 solar radii. The smallest resolvable <span class="hlt">periodic</span> structures that we identify are of comparable length to those found at 1 AU, providing further evidence that at least some <span class="hlt">periodic</span> density structures are generated in the solar corona as the solar wind is formed. Guided by the properties <span class="hlt">observed</span> during previous studies and the characteristics established through the work presented here, we examine possible candidate mechanisms in the solar corona that can form <span class="hlt">periodic</span> density structures. We conclude that: coronal activity creates coherent structures in the solar wind at smaller size scales than previously thought; corona-formed coherent structures persist to 1 AU largely intact; finally, a significant amount of discrete frequency wave power in Earth's magnetosphere is directly driven by these structures once they reach Earth.</p> <div class="credits"> <p class="dwt_author">Viall, Nicholeen Mary</p> <p class="dwt_publisher"></p> <p class="publishDate">2010-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">391</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.gpo.gov:80/fdsys/pkg/CFR-2010-title24-vol2/pdf/CFR-2010-title24-vol2-sec203-266.pdf"> <span id="translatedtitle">24 CFR 203.266 - <span class="hlt">Period</span> covered by <span class="hlt">periodic</span> MIP.</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.gpo.gov/fdsys/browse/collectionCfr.action?selectedYearFrom=2010&page.go=Go">Code of Federal Regulations, 2010 CFR</a></p> <p class="result-summary">...2010-04-01 false <span class="hlt">Period</span> covered by <span class="hlt">periodic</span> MIP. 203.266 Section 203.266 ...Obligations Mortgage Insurance Premiums-<span class="hlt">Periodic</span> Payment § 203.266 <span class="hlt">Period</span> covered by <span class="hlt">periodic</span> MIP. The initial MIP shall...</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate">2010-04-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">392</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://academic.research.microsoft.com/Publication/40784736"> <span id="translatedtitle">Apparent and effective creep parameters in single crystals of a nickel base superalloy. I. Incubation <span class="hlt">period</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Direct <span class="hlt">observation</span> of the dislocation structures in connection with the values of the effective parameters <span class="hlt">suggests</span> a creep model for that particular creep stage <span class="hlt">observed</span> in superalloys. The incubation <span class="hlt">period</span> may be described as a steady state creep rate when deformation is produced by the glide of a low density of mobile screw dislocations (p\\/sub m\\/ approximately equal to 10⁵</p> <div class="credits"> <p class="dwt_author">C. Carry; J. L. Strudel</p> <p class="dwt_publisher"></p> <p class="publishDate">1977-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">393</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://ia.usu.edu/viewproject.php?project=ia:15529"> <span id="translatedtitle">The <span class="hlt">Periodic</span> Table</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">The following will provide you with a brief overview of the <span class="hlt">Periodic</span> Table of Elements, as well as some interesting facts about the elements. There are also some games which will help you practice the names and symbols of the elements. A worksheet may be provided for you to record your newfound knowledge. Please follow the directions and links below to enlighten yourself on the wonders of the <span class="hlt">Periodic</span> Table. If provided, don't forget to fill in your worksheet as you go... Part A: Who, what, where and when? Read a brief History of the <span class="hlt">Periodic</span> Table:History of the PT2. Part B: Interactive <span class="hlt">Periodic</span> Tables: Find physical ...</p> <div class="credits"> <p class="dwt_author">Mrs. Cutting</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-05</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">394</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://spacemath.gsfc.nasa.gov/NASADocs/magbook2002.pdf#page=40"> <span id="translatedtitle">What is an Oscillation <span class="hlt">Period</span>?</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">This is an activity about oscillation. Learners will <span class="hlt">observe</span>, time, and graph the data of the side to side motion of the mirror used in the soda bottle magnetometer activity to determine the mirror's oscillation <span class="hlt">period</span>. This activity requires prior construction and experience in use of a soda bottle magnetometer, which is the eighth activity in the Exploring the Earth's Magnetic Field: An IMAGE Satellite Guide to the Magnetosphere educators guide. This is the ninth activity in the guide.</p> <div class="credits"> <p class="dwt_author"></p> <p class="dwt_publisher"></p> <p class="publishDate">2012-08-03</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">395</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/1996JGR...10126681E"> <span id="translatedtitle">Assimilative mapping of ionospheric electrodynamics in the thermosphere-ionosphere general circulation model comparisons with global ionospheric and thermospheric <span class="hlt">observations</span> during the GEM/SUNDIAL <span class="hlt">period</span> of March 28-29, 1992</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Satellite and ground-based <span class="hlt">observations</span> from March 28 to 29, 1992, were combined in the assimilative mapping of ionospheric electrodynamics (AMIE) procedure to derive realistic global distributions of the auroral precipitation and ionospheric convection which were used as inputs to the National Center for Atmospheric Research (NCAR) thermosphere-ionosphere general circulation model (TIGCM). Comparisons of neutral model winds were made with Fabry-Perot measurements and meridional winds derived from ionosondes. The peak equatorward winds occurred 1-2 hours later in the model. Gravity waves launched from high-latitude Joule heating sources reached the equator in about 2 hours and agreed with <span class="hlt">observed</span> variations in the height of the maximum electron density (hmF2) and in the meridional winds. Joule heating events produced minima in the O/N2 ratio that moved equatorward and usually westward in longitudinal strips which lasted about a day. Changes in the O/N2 ratio and in the peak electron density (NmF2) were strongly correlated so the <span class="hlt">observed</span> daytime NmF2 values for stations near 50° magnetic latitude were generally reproduced by AMIE-TIGCM on the second day of the simulation. The AMIE-TIGCM underestimated the electron density after midnight by up to a factor of 2 in midlatitudes, while the modeled F2 layer was about 35 km lower than the <span class="hlt">observations</span> at midnight. Shifting the model winds 2 hours earlier at night could double the NmF2 at 0400 LT and increase hmF2 by 20 km. NmF2 could also be increased at night by realistically increasing the TIGCM nighttime downward fluxes of O+ at the upper boundary.</p> <div class="credits"> <p class="dwt_author">Emery, B. A.; Lu, G.; Szuszczewicz, E. P.; Richmond, A. D.; Roble, R. G.; Richards, P. G.; Miller, K. L.; Niciejewski, R.; Evans, D. S.; Rich, F. J.; Denig, W. F.; Chenette, D. L.; Wilkinson, P.; Pulinets, S.; O'Loughlin, K. F.; Hanbaba, R.; Abdu, M.; Jiao, P.; Igarashi, K.; Reddy, B. M.</p> <p class="dwt_publisher"></p> <p class="publishDate">1996-12-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">396</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.agu.org/journals/ja/v101/iA12/96JA01285/96JA01285.pdf"> <span id="translatedtitle">Assimilative mapping of ionospheric electrodynamics in the thermosphere-ionosphere general circulation model comparisons with global ionospheric and thermospheric <span class="hlt">observations</span> during the GEM\\/SUNDIAL <span class="hlt">period</span> of March 28-29, 1992</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Satellite and ground-based <span class="hlt">observations</span> from March 28 to 29, 1992, were combined in the assimilative mapping of ionospheric electrodynamics (AMIE) procedure to derive realistic global distributions of the auroral precipitation and ionospheric convection which were used as inputs to the National Center for Atmospheric Research (NCAR) thermosphere-ionosphere general circulation model (TIGCM). Comparisons of neutral model winds were made with Fabry-Perot</p> <div class="credits"> <p class="dwt_author">B. A. Emery; G. Lu; E. P. Szuszczewicz; R. G. Roble; P. G. Richards; K. L. Miller; R. Niciejewski; D. S. Evans; F. J. Rich; W. F. Denig; D. L. Chenette; P. Wilkinson; S. Pulinets; K. F. O'Loughlin; R. Hanbaba; M. Abdu; P. Jiao; K. Igarashi; B. M. Reddy</p> <p class="dwt_publisher"></p> <p class="publishDate">1996-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">397</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2009GeoRL..3620103C"> <span id="translatedtitle">Dual <span class="hlt">periodicities</span> in energetic electrons at Saturn</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">The fluxes of energetic electrons (110-365 keV) in Saturn's magnetosphere were subjected to Lomb periodogram analyses for 1677 days from late 2004 to the middle of 2009. The electrons generally exhibited strong <span class="hlt">periodicities</span> at 10.82 hours and 10.60 hours for much of the ˜4.6 year interval. The longer <span class="hlt">period</span> was generally present all the time, while the shorter <span class="hlt">period</span> became prominent during the last ˜600 days of the interval. The 10.8-hour signal appeared strongly in <span class="hlt">observations</span> made north of the equator and weakly in the south, while the 10.6-hour signal appeared only for northern <span class="hlt">observations</span>. The dual <span class="hlt">periodicity</span> in the electrons is similar to that recently discovered in the Saturn kilometric radiation. <span class="hlt">Periods</span> in the 10.6 to 10.8 hour range are similar to the sun-referenced <span class="hlt">periods</span> of neutral winds measured in Saturn's polar atmospheres.</p> <div class="credits"> <p class="dwt_author">Carbary, J. F.; Mitchell, D. G.; Krimigis, S. M.; Krupp, N.</p> <p class="dwt_publisher"></p> <p class="publishDate">2009-10-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">398</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014RAA....14.1055S"> <span id="translatedtitle">Two <span class="hlt">suggested</span> configurations for the Chinese space telescope</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">China will establish a 2-meter space-based astronomical telescope. Its main science goals are performing a sky survey for research about dark matter and dark energy, and high resolution <span class="hlt">observations</span>. Some experts <span class="hlt">suggest</span> that this space telescope should be installed inside the Chinese space station. In accord with this <span class="hlt">suggestion</span> we put forward our first configuration, i.e., to adopt a coudé system for this telescope. This coudé system comes from the Chinese 2.16m telescope's coudé system, which includes a relay mirror so that excellent image quality can be obtained. In our second configuration, we <span class="hlt">suggest</span> that the whole space telescope fly freely as an independent satellite outside the space station. When it needs servicing, for example, changing instruments, refilling refrigerant or propellant, etc., this space telescope can fly near or even dock with the core space station. Although some space stations have had accompanying satellites, the one we propose is a space telescope that will be much larger than other accompanying satellites in terms of weight and volume. On the basis of the second configuration, we also put forward the following idea: the space station can be composed of several large independent modules if necessary.</p> <div class="credits"> <p class="dwt_author">Su, Ding-Qiang; Cui, Xiang-Qun</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-09-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">399</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.springerlink.com/index/w656123771375x2v.pdf"> <span id="translatedtitle">The <span class="hlt">Periodic</span> Table: An Eight <span class="hlt">Period</span> Table For The 21 st Centrury</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://academic.research.microsoft.com/">Microsoft Academic Search </a></p> <p class="result-summary">Throughout most of the 20th century, an eight-<span class="hlt">period</span> <span class="hlt">periodic</span> table (also known as an electron-configuration table) was offered as an improvement over the ubiquitous seven-<span class="hlt">period</span> format of wall charts and textbooks. The eight-<span class="hlt">period</span> version has never achieved wide acceptance although it has significant advantages. Many <span class="hlt">observers</span> have questioned the way helium is displayed in this format. Now, a reinterpretation of</p> <div class="credits"> <p class="dwt_author">Gary Katz</p> <p class="dwt_publisher"></p> <p class="publishDate">2001-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">400</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://pubs.er.usgs.gov/publication/70036583"> <span id="translatedtitle">The use (and misuse) of sediment traps in coral reef environments: Theory, <span class="hlt">observations</span>, and <span class="hlt">suggested</span> protocols</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p class="result-summary">Sediment traps are commonly used as standard tools for monitoring “sedimentation” in coral reef environments. In much of the literature where sediment traps were used to measure the effects of “sedimentation” on corals, it is clear from deployment descriptions and interpretations of the resulting data that information derived from sediment traps has frequently been misinterpreted or misapplied. Despite their widespread use in this setting, sediment traps do not provide quantitative information about “sedimentation” on coral surfaces. Traps can provide useful information about the relative magnitude of sediment dynamics if trap deployment standards are used. This conclusion is based first on a brief review of the state of knowledge of sediment trap dynamics, which has primarily focused on traps deployed high above the seabed in relatively deep water, followed by our understanding of near-bed sediment dynamics in shallow-water environments that characterize coral reefs. This overview is followed by the first synthesis of near-bed sediment trap data collected with concurrent hydrodynamic information in coral reef environments. This collective information is utilized to develop nine protocols for using sediment traps in coral reef environments, which focus on trap parameters that researchers can control such as trap height (H), trap mouth diameter (D), the height of the trap mouth above the substrate (z o ), and the spacing between traps. The hydrodynamic behavior of sediment traps and the limitations of data derived from these traps should be forefront when interpreting sediment trap data to infer sediment transport processes in coral reef environments.</p> <div class="credits"> <p class="dwt_author">Storlazzi, C.D.; Field, M.E.; Bothner, Michael H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-01-01</p> </div> </div> </div> </div> <div id="filter_results_form" class="filter_results_form floatContainer" style="visibility: visible;"> <div style="width:100%" id="PaginatedNavigation" class="paginatedNavigationElement"> <a id="FirstPageLink" onclick='return showDiv("page_1");' href="#" title="First Page"> <img id="FirstPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.first.18x20.png" alt="First Page" /></a> <a id="PreviousPageLink" onclick='return showDiv("page_19");' href="#" title="Previous Page"> <img id="PreviousPageLinkImage" class="Icon" 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<a onClick='return showDiv("page_6");' href="#">6</a> <a onClick='return showDiv("page_7");' href="#">7</a> <a onClick='return showDiv("page_8");' href="#">8</a> <a onClick='return showDiv("page_9");' href="#">9</a> <a onClick='return showDiv("page_10");' href="#">10</a> <a onClick='return showDiv("page_11");' href="#">11</a> <a onClick='return showDiv("page_12");' href="#">12</a> <a onClick='return showDiv("page_13");' href="#">13</a> <a onClick='return showDiv("page_14");' href="#">14</a> <a onClick='return showDiv("page_15");' href="#">15</a> <a onClick='return showDiv("page_16");' href="#">16</a> <a onClick='return showDiv("page_17");' href="#">17</a> <a onClick='return showDiv("page_18");' href="#">18</a> <a onClick='return showDiv("page_19");' href="#">19</a> <a onClick='return showDiv("page_20");' href="#">20</a> <a style="font-weight: bold;">21</a> <a onClick='return showDiv("page_22");' href="#">22</a> <a onClick='return showDiv("page_23");' href="#">23</a> <a onClick='return showDiv("page_24");' href="#">24</a> <a onClick='return showDiv("page_25");' href="#">25</a> </span> </span> <a id="NextPageLink" onclick='return showDiv("page_22");' href="#" title="Next Page"> <img id="NextPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.next.18x20.png" alt="Next Page" /></a> <a id="LastPageLink" onclick='return showDiv("page_25.0");' href="#" title="Last Page"> <img id="LastPageLinkImage" class="Icon" src="http://www.science.gov/scigov/images/icon.last.18x20.png" alt="Last Page" /></a> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">401</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://labs.mcb.harvard.edu/Cluzel/documents/Cluzel%20et%20al.%20Science%201996.pdf"> <span id="translatedtitle">Our <span class="hlt">observations</span> <span class="hlt">suggest</span> that ice shelves close to the climatic limit for existence may</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.osti.gov/eprints/">E-print Network</a></p> <p class="result-summary">). Mass balance for an entire glacier or ice shelf represents the overall change in mass. 19. The specific disintegrate rapidly. During the next years, increased attention should be paid to the section of the LIS south station near the Chilean Antarctic Base O'Higgins, operating on a campaign basis. The northern LIS</p> <div class="credits"> <p class="dwt_author">Cluzel, Philippe</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">402</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://pubs.er.usgs.gov/publication/70010737"> <span id="translatedtitle">Composition and evolution of the continental crust as <span class="hlt">suggested</span> by seismic <span class="hlt">observations</span></span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://pubs.er.usgs.gov/pubs/index.jsp?view=adv">USGS Publications Warehouse</a></p> <p class="result-summary">The average composition of the continental crust is more mafic than hitherto supposed. The conterminous United States can be divided, on the basis of seismic structure, into ten regions. The seven western and the three eastern regions can be termed western and eastern superprovinces. Seismic studies show that the crust is thinner and more silicic in tectonically active regions (western superprovince - average crustal thickness 34 km), than in stable regions (eastern superprovince - average crustal thickness 44 km). Mafic rocks are estimated to average 55% of the continental crust: 45% in the western and 59% in the eastern superprovince. These results express quantitatively the ideas expressed qualitatively by Pakiser and Zietz (1965). The computations of percentages of major oxides in the crust associate seismic velocities with rock compositions. ?? 1956.</p> <div class="credits"> <p class="dwt_author">Pakiser, L.C.; Robinson, R.</p> <p class="dwt_publisher"></p> <p class="publishDate">1966-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">403</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2011CorRe..30...23S"> <span id="translatedtitle">The use (and misuse) of sediment traps in coral reef environments: theory, <span class="hlt">observations</span>, and <span class="hlt">suggested</span> protocols</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary">Sediment traps are commonly used as standard tools for monitoring "sedimentation" in coral reef environments. In much of the literature where sediment traps were used to measure the effects of "sedimentation" on corals, it is clear from deployment descriptions and interpretations of the resulting data that information derived from sediment traps has frequently been misinterpreted or misapplied. Despite their widespread use in this setting, sediment traps do not provide quantitative information about "sedimentation" on coral surfaces. Traps can provide useful information about the relative magnitude of sediment dynamics if trap deployment standards are used. This conclusion is based first on a brief review of the state of knowledge of sediment trap dynamics, which has primarily focused on traps deployed high above the seabed in relatively deep water, followed by our understanding of near-bed sediment dynamics in shallow-water environments that characterize coral reefs. This overview is followed by the first synthesis of near-bed sediment trap data collected with concurrent hydrodynamic information in coral reef environments. This collective information is utilized to develop nine protocols for using sediment traps in coral reef environments, which focus on trap parameters that researchers can control such as trap height ( H), trap mouth diameter ( D), the height of the trap mouth above the substrate ( z o ), and the spacing between traps. The hydrodynamic behavior of sediment traps and the limitations of data derived from these traps should be forefront when interpreting sediment trap data to infer sediment transport processes in coral reef environments.</p> <div class="credits"> <p class="dwt_author">Storlazzi, C. D.; Field, M. E.; Bothner, M. H.</p> <p class="dwt_publisher"></p> <p class="publishDate">2011-03-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">404</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://www.dartmouth.edu/~chemlab/info/resources/p_table/Periodic.html"> <span id="translatedtitle"><span class="hlt">Periodic</span> table(3)</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">This site not only provides a clickable-by-element resource for quickly finding physical properties of the elements (up to 109), but also provides students with puzzles to hone their ability to identify and place elements in their respective place in the <span class="hlt">periodic</span> chart. Very useful for early learning of <span class="hlt">periodic</span> placements.</p> <div class="credits"> <p class="dwt_author">Brian P. Reid</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">405</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://learningcenter.nsta.org/product_detail.aspx?id=10.2505/4/ss04_027_04_32"> <span id="translatedtitle">Science Sampler: <span class="hlt">Periodic</span> Table</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">Teaching the <span class="hlt">periodic</span> table can be a mundane task filled with repetition and rote memorization. The techniques for engaging activities outlined in this article will help students become familiar with the <span class="hlt">periodic</span> table in fun and exciting ways through mediums such as games, silly stories, jokes, puzzles, and songs.</p> <div class="credits"> <p class="dwt_author">Pamela Galus</p> <p class="dwt_publisher"></p> <p class="publishDate">2004-01-01</p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">406</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://eric.ed.gov/?q=Periodic+AND+table&id=EJ721572"> <span id="translatedtitle">The Living <span class="hlt">Periodic</span> Table</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://www.eric.ed.gov/ERICWebPortal/search/extended.jsp?_pageLabel=advanced">ERIC Educational Resources Information Center</a></p> <p class="result-summary">To help make the abstract world of chemistry more concrete eighth-grade students, the author has them create a living <span class="hlt">periodic</span> table that can be displayed in the classroom or hallway. This display includes information about the elements arranged in the traditional <span class="hlt">periodic</span> table format, but also includes visual real-world representations of the…</p> <div class="credits"> <p class="dwt_author">Nahlik, Mary Schrodt</p> <p class="dwt_publisher"></p> <p class="publishDate">2005-01-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">407</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://dwb.unl.edu/Teacher/NSF/C04/C04Links/chemlab.pc.maricopa.edu/periodic/periodic.html"> <span id="translatedtitle">The Pictorial <span class="hlt">Periodic</span> Table</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://nsdl.org/nsdl_dds/services/ddsws1-1/service_explorer.jsp">NSDL National Science Digital Library</a></p> <p class="result-summary">This online <span class="hlt">periodic</span> table of the elements is a fabulous find for students of chemistry. On the main page, a clickable <span class="hlt">periodic</span> table allows users to choose an element and then view a page listing that element's electron configuration, atomic weight and number, isotopes and product elements, and a number of other physical properties such as ionization potential and boiling and melting points. Each entry is extremely thorough and contains links to related elements. The Pictorial <span class="hlt">Periodic</span> Table is also easily searchable by atomic and covalent radius, density, boiling and melting point, electronegativity, ionization potential, heat properties, and atomic weight or number. In addition, users can perform keyword searches. Graphs and tables of element properties, alternative styles of <span class="hlt">periodic</span> table (e.g., spiral, pyramid), a special page on isotopic properties, a printable table, and links to other <span class="hlt">periodic</span> table pages are among the wealth of information provided. The site is provided by the Chemlab server of Phoenix College, AZ.</p> <div class="credits"> <p class="dwt_author">Heilman, Chris.</p> <p class="dwt_publisher"></p> <p class="publishDate"></p> </div> </div> </div> </div> <div class="floatContainer result " lang="en"> <div class="resultNumber element">408</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/scigov/link.html?type=RESULT&redirectUrl=http://adsabs.harvard.edu/abs/2014AAS...22440202V"> <span id="translatedtitle"><span class="hlt">Periodic</span> Density Structures and the Source of the Slow Solar Wind</span></a>  </p> <div class="result-meta"> <p class="source"><a target="_blank" id="logoLink" href="http://adsabs.harvard.edu/abstract_service.html">NASA Astrophysics Data System (ADS)</a></p> <p class="result-summary"><span class="hlt">Periodic</span> density structures with length-scales of hundreds to several thousands of megameters, and frequencies of tens to hundreds of minutes, are <span class="hlt">observed</span> regularly in the solar wind at 1 AU. These structures coexist with, but are not due to, fluctuations in the plasma resulting from the turbulent cascade. Two lines of evidence <span class="hlt">suggest</span> that <span class="hlt">periodic</span> density structures are formed in the solar corona as part of the slow solar wind release and/or acceleration processes. The first is the identification of corresponding changes in compositional data in situ, and the other is the identification of <span class="hlt">periodic</span> density structures in the inner Heliospheric Imaging data onboard the STEREO/SECCHI suite. In this presentation, we show the results of tracking <span class="hlt">periodic</span> structures identified in the SECCHI/Hi1 images down through the corresponding SECCHI/Cor2 images. We demonstrate that the <span class="hlt">periodic</span> density structures are formed around or below 2.5 Rs - the inner edge of the Cor2 field of view. Further, we compute the occurrence rate of <span class="hlt">periodic</span> density structures in 10 days of Cor2 images as a function of location in the solar corona. We find that <span class="hlt">periodic</span> density structures do not occur throughout the entire space-filling volume of the solar wind; rather, there are particular places where they occur preferentially, <span class="hlt">suggesting</span> source locations for <span class="hlt">periodic</span> density structures in the slow solar wind.</p> <div class="credits"> <p class="dwt_author">Viall, Nicholeen; Vourlidas, Angelos</p> <p class="dwt_publisher"></p> <p class="publishDate">2014-06-01</p> </div> </div> </div> </div> <div class="floatContainer result odd" lang="en"> <div class="resultNumber element">409</div> <div class="resultBody element"> <p class="result-title"><a target="resultTitleLink" href="http://science.gov/sci