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Sample records for pks b1545-321 bow

  1. Bowed Strings

    NASA Astrophysics Data System (ADS)

    Rossing, Thomas D.; Hanson, Roger J.

    In the next eight chapters, we consider some aspects of the science of bowed string instruments, old and new. In this chapter, we present a brief discussion of bowed strings, a subject that will be developed much more thoroughly in Chap. 16. Chapters 13-15 discuss the violin, the cello, and the double bass. Chapter 17 discusses viols and other historic string instruments, and Chap. 18 discusses the Hutchins-Schelleng violin octet.

  2. Violin bow vibrations.

    PubMed

    Gough, Colin E

    2012-05-01

    The modal frequencies and bending mode shapes of a freely supported tapered violin bow are investigated by finite element analysis and direct measurement, with and without tensioned bow hair. Such computations are used with analytic models to model the admittance presented to the stretched bow hairs at the ends of the bow and to the string at the point of contact with the bow. Finite element computations are also used to demonstrate the influence of the lowest stick mode vibrations on the low frequency bouncing modes, when the hand-held bow is pressed against the string. The possible influence of the dynamic stick modes on the sound of the bowed instrument is briefly discussed.

  3. The Modern Compound Bow.

    PubMed

    Sung, LokMan; Kesha, Kilak; Avedschmidt, Sarah; Root, Kelly; Hlavaty, Leigh

    2017-06-12

    Bows and arrows are ancient weapons that have risen and fallen as the preeminent armaments used by man. Because of the ubiquity of firearms, fatalities from archery injuries in the United States have radically declined. However, when deaths involving this weapon do present themselves, the paucity of reference materials can be a hurdle for forensic pathologists and other forensic scientists. This article will provide a brief history of the origins of the bow and the inception of the compound bow. Comparing and contrasting the structures comprising a traditional bow to those of the modern compound bow will provide insight into how these components function in unison to propel arrows. © 2017 American Academy of Forensic Sciences.

  4. Bow and arrow dynamics

    NASA Astrophysics Data System (ADS)

    Marlow, W. C.

    1981-04-01

    Past analyses of bow and arrow dynamics have assumed the string to be inextensible. This results in predictions of efficiencies that are significantly higher than measured values (efficiencies over 90% are predicted versus 70% to 85% for measurements, circa 1960). The present analysis allows for an elastic string. It is found that arrow exit then takes place when the string and bow limbs still have substantial kinetic energy, and therefore this energy is unavailable for kinetic energy of the arrow. Moreover, the potential energy remaining in the string and bow limb system can also reduce the amount of energy available for the arrow. For the Hickman model of a long bow used in this study, the elastic string prediction of efficiency is 78%, whereas the inelastic prediction is 92%. The analysis utilizes a Lagrangian distributed mass formulation to develop the governing equations of motion and to generate an equivalent point mass model. The equations of motion were numerically integrated to obtain efficiency, arrow velocity, virtual masses, string tension, string extension, arrow exit time, string and limb potential energies, system momentum, and the dynamic force required to hold the bow handle stationary. Estimates of the effect of air resistance were made and found to be less than 2% of the total system energy. The vibratory dynamics of the string and bow limbs subsequent to arrow exit was analyzed. The results of the elastic string considerations are in reasonable agreement with experimental data and negate the usual explanation for the long-standing discrepancy between theory and experiment as due to air resistance and hysteresis losses in the string and bow limbs.

  5. 43. Bow thruster room. Bow thruster engine not used for ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    43. Bow thruster room. Bow thruster engine not used for powering hydraulics to boom as in some other tenders in same class. - U.S. Coast Guard Cutter BRAMBLE, Waterfront at Lincoln Avenue, Port Huron, St. Clair County, MI

  6. Neptune inbound bow shock

    NASA Technical Reports Server (NTRS)

    Szabo, Adam; Lepping, Ronald P.

    1995-01-01

    Voyager 2 crossed the inbound or upstream Neptunian bow shock at 1430 spacecraft event time on August 24 in 1989 (Belcher et al., 1989). The plasma and magnetic field measurements allow us to study the solar wind interaction with the outermost gas giant. To fully utilize all of the spacecraft observations, an improved nonlinear least squares, 'Rankine-Hugoniot' magnetohydrodynamic shock-fitting technique has been developed (Szabo, 1994). This technique is applied to the Neptunian data set. We find that the upstream bow shock normal points nearly exactly toward the Sun consistent with any reasonable large-scale model of the bow shock for a near subsolar crossing. The shock was moving outward with a speed of 14 +/- 12 km/s. The shock can be characterized as a low beta, high Mach number, strong quasi-perpendicular shock. Finally, the shock microstructure features are resolved and found to scale well with theoretical expectations.

  7. Bow Shocks in Space

    NASA Image and Video Library

    2016-01-05

    Bow shocks thought to mark the paths of massive, speeding stars are highlighted in these images from NASA's Spitzer Space Telescope and Wide-field Infrared Survey Explorer, or WISE. Cosmic bow shocks occur when massive stars zip through space, pushing material ahead of them in the same way that water piles up in front of a race boat. The stars also produce high-speed winds that smack into this compressed material. The end result is pile-up of heated material that glows in infrared light. In these images, infrared light has been assigned the colored red. Green shows wispy dust in the region and blue shows stars. The two images at left are from Spitzer, and the one on the right is from WISE. The speeding stars thought to be creating the bow shocks can be seen at the center of each arc-shaped feature. The image at right actually consists of two bow shocks and two speeding stars. All the speeding stars are massive, ranging from about 8 to 30 times the mass of our sun. http://photojournal.jpl.nasa.gov/catalog/PIA20062

  8. Bow shock: Power aspects

    NASA Astrophysics Data System (ADS)

    Sedykh, P. A.

    2014-07-01

    It is clear that the primary energy source for magnetospheric processes is the solar wind, but the process of energy transfer from the solar wind into the magnetosphere, or rather, to convecting magnetospheric plasma, appears to be rather complicated. Bow shock is a powerful transformer of the solar wind kinetic energy into the gas dynamic and electromagnetic energy. A jump of the magnetic field tangential component at front crossing means that the front carries an electric current. The solar wind kinetic energy partly transforms to gas kinetic and electromagnetic energy during its passage through the bow shock front. The transition layer (magnetosheath) can use part of this energy for accelerating of plasma, but can conversely spend part its kinetic energy on the electric power generation, which afterwards may be used by the magnetosphere. Thereby, transition layer can be both consumer (sink) and generator (source) of electric power depending upon special conditions. The direction of the current behind the bow shock front depends on the sign of the IMF Bz-component. It is this electric current which sets convection of plasma in motion.

  9. Martian bow shock - Phobos observations

    NASA Technical Reports Server (NTRS)

    Schwingenschuh, K.; Riedler, W.; Lichtenegger, H.; Eroshenko, E.; Sauer, K.

    1990-01-01

    Data obtained with the Magma magnetometer on the subsolar passes of the Phobos spacecraft during its 3 elliptic orbits reveals a turbulent bow shock with a strong foot consistent with the reflection of solar wind protons. The bow shock lies at a subsolar distance of 1.47 + or - .03 R(M). The circular orbit phase of the mission reveals a bow shock with a highly varying location. The median terminator crossing lies at 2.72 Mars radii. The location of the bow shock in the terminator plane is sensitive to neither the EUV flux nor to planetary longitude.

  10. Martian bow shock: Phobos observations

    SciTech Connect

    Schwingenschuh, K.; Riedler, W.; Lichtenegger, H. ); Yeroshenko, Ye. ); Sauer, K. ); Luhmann, J.G.; Ong, M.; Russell, C.T. )

    1990-05-01

    Data obtained with the MAGMA magnetometer on the subsolar passes of the Phobos spacecraft during its 3 elliptic orbits reveals a turbulent bow shock with a strong foot consistent with the reflection of solar wind protons. The bow shock lies at a subsolar distance of 1.47 {plus minus} .03 R{sub M}. The circular orbit phase of the mission reveals a bow shock with a highly varying location. The median terminator crossing lies at 2.72 Mars radii. The location of the bow shock in the terminator plane is sensitive to neither the EUV flux nor to planetary longitude.

  11. Martian bow shock - PHOBOS observations

    NASA Astrophysics Data System (ADS)

    Schwingenschuh, K.; Riedler, W.; Lichtenegger, H.; Yeroshenko, Ye.; Sauer, K.; Luhmann, J. G.; Ong, M.; Russell, C. T.

    1990-05-01

    Data obtained with the Magma magnetometer on the subsolar passes of the Phobos spacecraft during its 3 elliptic orbits reveals a turbulent bow shock with a strong foot consistent with the reflection of solar wind protons. The bow shock lies at a subsolar distance of 1.47 + or - .03 R(M). The circular orbit phase of the mission reveals a bow shock with a highly varying location. The median terminator crossing lies at 2.72 Mars radii. The location of the bow shock in the terminator plane is sensitive to neither the EUV flux nor to planetary longitude.

  12. AOTV bow shock location

    NASA Technical Reports Server (NTRS)

    Desautel, D.

    1985-01-01

    Hypersonic bow-shock location and geometry are of central importance to the aerodynamics and aerothermodynamics of aeroassisted orbital transfer vehicles (AOTVs), but they are difficult to predict for a given vehicle configuration. This paper reports experimental measurements of shock standoff distance for the 70 deg cone AOTV configuration in shock-tunnel-test flows at Mach numbers of 3.8 to 7.9 and for angles of attack from 0 deg to 20 deg. The controlling parameter for hypersonic bow-shock standoff distance (for a given forebody shape) is the mean normal-shock density ratio. Values for this parameter in the tests reported are in the same range as those of the drag-brake AOTV perigee regime. Results for standoff distance are compared with those previously reported in the literature for this AOTV configuration. It is concluded that the AOTV shock standoff distance for the conical configuration, based on frustrum (base) radius, is equivalent to that of a sphere with a radius about 35 percent greater than that of the cone; the distance is, therefore, much less than reported in previous studies. Some reasons for the discrepancies between the present and previous are advanced. The smaller standoff distance determined here implies there will be less radiative heat transfer than was previously expected.

  13. NRPS-PKS: a knowledge-based resource for analysis of NRPS/PKS megasynthases.

    PubMed

    Ansari, Mohd Zeeshan; Yadav, Gitanjali; Gokhale, Rajesh S; Mohanty, Debasisa

    2004-07-01

    NRPS-PKS is web-based software for analysing large multi-enzymatic, multi-domain megasynthases that are involved in the biosynthesis of pharmaceutically important natural products such as cyclosporin, rifamycin and erythromycin. NRPS-PKS has been developed based on a comprehensive analysis of the sequence and structural features of several experimentally characterized biosynthetic gene clusters. The results of these analyses have been organized as four integrated searchable databases for elucidating domain organization and substrate specificity of nonribosomal peptide synthetases and three types of polyketide synthases. These databases work as the backend of NRPS-PKS and provide the knowledge base for predicting domain organization and substrate specificity of uncharacterized NRPS/PKS clusters. Benchmarking on a large set of biosynthetic gene clusters has demonstrated that, apart from correct identification of NRPS and PKS domains, NRPS-PKS can also predict specificities of adenylation and acyltransferase domains with reasonably high accuracy. These features of NRPS-PKS make it a valuable resource for identification of natural products biosynthesized by NRPS/PKS gene clusters found in newly sequenced genomes. The training and test sets of gene clusters included in NRPS-PKS correlate information on 307 open reading frames, 2223 functional protein domains, 68 starter/extender precursors and their specific recognition motifs, and also the chemical structure of 101 natural products from four different families. NRPS-PKS is a unique resource which provides a user-friendly interface for correlating chemical structures of natural products with the domains and modules in the corresponding nonribosomal peptide synthetases or polyketide synthases. It also provides guidelines for domain/module swapping as well as site-directed mutagenesis experiments to engineer biosynthesis of novel natural products. NRPS-PKS can be accessed at http://www.nii.res.in/nrps-pks.html.

  14. VLBI Observations of Southern EGRET Identifications. 1; PKS 0208-512, PKS 0521-365 and PKS 0537-441

    NASA Technical Reports Server (NTRS)

    Tingay, S. J.; Edwards, P. G.; Costa, M. E.; Lovell, J. E. J.; McCulloch, P. M.; Jauncey, D. L.; Reynolds, J. E.; Tzioumis, A. K.; Migenes, V.; Gough, R.

    1996-01-01

    We present high-resolution very long baseline interferometry images of three southern radio sources that the Energetic Gamma-Ray Experiment Telescope (EGRET), on board the Compton Gamma Ray Observatory, has identified as greater than 100 MeV gamma-ray sources. These are the first results in a continuing program of VLBI observations of southern EGRET identifications. For two of these sources, PKS 0208-512 (at 4.851 GHz) and PKS 0537-441 (at 4.851 and 8.418 GHz), the images represent first-epoch observations. For the remaining lower redshift object, PKS 0521-365, we present images from three epochs at 4.851 GHz and an image from one further epoch at 8.418 GHz, spanning approximately 1 yr. We discuss the need for further extensive VLBI observations of EGRET-identified radio sources.

  15. Magnetic Fields and Bow Shocks Illustration

    NASA Image and Video Library

    2013-02-19

    This illustration shows quasi-parallel top and quasi-perpendicular bottom magnetic field conditions at a planetary bow shock. Bow shocks are shockwaves created when the solar wind blows on a planet magnetic field.

  16. The player and the bowed string: coordination of bowing parameters in violin and viola performance.

    PubMed

    Schoonderwaldt, E

    2009-11-01

    An experiment was conducted with four violin and viola players, measuring their bowing performance using an optical motion capture system and sensors on the bow. The measurements allowed for a detailed analysis of the use and coordination of the main bowing parameters bow velocity, bow force, and bow-bridge distance. An analysis of bowing strategies in detache playing of notes of three durations (0.2, 2, and 4 s) at three dynamic levels (pp, mf, and f) on all four strings is presented, focusing on the "steady" part of the notes. The results revealed clear trends in the coordinated variations of the bowing parameters depending on the constraints of the task, reflecting a common behavior as well as individual strategies. Furthermore, there were clear indications that the players adapted the bowing parameters to the physical properties of the string and the instrument, respecting the limits of the playable control parameter space.

  17. Orion Nebula and Bow Shock

    NASA Technical Reports Server (NTRS)

    1999-01-01

    Astronomers using NASA's Hubble Space Telescope have found a bow shock around a very young star in the nearby Orion nebula, an intense star-forming region of gas and dust.

    A picture, from the Hubble Heritage team, is available at http://heritage.stsci.edu or http://oposite.stsci.edu/pubinfo/pr/2002/05 or http://www.jpl.nasa.gov/images/wfpc . It was taken in February 1995 as part of the Hubble Orion Nebula mosaic by Hubble's Wide Field and Planetary Camera 2, designed and built by NASA's Jet Propulsion Laboratory, Pasadena, Calif.

    Named for the crescent-shaped wave a ship makes as it moves through water, a bow shock can form in space when two gas streams collide. In this case, the young star, LL Ori, emits a vigorous wind, a stream of charged particles moving rapidly outward from the star. Our own Sun has a less energetic version of this wind that is responsible for auroral displays on the Earth.

    The material spewed from LL Ori collides with slow-moving gas evaporating away from the center of the Orion nebula, located to the lower right of the image. The surface where the two winds collide is seen as the crescent-shaped bow shock.

    Unlike a water wave from a ship, this interstellar bow shock is three-dimensional. The filamentary emission has a distinct boundary on the side facing away from LL Ori, but is diffuse on the side closest to the star, a trait common to many bow shocks.

    A second, fainter bow shock can be seen around a star near the upper right-hand corner of the image. Astronomers have identified numerous shock fronts in this complex star-forming region and are using this data to understand the complex phenomena associated with star birth.

    The Orion nebula is a close neighbor in our Milky Way galaxy, at only 1,500 light-years from Earth. The filters used in this color composite represent oxygen, nitrogen, and hydrogen emissions.

  18. Articulated coordination of the right arm underlies control of bow parameters and quick bow reversals in skilled cello bowing

    PubMed Central

    Verrel, Julius; Woollacott, Marjorie; Lindenberger, Ulman

    2014-01-01

    Stringed instrument bowing is a complex coordinative motor skill acquired though years of intense practice. We apply a novel “freezing” analysis to investigate how movement at different joints contributes to bow transport (movement amplitude), stabilization of bow parameters (angle, velocity) during bow movements, and quick reversals of bow direction (acceleration amplitude). Participants were ten advanced or professional cellists (19–32 years, at least 10 years of practice) and ten age-matched novice players. Arm and bow movements were recorded using 3D motion capture. To assess how performance depends on articulated use of the right arm, actual data were compared to surrogate data, generated by artificially removing movement at (“freezing”) individual joints in measured arm movements. This analysis showed that both elbow and shoulder significantly contribute to bow transport in experts, while only the shoulder contributed to bow transport in novices. Moreover, experts showed more strongly increased variability of bow parameters and reduced acceleration amplitudes at bow reversals for surrogate compared to actual movement data. This indicates that movement across joints was organized to reduce bow variability and achieve quick bow reversals. Corresponding effects were less pronounced or absent in the novices, in particular for the wrist and elbow. Our results demonstrate the importance of articulated use of the right arm and clarify the contribution of different joints in experts’ bowing performance. Moreover, they support theories of motor control and learning that propose exploitation of biomechanical degrees of freedom, in particular of distal joints, as a critical component in skilled motor performance. PMID:25191284

  19. [Homicide by bow and arrow].

    PubMed

    Germerott, Tanja; Jänisch, Stefanie; Tröger, Hans Dieter; Günther, Detlef

    2010-01-01

    Since the invention of firearms, arrow wounds represent a rarity in the daily routine of forensic pathologists. In the present paper, we describe a homicide by a broadhead arrow shot from a compound bow in a domestic environment. Based on this homicide, we discuss the characteristics of the lesion caused by broadhead arrows and field-tip arrows. We look critically at the free saleability of this equipment mostly used for sport shooting in Germany.

  20. Effects of bowing on perception of attractiveness.

    PubMed

    Osugi, Takayuki; Kawahara, Jun I

    2015-07-01

    Bowing is a greeting behavior. The present study examined the modulation effect of bowing on perception of attractiveness. In each trial, a portrait digitized from university yearbooks was presented on a computer screen. The portrait was mildly tilted toward participants to simulate a greeting bow (25-degree angle). Participants evaluated the subjective attractiveness of the face using a visual analog scale (0-100). The mean attractiveness judgment of the bowing portrait was significantly higher relative to that of the bending-backward or standing-still control conditions (Experiment 1). Additional control experiments revealed that alternative accounts relying on apparent spatial proximity and physical characteristics could not solely explain the effect of bowing (Experiment 2) and indicated that the effect was specific to objects perceived as faces (Experiment 3). Furthermore, observers' in-return bowing behavior did not reduce the bowing effect (Experiment 4), and bowing motion increased the ratings of subjective politeness and submissiveness (Experiment 5). Finally, tilting the 3D faces elicited the same effect from observers as did tilting the still photos (Experiment 6). These results suggest that a tilting motion of portraits (or images of face-like objects) mimicking bowing enhances perceived attractiveness, at least as measured in a culture familiar with greeting by bowing.

  1. Insect-specific polyketide synthases (PKSs), potential PKS-nonribosomal peptide synthetase hybrids, and novel PKS clades in tropical fungi.

    PubMed

    Amnuaykanjanasin, Alongkorn; Phonghanpot, Suranat; Sengpanich, Nattapong; Cheevadhanarak, Supapon; Tanticharoen, Morakot

    2009-06-01

    Polyketides draw much attention because of their potential use in pharmaceutical and biotechnological applications. This study identifies an abundant pool of polyketide synthase (PKS) genes from local isolates of tropical fungi found in Thailand in three different ecological niches: insect pathogens, marine inhabitants, and lichen mutualists. We detected 149 PKS genes from 48 fungi using PCR with PKS-specific degenerate primers. We identified and classified 283 additional PKS genes from 13 fungal genomes. Phylogenetic analysis of all these PKS sequences the comprising ketosynthase (KS) conserved region and the KS-acyltransferase interdomain region yielded results very similar to those for phylogenies of the KS domain and suggested a number of remarkable points. (i) Twelve PKS genes amplified from 12 different insect-pathogenic fungi form a tight cluster, although along with two PKS genes extracted from genomes of Aspergillus niger and Aspergillus terreus, in reducing clade III. Some of these insect-specific fungal PKSs are nearly identical. (ii) We identified 38 new PKS-nonribosomal peptide synthetase hybrid genes in reducing clade II. (iii) Four distinct clades were discovered with more than 75% bootstrap support. We propose to designate the novel clade D1 with 100% bootstrap support "reducing clade V." The newly cloned PKS genes from these tropical fungi should provide useful and diverse genetic resources for future research on the characterization of polyketide compounds synthesized by these enzymes.

  2. The violin bow: taper, camber and flexibility.

    PubMed

    Gough, Colin

    2011-12-01

    An analytic, small-deflection, simplified model of the modern violin bow is introduced to describe the bending profiles and related strengths of an initially straight, uniform cross-section, stick as a function of bow hair tension. A number of illustrative bending profiles (cambers) of the bow are considered, which demonstrate the strong dependence of the flexibility of the bow on longitudinal forces across the ends of the bent stick. Such forces are shown to be comparable in strength to critical buckling loads causing excessive sideways buckling unless the stick is very straight. Non-linear, large deformation, finite element computations extend the analysis to bow hair tensions comparable with and above the critical buckling strength of the straight stick. The geometric model assumes an expression for the taper of Tourte bows introduced by Vuillaume, which is re-examined and generalized to describe violin, viola and cello bows. A comparison is made with recently published measurements of the taper and bending profiles of a particularly fine bow by Kittel.

  3. Entropy Generation Across Earth's Bow Shock

    NASA Technical Reports Server (NTRS)

    Parks, George K.; McCarthy, Michael; Fu, Suiyan; Lee E. s; Cao, Jinbin; Goldstein, Melvyn L.; Canu, Patrick; Dandouras, Iannis S.; Reme, Henri; Fazakerley, Andrew; Lin, Naiguo; Wilber, Mark

    2011-01-01

    Earth's bow shock is a transition layer that causes an irreversible change in the state of plasma that is stationary in time. Theories predict entropy increases across the bow shock but entropy has never been directly measured. Cluster and Double Star plasma experiments measure 3D plasma distributions upstream and downstream of the bow shock that allow calculation of Boltzmann's entropy function H and his famous H-theorem, dH/dt O. We present the first direct measurements of entropy density changes across Earth's bow shock. We will show that this entropy generation may be part of the processes that produce the non-thermal plasma distributions is consistent with a kinetic entropy flux model derived from the collisionless Boltzmann equation, giving strong support that solar wind's total entropy across the bow shock remains unchanged. As far as we know, our results are not explained by any existing shock models and should be of interests to theorists.

  4. The supernumerary bows of the rainbow

    NASA Astrophysics Data System (ADS)

    Adams, Peter; Ricard, Jean; Barckicke, Jean

    2016-04-01

    Everyone appreciate the mysterious beauty of a Rainbow picture. The primary bow shows red on the outer part and violet on the inner side. It is caused by light being refracted when entering a droplet of water, then reflected inside on the back of the droplet and refracted again when leaving it. The secondaty bow is seen outside the primary arc, and has the order of its colours reversed, with red on the inner side of the arc. The supernumerary bows are alternating faint bows on the inner side of the primary rainbow (and also outside the secondary rainbow). In this presentation, we will describe the present knowledge and the future perspectives A fully funded PhD Scholarship on this topic is open at the University of Granada. Picture = Contrast-enhanced photograph of a primary bow picture (prepared by Andrew Dunn).

  5. Accuracy of an earpiece face-bow.

    PubMed

    Palik, J F; Nelson, D R; White, J T

    1985-06-01

    The validity of the Hanau ear-bow to transfer an arbitrary hinge axis to a Hanau articulator was clinically compared with a Hanau kinematic face-bow. The study was conducted with 18 randomly selected patients. This investigation demonstrated a significant statistical difference between the arbitrary axis located with an ear-bow and the terminal hinge axis. This discrepancy was significant in the anteroposterior direction but not in the superior-inferior direction. Only 50% of the arbitrary hinge axes were within a 5 mm radius of the terminal hinge axis, while 89% were within a 6 mm radius. Furthermore, the ear-bow method was not repeatable statistically. Additional study is needed to determine the practical value of the arbitrary face-bow and to pursue modifications to improve its accuracy.

  6. Engineering of the spinosyn PKS: directing starter unit incorporation.

    PubMed

    Sheehan, Lesley S; Lill, Rachel E; Wilkinson, Barrie; Sheridan, Rose M; Vousden, William A; Kaja, Andrew L; Crouse, Gary D; Gifford, James; Graupner, Paul R; Karr, Laura; Lewer, Paul; Sparks, Thomas C; Leadlay, Peter F; Waldron, Clive; Martin, Christine J

    2006-12-01

    The spinosyns are a family of potent and highly selective insect control agents that display a favorable environmental profile. As some regions of the spinosyn molecule are recalcitrant to chemical modification, a targeted genetic approach was carried out to generate new analogues. The polyketide synthase (PKS) loading modules from the avermectin PKS of Streptomyces avermitilis and the erythromcyin PKS of Saccharopolyspora erythraea were each used to replace the spinosyn PKS loading module. Both of the resulting strains containing hybrid PKS pathways produced the anticipated spinosyn analogues. Supplementation of the culture media with a range of exogenous carboxylic acids led to the successful incorporation of these novel elements to yield further novel spinosyn molecules, some of which demonstrated potent and new insecticidal activities. Furthermore, it has been demonstrated that semisynthesis of such novel metabolites can then be used to generate active analogues, demonstrating the effectiveness of utilizing these complementary methods to search the chemical space around this template.

  7. NIR Flare of PKS2032+107

    NASA Astrophysics Data System (ADS)

    Carrasco, L.; Miramon, J.; Recillas, E.; Porras, A.; Chabushyan, V.; Carraminana, A.; Mayya, D.

    2013-11-01

    We have observed a recent NIR flare of the intermediate redshift quasar PKS2032+107. This radio source is cross identified with the gamma ray source 2FGLJ2035.4+1058 and the optical source BZQJ2035+1056. From observations carried out on November 12th, 2013 (JD 2456608.603380), we determined the following photometric values H = 13.452 +/- 0.03, J = 14.628 +/- 0.03 and Ks = 12.777 +/- 0.05. Our previous NIR photometry of the object (JD2456595.644780) yielded the value: H = 15.012 =/- 0.05.

  8. Modeling nonthermal emission from stellar bow shocks

    NASA Astrophysics Data System (ADS)

    Pereira, V.; López-Santiago, J.; Miceli, M.; Bonito, R.; de Castro, E.

    2016-04-01

    Context. Runaway O- and early B-type stars passing through the interstellar medium at supersonic velocities and characterized by strong stellar winds may produce bow shocks that can serve as particle acceleration sites. Previous theoretical models predict the production of high-energy photons by nonthermal radiative processes, but their efficiency is still debated. Aims: We aim to test and explain the possibility of emission from the bow shocks formed by runaway stars traveling through the interstellar medium by using previous theoretical models. Methods: We applied our model to AE Aurigae, the first reported star with an X-ray detected bow shock, to BD+43 3654, in which the observations failed in detecting high-energy emission, and to the transition phase of a supergiant star in the late stages of its life. Results: From our analysis, we confirm that the X-ray emission from the bow shock produced by AE Aurigae can be explained by inverse Compton processes involving the infrared photons of the heated dust. We also predict low high-energy flux emission from the bow shock produced by BD+43 3654, and the possibility of high-energy emission from the bow shock formed by a supergiant star during the transition phase from blue to red supergiant. Conclusions: Bow shocks formed by different types of runaway stars are revealed as a new possible source of high-energy photons in our neighborhood.

  9. Viols and Other Historic Bowed String Instruments

    NASA Astrophysics Data System (ADS)

    Campbell, Murray; Campbell, Patsy

    While plucked strings have been used for musical purposes since at least the third millennium BCE, the idea of sounding a string by bowing it is a much more recent development. Bowed string instruments seem to have originated in Asia toward the end of the first millennium CE, and were in widespread use in Western Europe by the end of the eleventh century. For the next three centuries many different types of bowed instrument, with a bewildering variety of names, were in common use throughout Europe.

  10. 46 CFR 42.20-70 - Minimum bow height.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 2 2011-10-01 2011-10-01 false Minimum bow height. 42.20-70 Section 42.20-70 Shipping... Freeboards § 42.20-70 Minimum bow height. (a) The bow height defined as the vertical distance at the forward....68. (b) Where the bow height required in paragraph (a) of this section is obtained by sheer, the...

  11. 46 CFR 42.20-70 - Minimum bow height.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 2 2010-10-01 2010-10-01 false Minimum bow height. 42.20-70 Section 42.20-70 Shipping... Freeboards § 42.20-70 Minimum bow height. (a) The bow height defined as the vertical distance at the forward....68. (b) Where the bow height required in paragraph (a) of this section is obtained by sheer, the...

  12. Bow-shaped toroidal field coils

    SciTech Connect

    Bonanos, P.

    1981-05-01

    Design features of Bow-Shaped Toroidal Field Coils are described and compared with circular and D shaped coils. The results indicate that bow coils can produce higher field strengths, store more energy and be made demountable. The design offers the potential for the production of ultrahigh toroidal fields. Included are representative coil shapes and their engineering properties, a suggested structural design and an analysis of a specific case.

  13. Dielectric bow-tie nanocavity.

    PubMed

    Lu, Qijing; Shu, Fang-Jie; Zou, Chang-Ling

    2013-12-15

    We propose a novel dielectric bow-tie (DBT) nanocavity consisting of two opposing tip-to-tip triangle semiconductor nanowires, whose end faces are coated by silver nanofilms. Based on the advantages of the dielectric slot and tip structures, and the high reflectivity of the silver mirror, light can be confined in this nanocavity with low loss. We demonstrate that at 4.5 K (300 K) around the resonance wavelength of 1550 nm, the mode excited in this nanocavity has a deep subwavelength mode volume of 2.8×10(-4) μm³ and a high quality factor of 4.9×10(4) (401.3), corresponding to an ultrahigh Purcell factor of 1.6×10(7) (1.36×10(5)). This DBT nanocavity may find applications for integrated nanophotonic circuits, such as high-efficiency single photon sources, thresholdless nanolasers, and strong coupling in cavity quantum electrodynamics experiments.

  14. Interstellar Scattering and the Einstein Ring PKS 1830-211

    NASA Technical Reports Server (NTRS)

    Jones, D. L.; Preston, R. A.; Murphy, D. W.; Meier, D. L.; Jauncey, D. L.; Reynolds, J. E.; Tziomis, A. K.

    1995-01-01

    High frequency (22 GHz) data have been used two resolve two compact components of the strong gravitational lens PKS 1830-211. The two bright components are at opposite sides of a one arcsecond diameter Einstein ring.

  15. Bow-arrow interaction in archery.

    PubMed

    Kooi, B W

    1998-11-01

    A mathematical model of the flight of the arrow during its discharge from a bow was proposed by Pekalski (1990). His description of the model was incomplete. In this paper, I give a full description of the model. Furthermore, I propose some improvements that make his model more consistent with reality. One achievement is the modelling of contact of the arrow and grip; the pressure button is modelled as a unilateral elastic support. The acceleration force acting upon the arrow during the launch is predicted by an advanced mathematical model of bow dynamics. There is a satisfactory conformity of the simulation and experimental results. The new model predicts that the arrow leaves the pressure button before it leaves the string, as reported previously. The ability to model arrow dynamics can be used to improve the adjustment of the bow-arrow system for optimal performance.

  16. Suicide using a compound bow and arrow.

    PubMed

    Cina, S J; Radentz, S S; Smialek, J E

    1998-03-01

    Accidental, suicidal, and homicidal injuries have been caused by arrows fired from crossbows. To our knowledge, a case of suicide using a full-size compound bow to fire a projectile has not been reported in the English literature. Described is a case of a 17-year-old man who shot himself in the chest with a broadhead hunting arrow fired from a compound bow. Examination of the footwear suggests that the decedent drew the bowstring with his left foot while holding the bow in his hands. The mechanism of injury is discussed. When dealing with a longbow-related fatality, examination of the weaponry used and reenactment of the fatal methodology are critical in determining whether self-inflicted injury is a probability.

  17. A precursor to the Venus bow shock

    NASA Technical Reports Server (NTRS)

    Brace, L. H.; Theis, R. F.; Curtis, S. A.; Parker, L. W.

    1988-01-01

    This paper describes the observations by the Pioneer-Venus-Orbiter Langmuir probe of the low-density Venus bow shock precursor, i.e., a region of electron and ion-current enhancements just upstream from the Venus bow shock. It is suggested that the precursor signatures represent the effects of a small population of energetic ions in this region. Several possible planetary sources of these ions are considered. The paper also discusses the Langmuir probe measurement technique itself as it applies to the very low densities of the precursor.

  18. 1. View looking south on Montana Street. The Silver Bow ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    1. View looking south on Montana Street. The Silver Bow County Courthouse (1910-1912) is on the left. - Butte Historic District, Bounded by Copper, Arizona, Mercury & Continental Streets, Butte, Silver Bow County, MT

  19. 2. VIEW NORTH OF BOW OF JFK IN DRYDOCK NO. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    2. VIEW NORTH OF BOW OF JFK IN DRYDOCK NO. 5; NOTE BOW ANCHOR AT TOP CENTER. - Naval Base Philadelphia-Philadelphia Naval Shipyard, Dry Dock No. 5, League Island, Philadelphia, Philadelphia County, PA

  20. Butte-Silver Bow County Monthly Progress Reports

    EPA Pesticide Factsheets

    Last three monthly progress reports submitted by Butte-Silver Bow County on cleanup activities at the Silver Bow Creek/Butte Area Superfund Site, as required by the Butte Priority Soils UAO, Docket No. CERCLA 08-2011-0011.

  1. Tibial Bowing and Pseudarthrosis in Neurofibromatosis Type 1

    DTIC Science & Technology

    2012-04-01

    anterolateral bowing of the lower leg prior to fracture in neurofibromatosis type 1. J Pediatr Orthop 2009;29:385-92. 3. Stevenson DA, Yan J, He Y, Li H...neurofibromatosis type 1 (NF1), typically identified in infancy. The majority of NF1 individuals with tibial bowing will sustain a fracture that will not...not fracture and the bowing improves over time. Clinical predictors to help drive management are lacking, and the pathophysiology of tibial bowing

  2. 46 CFR 154.355 - Bow and stern loading piping.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 5 2013-10-01 2013-10-01 false Bow and stern loading piping. 154.355 Section 154.355 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CERTAIN BULK DANGEROUS CARGOES SAFETY... Arrangements § 154.355 Bow and stern loading piping. (a) Bow and stern loading piping must: (1) Meet § 154.310...

  3. 46 CFR 154.355 - Bow and stern loading piping.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 5 2011-10-01 2011-10-01 false Bow and stern loading piping. 154.355 Section 154.355 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CERTAIN BULK DANGEROUS CARGOES SAFETY... Arrangements § 154.355 Bow and stern loading piping. (a) Bow and stern loading piping must: (1) Meet § 154.310...

  4. Extraction of bowing parameters from violin performance combining motion capture and sensors.

    PubMed

    Schoonderwaldt, E; Demoucron, M

    2009-11-01

    A method is described for measurement of a complete set of bowing parameters in violin performance. Optical motion capture was combined with sensors for accurate measurement of the main bowing parameters (bow position, bow velocity, bow acceleration, bow-bridge distance, and bow force) as well as secondary control parameters (skewness, inclination, and tilt of the bow). In addition, other performance features (moments of on/off in bow-string contact, string played, and bowing direction) were extracted. Detailed descriptions of the calculations of the bowing parameters, features, and calibrations are given. The described system is capable of measuring all bowing parameters without disturbing the player, allowing for detailed studies of musically relevant aspects of bow control and coordination of bowing parameters in bowed-string instrument performance.

  5. Comparison of cast positions by using four face-bows.

    PubMed

    Goska, J R; Christensen, L V

    1988-01-01

    The positions that the maxillary right and left first molars occupy when a maxillary cast is mounted in the three-dimensional space of a semiadjustable articulator (Hanau H2) were studied. Mountings were made by using four face-bows, the Hanau Kinematic Face-bow, the Hanau Facia-bow, the Hanau 159 Earpiece Face-bow, and the Hanau Twirl Earpiece Face-bow. A kinematically determined hinge-axis was used arbitrarily as the baseline for comparisons among the three other bows. Deviations from the baseline were measured along the X, Y, and Z axes by using a contour meter (Fig. 1). The deviations showed great variability (Table I), and because maxillary casts are mounted in relation to anatomic landmarks that differ from subject to subject, it was not possible to establish clinical superiority of one face-bow over another.

  6. A BOW SHOCK NEAR A YOUNG STAR

    NASA Technical Reports Server (NTRS)

    2002-01-01

    NASA's Hubble Space Telescope continues to reveal various stunning and intricate treasures that reside within the nearby, intense star-forming region known as the Great Nebula in Orion. One such jewel is the bow shock around the very young star, LL Ori, featured in this Hubble Heritage image. Named for the crescent-shaped wave made by a ship as it moves through water, a bow shock can be created in space when two streams of gas collide. LL Ori emits a vigorous solar wind, a stream of charged particles moving rapidly outward from the star. Our own Sun has a less energetic version of this wind that is responsible for auroral displays on the Earth. The material in the fast wind from LL Ori collides with slow-moving gas evaporating away from the center of the Orion Nebula, which is located to the lower right in this Heritage image. The surface where the two winds collide is the crescent-shaped bow shock seen in the image. Unlike a water wave made by a ship, this interstellar bow shock is a three-dimensional structure. The filamentary emission has a very distinct boundary on the side facing away from LL Ori, but is diffuse on the side closest to the star, a characteristic common to many bow shocks. A second, fainter bow shock can be seen around a star near the upper right-hand corner of the Heritage image. Astronomers have identified numerous shock fronts in this complex star-forming region and are using this data to understand the many complex phenomena associated with the birth of stars. This image was taken in February 1995 as part of the Hubble Orion Nebula mosaic. A close visitor in our Milky Way galaxy, the nebula is only 1,500 light-years from Earth. The filters used in this color composite represent oxygen, nitrogen, and hydrogen emissions. Image Credit: NASA and the Hubble Heritage Team (STScI/AURA) Acknowledgment: C. R. O'Dell (Vanderbilt University)

  7. A BOW SHOCK NEAR A YOUNG STAR

    NASA Technical Reports Server (NTRS)

    2002-01-01

    NASA's Hubble Space Telescope continues to reveal various stunning and intricate treasures that reside within the nearby, intense star-forming region known as the Great Nebula in Orion. One such jewel is the bow shock around the very young star, LL Ori, featured in this Hubble Heritage image. Named for the crescent-shaped wave made by a ship as it moves through water, a bow shock can be created in space when two streams of gas collide. LL Ori emits a vigorous solar wind, a stream of charged particles moving rapidly outward from the star. Our own Sun has a less energetic version of this wind that is responsible for auroral displays on the Earth. The material in the fast wind from LL Ori collides with slow-moving gas evaporating away from the center of the Orion Nebula, which is located to the lower right in this Heritage image. The surface where the two winds collide is the crescent-shaped bow shock seen in the image. Unlike a water wave made by a ship, this interstellar bow shock is a three-dimensional structure. The filamentary emission has a very distinct boundary on the side facing away from LL Ori, but is diffuse on the side closest to the star, a characteristic common to many bow shocks. A second, fainter bow shock can be seen around a star near the upper right-hand corner of the Heritage image. Astronomers have identified numerous shock fronts in this complex star-forming region and are using this data to understand the many complex phenomena associated with the birth of stars. This image was taken in February 1995 as part of the Hubble Orion Nebula mosaic. A close visitor in our Milky Way galaxy, the nebula is only 1,500 light-years from Earth. The filters used in this color composite represent oxygen, nitrogen, and hydrogen emissions. Image Credit: NASA and the Hubble Heritage Team (STScI/AURA) Acknowledgment: C. R. O'Dell (Vanderbilt University)

  8. Bow shock and magnetosheath waves at Mercury

    NASA Technical Reports Server (NTRS)

    Fairfield, D. H.; Behannon, K. W.

    1975-01-01

    Mariner 10 measurements at the Mercury bow shock provide examples where the magnetic field is approximately parallel or perpendicular to the bow shock normal. Upstream of a broad irregular parallel shock, left hand circularly polarized waves are observed which cut off very sharply at approximately 4 Hz. Upstream of a perpendicular shock, right hand circularly polarized waves are observed which persist up to the Nyquist frequency of 12 Ha. Determination of the wave propagation vector as a function of frequency helps conclusively identify the waves as whistler mode waves propagating from the shock. The magnetosheath downstream of the parallel shock is disturbed more than that downstream of the perpendicular shock particularly below 1 Hz. In the latter case regular left hand polarized waves observed slightly above the proton gyrofrequency are identified as ion cyclotron waves with wavelength approximately 300 km which are Doppler shifted up to their observed frequency.

  9. A survey for Hα pulsar bow shocks

    SciTech Connect

    Brownsberger, Sasha; Romani, Roger W. E-mail: sashab@stanford.edu

    2014-04-01

    We report on a survey for Hα bow shock emission around nearby γ-detected energetic pulsars. This survey adds three Balmer-dominated neutron star bow shocks to the six previously confirmed examples. In addition to the shock around Fermi pulsar PSR J1741–2054, we now report Hα structures around two additional γ-ray pulsars, PSR J2030+4415 and PSR J1509–5850. These are the first known examples of Hα nebulae with pre-ionization halos. With new measurements, we show that a simple analytic model can account for the angular size and flux of the bow shocks' apices. The latter, in particular, provides a new pulsar probe and indicates large moments of inertia and smaller distances than previously assumed in several cases. In particular, we show that the re-measured PSR J0437–4715 shock flux implies I = (1.7 ± 0.2) × 10{sup 45}/(f {sub HI}sin i) g cm{sup 2}. We also derive a distance d ≈ 0.72 kpc for the γ-ray only pulsar PSR J2030+4415 and revised distances for PSRs J1959+2048 (1.4 kpc) and J2555+6535 (∼1 kpc), smaller than the conventional DM-estimated values. Finally, we report upper limits for 94 additional LAT pulsars. An estimate of the survey sensitivity indicates that for a warm neutral medium filling factor φ{sub WNM} ∼ 0.3 there should be a total of approximately nine Hα bow shocks in our LAT-targeted survey; given that seven such objects are now known, a much larger φ{sub WNM} seems problematic.

  10. A Survey for Hα Pulsar Bow Shocks

    NASA Astrophysics Data System (ADS)

    Brownsberger, Sasha; Romani, Roger W.

    2014-04-01

    We report on a survey for Hα bow shock emission around nearby γ-detected energetic pulsars. This survey adds three Balmer-dominated neutron star bow shocks to the six previously confirmed examples. In addition to the shock around Fermi pulsar PSR J1741-2054, we now report Hα structures around two additional γ-ray pulsars, PSR J2030+4415 and PSR J1509-5850. These are the first known examples of Hα nebulae with pre-ionization halos. With new measurements, we show that a simple analytic model can account for the angular size and flux of the bow shocks' apices. The latter, in particular, provides a new pulsar probe and indicates large moments of inertia and smaller distances than previously assumed in several cases. In particular, we show that the re-measured PSR J0437-4715 shock flux implies I = (1.7 ± 0.2) × 1045/(f H I sin i) g cm2. We also derive a distance d ≈ 0.72 kpc for the γ-ray only pulsar PSR J2030+4415 and revised distances for PSRs J1959+2048 (1.4 kpc) and J2555+6535 (~1 kpc), smaller than the conventional DM-estimated values. Finally, we report upper limits for 94 additional LAT pulsars. An estimate of the survey sensitivity indicates that for a warm neutral medium filling factor phiWNM ~ 0.3 there should be a total of approximately nine Hα bow shocks in our LAT-targeted survey; given that seven such objects are now known, a much larger phiWNM seems problematic.

  11. The earth's foreshock, bow shock, and magnetosheath

    SciTech Connect

    Onsager, T.G.; Thomsen, M.F. )

    1991-01-01

    Studies directly pertaining to the earth's foreshock, bow shock, and magnetosheath are reviewed, and some comparisons are made with data on other planets. Topics considered in detail include the electron foreshock, the ion foreshock, the quasi-parallel shock, the quasi-perpendicular shock, and the magnetosheath. Information discussed spans a broad range of disciplines, from large-scale macroscopic plasma phenomena to small-scale microphysical interactions. 184 refs.

  12. Bow Shock in the Great Nebula

    NASA Technical Reports Server (NTRS)

    1995-01-01

    The nearby intense star-forming region known as the Great Nebula in the Orion constellation reveals a bow shock around a very young star as seen by NASA's Hubble Space Telescope (HST). Named for the crescent-shaped wave made by a ship as it moves through the water, a bow shock can be created in space where two streams of gas collide. LL Ori emits a vigorous solar wind, a stream of charged particles moving rapidly outward from the star. Our own sun has a less energetic version of this wind. The material in the fast wind from LL Ori collides with slow moving gas evaporating away form the center of the Orion Nebula, which is located in the lower right of this image, producing the crescent shaped bow shock seen in the image. Astronomers have identified numerous shock fronts in this complex star-forming region and are using this data to understand the many complex phenomena associated with the birth of stars. A close visitor in our Milky Way Galaxy, the nebula is only 1,500 light years away from Earth. The filters used in this color composite represent oxygen, nitrogen, and hydrogen emissions.

  13. Gamma radiation from blazar PKS 0537-441

    NASA Technical Reports Server (NTRS)

    Thompson, D. J.; Bertsch, D. L.; Fichtel, C. E.; Hartman, R. C.; Hunter, S. D.; Kanbach, G.; Kniffen, D. A.; Kwok, P. W.; Lin, Y. C.; Mattox, J. R.

    1993-01-01

    The Energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory (CGRO) observed high-energy gamma rays from PKS 0537-441 during observations in 1991 July-August. Upper limits from later EGRET observations suggest time variability.

  14. Gamma radiation from blazar PKS 0537-441

    NASA Technical Reports Server (NTRS)

    Thompson, D. J.; Bertsch, D. L.; Fichtel, C. E.; Hartman, R. C.; Hunter, S. D.; Kanbach, G.; Kniffen, D. A.; Kwok, P. W.; Lin, Y. C.; Mattox, J. R.

    1993-01-01

    The Energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory (CGRO) observed high-energy gamma rays from PKS 0537-441 during observations in 1991 July-August. Upper limits from later EGRET observations suggest time variability.

  15. Coordination in fast repetitive violin-bowing patterns.

    PubMed

    Schoonderwaldt, Erwin; Altenmüller, Eckart

    2014-01-01

    We present a study of coordination behavior in complex violin-bowing patterns involving simultaneous bow changes (reversal of bowing direction) and string crossings (changing from one string to another). Twenty-two violinists (8 advanced amateurs, 8 students with violin as major subject, and 6 elite professionals) participated in the experiment. We investigated the influence of a variety of performance conditions (specific bowing patterns, dynamic level, tempo, and transposition) and level of expertise on coordination behavior (a.o., relative phase and amplitude) and stability. It was found that the general coordination behavior was highly consistent, characterized by a systematic phase lead of bow inclination over bow velocity of about 15° (i.e., string crossings were consistently timed earlier than bow changes). Within similar conditions, a high individual consistency was found, whereas the inter-individual agreement was considerably less. Furthermore, systematic influences of performance conditions on coordination behavior and stability were found, which could be partly explained in terms of particular performance constraints. Concerning level of expertise, only subtle differences were found, the student and professional groups (higher level of expertise) showing a slightly higher stability than the amateur group (lower level of expertise). The general coordination behavior as observed in the current study showed a high agreement with perceptual preferences reported in an earlier study to similar bowing patterns, implying that complex bowing trajectories for an important part emerge from auditory-motor interaction.

  16. Coordination in Fast Repetitive Violin-Bowing Patterns

    PubMed Central

    Schoonderwaldt, Erwin; Altenmüller, Eckart

    2014-01-01

    We present a study of coordination behavior in complex violin-bowing patterns involving simultaneous bow changes (reversal of bowing direction) and string crossings (changing from one string to another). Twenty-two violinists (8 advanced amateurs, 8 students with violin as major subject, and 6 elite professionals) participated in the experiment. We investigated the influence of a variety of performance conditions (specific bowing patterns, dynamic level, tempo, and transposition) and level of expertise on coordination behavior (a.o., relative phase and amplitude) and stability. It was found that the general coordination behavior was highly consistent, characterized by a systematic phase lead of bow inclination over bow velocity of about 15° (i.e., string crossings were consistently timed earlier than bow changes). Within similar conditions, a high individual consistency was found, whereas the inter-individual agreement was considerably less. Furthermore, systematic influences of performance conditions on coordination behavior and stability were found, which could be partly explained in terms of particular performance constraints. Concerning level of expertise, only subtle differences were found, the student and professional groups (higher level of expertise) showing a slightly higher stability than the amateur group (lower level of expertise). The general coordination behavior as observed in the current study showed a high agreement with perceptual preferences reported in an earlier study to similar bowing patterns, implying that complex bowing trajectories for an important part emerge from auditory-motor interaction. PMID:25207542

  17. Measurement of Force of Bow Holding and Contact Force between Bow Hair and String in Violin Playing by Pressure Measuring Film

    NASA Astrophysics Data System (ADS)

    Matsutani, Akihiro

    2001-09-01

    The force of bow holding and the contact force between bow hair and string in violin playing were measured by a pressure measuring film for the first time. It was scientifically identified that relaxed bowing was important for achieving a good violin tone. The proposed measurement manner may be helpful for objective evaluation of the bowing skill of amateur violinists.

  18. Intriguing Microvariability Observations of PKS 0736+017

    NASA Astrophysics Data System (ADS)

    Clements, S. D.; Reyes, F.; Clark, D.; Gomez, C.; Jenks, A.; Torres, Y.

    2002-05-01

    The optically violent variable quasar PKS 0736+017 was monitored for microvariability in early 2002. Observations were made with the 0.9m SARA telescope atop Kitt Peak in Arizona and with the 0.76m telescope at Rosemary Hill Observatory in Bronson, Florida. In January, it underwent a substantial flaring event, brightening by 1.3 R magnitudes in 2 hours and exhibiting unusual oscillatory fluctuations once it reached its bright state. Later, its V-R color was also monitored and it was found to exhibit atypical color variations, reddening as it got brighter. The curious behavior displayed by PKS 0736+017 will be compared to that of other sources.

  19. A NIR Flare of the Blazar PKS0235+164

    NASA Astrophysics Data System (ADS)

    Carrasco, L.; Recillas, E.; Porras, A.; Chavushyan, V.; Mayya, D. Y.

    2017-02-01

    We report on the recent NIR flare of the high redshift QSO (z=0.94) PKS0235+164 also known as CGRaBSJ0238+1636, cross correlated with the Gamma-ray source 2FGLJ0238.7+1637.On FEbruary 3rd,2017 MJD(2457787.6717, we found the source with NIR fluxes corresponding to J = 14.867+/- 0.04, H = 13.795 +/- 0.03 and Ks = 12.947 +/- 0.05.

  20. AGILE detection of a flare from PKS 1510-089

    NASA Astrophysics Data System (ADS)

    Bulgarelli, A.; Tavani, M.; Fioretti, V.; Gianotti, F.; Trifoglio, M.; Pittori, C.; Verrecchia, F.; Lucarelli, F.; Vercellone, S.; Piano, G.; Donnarumma, I.; Striani, E.; Cardillo, M.; Giuliani, A.; Mereghetti, S.; Caraveo, P.; Perotti, F.; Chen, A.; Colafrancesco, S.; Del Monte, E.; Evangelista, Y.; Feroci, M.; Lazzarotto, F.; Pacciani, L.; Soffitta, P.; Costa, E.; Lapshov, I.; Rapisarda, M.; Argan, A.; Pucella, G.; Sabatini, S.; Trois, A.; Vittorini, V.; Fuschino, F.; Galli, M.; Labanti, C.; Marisaldi, M.; Di Cocco, G.; Pellizzoni, A.; Pilia, M.; Barbiellini, G.; Vallazza, E.; Longo, F.; Morselli, A.; Picozza, P.; Prest, M.; Lipari, P.; Zanello, D.; Cattaneo, P. W.; Rappoldi, A.; Giommi, P.; Salotti, L.; Valentini, G.

    2014-08-01

    AGILE is now detecting transient gamma-ray emission above 100 MeV from a source positionally consistent with PKS 1510-089. Integrating from 2014-07-31 00:43 UT to 2014-08-02 02:15 UT, a preliminary maximum likelihood analysis yields a detection above 100 MeV positioned at Galactic coordinates (l,b) = (350.96, 40.12) +/- 0.9 (stat.) +/- 0.1 (syst.).

  1. On the mechanics of the modern working-recurve bow

    NASA Astrophysics Data System (ADS)

    Kooi, B. W.

    1991-09-01

    Characteristic for the bow are the slender elastic arms or limbs. The bow is braced by putting a string shorter than the bow between the tips of the limbs. Additional deformation energy is stored in the elastic limbs by drawing the bow into the fully drawn position. Part of this amount of energy is transformed into kinetic energy of a light arrow. In the 1930's the design of the bow became a subject of scientific research. Experiments were performed in which design parameters were changed more or less systematically. However, the mathematical models were rather simple. Because fast computers are now available the presented model in this paper can be much more advanced. The resulting set of partial differential equations with known initial values and moving boundaries is solved numberically using a finite-difference method. In this paper the design parameters associated with the developed model are charted accurately. Bows used in the past and nowadays on shooting meetings such as the Olympic Games are compared. It turns out that the application of better materials which can store more deformation energy per unit of mass and that this material is used to a larger extent, contribute most to the improvement of the bow. The parameters which fix the mechanical performance of the bow appear to be less important as is often claimed.

  2. 75 FR 39201 - MedBow-Routt Resource Advisory Committee

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-07-08

    ... Forest Service MedBow-Routt Resource Advisory Committee AGENCY: Forest Service, USDA. ACTION: Notice of meeting. SUMMARY: The MedBow-Routt Resource Advisory Committee will meet in Steamboat Springs, Colorado... Act (Pub. L. 110-343) and in compliance with the Federal Advisory Committee Act. The purpose of the...

  3. Muscular activation patterns of the bow arm in recurve archery.

    PubMed

    Ertan, Hayri

    2009-05-01

    In archery shooting, the archer should hold the bow in place using only the pressure produced through drawing back the bowstring. Most coaches discourage the archer from gripping the bow as this is believed to produce a sideways deflecting torque on the bow and arrow during the release. The purpose of this study was to compare the bow hand forearm muscular activation patterns of elite archers with beginners to define the muscular contraction-relaxation strategies in the bow hand forearm muscles during archery shooting and investigate the effects of performance level on these strategies. Electromyographic activity of the M. flexor digitorum superficialis and the M. extensor digitorum of 10 elite and 10 beginner archers were recorded together with a pulse synchronized with the clicker snap. Raw electromyographic records as 1s before and after the clicker pulse were rectified, integrated, and normalized. The data was then averaged for successive shots of each subject and later for both groups of archers. The main difference between the elite and beginner archers was that the elite archers had a greater activation of the M. extensor digitorum, which indicates that they avoid gripping the bow-handle not only relaxing the flexor muscles, but also contracting the extensor muscle groups. This muscular contraction strategy secures the archer to not interfere with the forward movement of the bow, which is the forward acceleration of the bow caused by the pushing power of the bowstring.

  4. 46 CFR 154.355 - Bow and stern loading piping.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... Arrangements § 154.355 Bow and stern loading piping. (a) Bow and stern loading piping must: (1) Meet § 154.310; (2) Be installed in an area away from the accommodation, service, or control space on type IG hulls; (3) Be clearly marked; (4) Be segregated from the cargo piping by a removable spool piece in the...

  5. 46 CFR 45.69 - Correction for bow height.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 2 2010-10-01 2010-10-01 false Correction for bow height. 45.69 Section 45.69 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) LOAD LINES GREAT LAKES LOAD LINES Freeboards § 45.69 Correction for bow height. (a) The minimum summer freeboard of all manned vessels must...

  6. 46 CFR 45.69 - Correction for bow height.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 2 2011-10-01 2011-10-01 false Correction for bow height. 45.69 Section 45.69 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) LOAD LINES GREAT LAKES LOAD LINES Freeboards § 45.69 Correction for bow height. (a) The minimum summer freeboard of all manned vessels must...

  7. 46 CFR 154.1870 - Bow and stern loading.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CERTAIN BULK DANGEROUS CARGOES SAFETY... loading. (a) When the bow or stern loading piping is not in use, the master shall lock closed the shut-off... cargo transfer shall ensure that after the bow or stern loading piping is used it is purged of cargo...

  8. 46 CFR 154.1870 - Bow and stern loading.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CERTAIN BULK DANGEROUS CARGOES SAFETY... loading. (a) When the bow or stern loading piping is not in use, the master shall lock closed the shut-off... cargo transfer shall ensure that after the bow or stern loading piping is used it is purged of cargo...

  9. 46 CFR 154.1870 - Bow and stern loading.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CERTAIN BULK DANGEROUS CARGOES SAFETY... loading. (a) When the bow or stern loading piping is not in use, the master shall lock closed the shut-off... cargo transfer shall ensure that after the bow or stern loading piping is used it is purged of cargo...

  10. Evolution of Bow-Tie Architectures in Biology

    PubMed Central

    Friedlander, Tamar; Mayo, Avraham E.; Tlusty, Tsvi; Alon, Uri

    2015-01-01

    Bow-tie or hourglass structure is a common architectural feature found in many biological systems. A bow-tie in a multi-layered structure occurs when intermediate layers have much fewer components than the input and output layers. Examples include metabolism where a handful of building blocks mediate between multiple input nutrients and multiple output biomass components, and signaling networks where information from numerous receptor types passes through a small set of signaling pathways to regulate multiple output genes. Little is known, however, about how bow-tie architectures evolve. Here, we address the evolution of bow-tie architectures using simulations of multi-layered systems evolving to fulfill a given input-output goal. We find that bow-ties spontaneously evolve when the information in the evolutionary goal can be compressed. Mathematically speaking, bow-ties evolve when the rank of the input-output matrix describing the evolutionary goal is deficient. The maximal compression possible (the rank of the goal) determines the size of the narrowest part of the network—that is the bow-tie. A further requirement is that a process is active to reduce the number of links in the network, such as product-rule mutations, otherwise a non-bow-tie solution is found in the evolutionary simulations. This offers a mechanism to understand a common architectural principle of biological systems, and a way to quantitate the effective rank of the goals under which they evolved. PMID:25798588

  11. Evolution of bow-tie architectures in biology.

    PubMed

    Friedlander, Tamar; Mayo, Avraham E; Tlusty, Tsvi; Alon, Uri

    2015-03-01

    Bow-tie or hourglass structure is a common architectural feature found in many biological systems. A bow-tie in a multi-layered structure occurs when intermediate layers have much fewer components than the input and output layers. Examples include metabolism where a handful of building blocks mediate between multiple input nutrients and multiple output biomass components, and signaling networks where information from numerous receptor types passes through a small set of signaling pathways to regulate multiple output genes. Little is known, however, about how bow-tie architectures evolve. Here, we address the evolution of bow-tie architectures using simulations of multi-layered systems evolving to fulfill a given input-output goal. We find that bow-ties spontaneously evolve when the information in the evolutionary goal can be compressed. Mathematically speaking, bow-ties evolve when the rank of the input-output matrix describing the evolutionary goal is deficient. The maximal compression possible (the rank of the goal) determines the size of the narrowest part of the network-that is the bow-tie. A further requirement is that a process is active to reduce the number of links in the network, such as product-rule mutations, otherwise a non-bow-tie solution is found in the evolutionary simulations. This offers a mechanism to understand a common architectural principle of biological systems, and a way to quantitate the effective rank of the goals under which they evolved.

  12. Auditory perception of note transitions in simulated complex bowing patterns.

    PubMed

    Schoonderwaldt, Erwin; Demoucron, Matthias; Altenmüller, Eckart; Leman, Marc

    2013-06-01

    Recent motion-capture measurements of violin bowing revealed an interesting coordination behavior in fast repetitive bowing patterns involving bow changes and string crossings; bow changes were consistently lagging behind string crossings, and the relative timing appeared to be an integral part of the bow-movement patterns. The aim of the current study was to investigate if there might be a perceptual explanation for the observed coordination behavior. For this purpose a virtual violin was used, controlled by simulated bowing gestures. A simplified coordination model is presented, which was implemented to allow real-time control of complex bowing patterns. This synthesis approach was employed in a perceptual experiment in which the participants were asked to optimize the sound by adjusting a slider controlling the main coordination parameters. It was found that the resulting coordination patterns were similar to those observed in performance, implying that complex bowing trajectories for an important part emerge from auditory-motor interaction. Further analysis of the responses shed light on temporal and spatial constraints of the simulated gestures associated with the note transitions. The results raise interesting questions with regard to auditory-motor interaction in complex instrumental control gestures.

  13. Marble bowing: comparative studies of three different public building facades

    NASA Astrophysics Data System (ADS)

    Siegesmund, S.; Ruedrich, J.; Koch, A.

    2008-12-01

    The veneer cladding of the Oeconomicum (OEC, Göttingen), the State Theatre of Darmstadt (STD, Darmstadt) and of the State and University Library (SUB, Göttingen) is characterised by pronounced bowing after a short time of exposure. Direct comparison of bowing data related to measurements from 2000 to 2003 at the SUB clearly show that the amplitude in bowing had significantly increased. The bowing is different in intensity and orientation (concave, convex). The cladding material (Peccia marble, Rosa Estremoz marble and Carrara marble) are different in lattice preferred orientation, grain size distribution and grain interlocking. Depending on the bowing, panels may show cracks mostly initiated at the dowels. The percentage of visible cracks and breakouts increases with the amplitude of bowing except for the STD. Repetitive heating-cooling under dry conditions leads to considerable inelastic residual strain only after the first or second thermal cycle. The residual strain continuously increases again if water is present, whereby the moisture content after a thermal cycle has a certain impact on the decay rate. The water-enhanced thermal dilatation strongly correlates with the deterioration rate obtained from the laboratory bow test. Detailed petrophysical investigations provide evidence that with increasing bowing a decrease of mechanical properties (flexural strength or breaking load at dowel hole) occur. Marble degradation is also connected with the increase in porosity and a general shift of the maximum pore radii to larger pore sizes. On-site damage analyses were combined with laboratory tests of the bowing potential to constrain factors that may influence the risk failure. The experimental bowing data clearly demonstrate that after 40 heating cycles combined with the effect of moisture a certain impact on the decay rate is observed. In the case of demounted panels the bowing tests show that already strongly deformed panels from the building exhibit a lower

  14. Prevalence and characteristics of pks genotoxin gene cluster-positive clinical Klebsiella pneumoniae isolates in Taiwan

    PubMed Central

    Chen, Ying-Tsong; Lai, Yi-Chyi; Tan, Mei-Chen; Hsieh, Li-Yun; Wang, Jann-Tay; Shiau, Yih-Ru; Wang, Hui-Ying; Lin, Ann-Chi; Lai, Jui-Fen; Huang, I-Wen; Lauderdale, Tsai-Ling

    2017-01-01

    The pks gene cluster encodes enzymes responsible for the synthesis of colibactin, a genotoxin that has been shown to induce DNA damage and contribute to increased virulence. The present study investigated the prevalence of pks in clinical K. pneumoniae isolates from a national surveillance program in Taiwan, and identified microbiological and molecular factors associated with pks-carriage. The pks gene cluster was detected in 67 (16.7%) of 400 isolates from various specimen types. Multivariate analysis revealed that isolates of K1, K2, K20, and K62 capsular types (p < 0.001), and those more susceptible to antimicrobial agents (p = 0.001) were independent factors strongly associated with pks-carriage. Phylogenetic studies on the sequence type (ST) and pulsed-field gel electrophoresis patterns indicated that the pks-positive isolates belong to a clonal group of ST23 in K1, a locally expanding ST65 clone in K2, a ST268-related K20 group, and a highly clonal ST36:K62 group. Carriage of rmpA, iutC, and ybtA, the genes associated with hypervirulence, was significantly higher in the pks-positive isolates than the pks-negative isolates (95.5% vs. 13.2%, p < 0.001). Further studies to determine the presence of hypervirulent pks-bearing bacterial populations in the flora of community residents and their association with different disease entities may be warranted. PMID:28233784

  15. The foreshock region upstream from the Comet Halley bow shock

    NASA Technical Reports Server (NTRS)

    Fuselier, S. A.; Anderson, K. A.; Balsiger, H.; Glassmeier, K. H.; Goldstein, B. E.; Neugebauer, M.; Rosenbauer, H.; Shelley, E. G.

    1987-01-01

    A few hours prior to the crossing of the Comet Halley bow shock, the Giotto spacecraft intermittently encountered an electron foreshock region. The electron foreshock is characterized by magnetic connection to the cometary bow shock and increased field aligned electron heat flux directed away from the bow shock. A similar region was intermittently encountered by the ICE spacecraft prior to its crossing of the Giacobini-Zinner bow wave. During periods of magnetic connection with the Halley bow shock, enhanced magnetic field fluctuations were observed. These enhancements are interpreted as indirect evidence of an ion foreshock in the electron foreshock. No clearly identifiable backstreaming protons are observed during these periods of magnetic connection, however, because it may be difficult to separate a backstreaming population from the cometary pick-up proton population already present in the upstream region.

  16. The foreshock region upstream from the Comet Halley bow shock

    NASA Technical Reports Server (NTRS)

    Fuselier, S. A.; Anderson, K. A.; Balsiger, H.; Glassmeier, K. H.; Goldstein, B. E.; Neugebauer, M.; Rosenbauer, H.; Shelley, E. G.

    1987-01-01

    A few hours prior to the crossing of the Comet Halley bow shock, the Giotto spacecraft intermittently encountered an electron foreshock region. The electron foreshock is characterized by magnetic connection to the cometary bow shock and increased field aligned electron heat flux directed away from the bow shock. A similar region was intermittently encountered by the ICE spacecraft prior to its crossing of the Giacobini-Zinner bow wave. During periods of magnetic connection with the Halley bow shock, enhanced magnetic field fluctuations were observed. These enhancements are interpreted as indirect evidence of an ion foreshock in the electron foreshock. No clearly identifiable backstreaming protons are observed during these periods of magnetic connection, however, because it may be difficult to separate a backstreaming population from the cometary pick-up proton population already present in the upstream region.

  17. The bow and cultural complexity of the Canadian Plains.

    PubMed

    Walde, Dale

    2013-01-01

    The timing and circumstances of the introduction of the bow and arrow into past North American economic and social lifeways have been sources of interest and controversy among archeologists for a very long time. Initial interpretations of the adoption of the bow and arrow generally seem to have been based on the rather straightforward assumption of functional superiority as a hunting tool. That is, the bow and arrow was simply a better instrument than the atlatl-dart technology it replaced. More recently, however, researchers exploring the effectiveness of the atlatl as a hunting tool have responded with studies that challenge the assumed universal functional superiority of the bow and arrow as a hunting device. Social coercion and warfare theory presents an alternative perspective on the adoption of the bow and arrow.

  18. A biodifferential system of face-bow mechanics.

    PubMed

    Dougherty, H L; Beazley, W W

    1976-11-01

    A review of the literature, both scientific and commercial, did not demonstrate the separation of the inner and outer bows into a biodifferential interchangeable system. The prime design idea, to separate the inner and outer bows, increased versatility and yielded a multiple appliance with a greater range of use and safety. The joint couple systems could be adapted to fulfill the criteria cited in the literature during preliminary treatment (deciduous dentition), partial treatment, full-banded treatment, and retention. The biodifferential design was compatible with most mechanical orthodontic appliances and systems currently used. The three joint designs presented and the three inner bow lock devices fulfilled the parameters expected from the normal use of the present face-bow in necessary strength, stability, and use. Further, the use of a joint couple between the inner and outer bows expanded the versatility of the face-bow into a biodifferential system and allowed for an easily manageable and orderly change of forces, vectors, sizes, and shapes requiring little chair time and minimum instruction to the patient. The inner bow could be used as an intraoral appliance for bumpers, shields, and oral screens. These easily made, preformed, interlocking parts could be marked or color coded as to type and size and keyed, grooved, and designed to prevent inverted interlocking of parts. The inner bow could be tied in, as an aid in patient cooperation, or the inner and outer bows could be pinned or ligated together to prevent separation. One of the most important factors of the biodifferential system is protection of the patient from severe trauma to the eyes, face, and mouth due to misuse or accident, as has occurred in the one-piece face-bow. The biodifferential system fulfills the five criteria of the investigation: (1) a system of interchangeable, interlocking joint parts, (2) safety and dependability, (3) easy changes in force, vectors, and moments, (4) enhanced

  19. How we broke the BOWS watermark

    NASA Astrophysics Data System (ADS)

    Craver, Scott; Atakli, Idris; Yu, Jun

    2007-02-01

    From December 2005 to March of 2006, the Break Our Watermarking System (BOWS) contest challenged researchers to break an image watermark of unknown design. The attacked images had to possess a minimum quality level of 30 dB PSNR, and the winners would be those of highest average quality over three images. Our research team won this challenge, employing the strategy of reverse-engineering the watermark before any attempts to attack it in earnest. We determined the frequency transform, sub-band, and an exploitable quirk in the detector that made it sensitive to noise spikes. Of interest is our overall methodology of reverse-engineering through severe false alarms, and we introduce a new concept, "superrobustness," which despite its positive name is a security flaw.

  20. Distant Bow Shock Observations by Explorer 33

    NASA Technical Reports Server (NTRS)

    Mihalov, J. D.

    1973-01-01

    Locations, orientations and magnetic field changes are given for 135 bow shock crossings at distances downstream from earth between 84 and 117 earth radii. The shock locations are dependent on the spacecraft trajectory and agree with locations calculated for the hypersonic analogue for a Mach number of 3.8. The shock normal vectors have been calculated using magnetic coplanarity. The average normal vectors have a greater inclination by approximately 17 + or - 5 deg from the symmetry axis than the Dryer and Heckman shock orientations for a 3.8 Mach number. Over a range of downstream distances from 60 to 115 earth radii, the median magnetic field magnitude jump across the shock changes from 1.90 to 1.70 times.

  1. Suprathermal Electrons at Saturn's Bow Shock

    NASA Astrophysics Data System (ADS)

    Masters, A.; Sulaiman, A. H.; Sergis, N.; Stawarz, L.; Fujimoto, M.; Coates, A. J.; Dougherty, M. K.

    2016-07-01

    The leading explanation for the origin of galactic cosmic rays is particle acceleration at the shocks surrounding young supernova remnants (SNRs), although crucial aspects of the acceleration process are unclear. The similar collisionless plasma shocks frequently encountered by spacecraft in the solar wind are generally far weaker (lower Mach number) than these SNR shocks. However, the Cassini spacecraft has shown that the shock standing in the solar wind sunward of Saturn (Saturn's bow shock) can occasionally reach this high-Mach number astrophysical regime. In this regime Cassini has provided the first in situ evidence for electron acceleration under quasi-parallel upstream magnetic conditions. Here we present the full picture of suprathermal electrons at Saturn's bow shock revealed by Cassini. The downstream thermal electron distribution is resolved in all data taken by the low-energy electron detector (CAPS-ELS, <28 keV) during shock crossings, but the higher energy channels were at (or close to) background. The high-energy electron detector (MIMI-LEMMS, >18 keV) measured a suprathermal electron signature at 31 of 508 crossings, where typically only the lowest energy channels (<100 keV) were above background. We show that these results are consistent with the theory in which the “injection” of thermal electrons into an acceleration process involves interaction with whistler waves at the shock front, and becomes possible for all upstream magnetic field orientations at high Mach numbers like those of the strong shocks around young SNRs. A future dedicated study will analyze the rare crossings with evidence for relativistic electrons (up to ˜1 MeV).

  2. Femoral bow predicts postoperative malalignment in revision total knee arthroplasty.

    PubMed

    Sebastian, Arjun S; Wilke, Benjamin K; Taunton, Michael J; Trousdale, Robert T

    2014-08-01

    Diaphyseal bowing may compromise axial alignment in revision total knee arthroplasty (TKA). 277 patients undergoing revision TKA were evaluated for coronal bowing and hip-knee-ankle (HKA) axis. The mean femoral bow was 1.52° ± 0.18° varus (-10.1° to +8.4°). The mean tibial bow was 1.25° ± 0.13° valgus (-5.9° to +10°). HKA axis averaged 3.08° ± 0.35° varus preoperatively compared to 0.86° ± 0.25° varus postoperatively. Inter-rater and intra-rater reliability was high. Femoral bow greater than 4° significantly correlated with postoperative HKA axis malalignment (r = 0.402, P = 0.008). 39.7% of patients deviated 3° or greater from a neutral mechanical axis with a significant difference in femoral bow (0.94° ± 0.31°, P = 0.003). Diaphyseal bowing clearly has an important effect on postoperative limb alignment in revision TKA.

  3. Optimization of bow shape for a non ballast water ship

    NASA Astrophysics Data System (ADS)

    Van He, Ngo; Ikeda, Yoshiho

    2013-09-01

    In this research, a commercial CFD code "Fluent" was applied to optimization of bulbous bow shape for a non ballast water ships (NBS). The ship was developed at the Laboratory of the authors in Osaka Prefecture University, Japan. At first, accuracy of the CFD code was validated by comparing the CFD results with experimental results at towing tank of Osaka Prefecture University. In the optimizing process, the resistances acting on ships in calm water and in regular head waves were defined as the object function. Following features of bulbous bow shapes were considered as design parameters: volume of bulbous bow, height of its volume center, angle of bow bottom, and length of bulbous bow. When referring to the computed results given by the CFD like resistance, pressure and wave pattern made by ships in calm water and in waves, an optimal bow shape for ships was discovered by comparing the results in the series of bow shapes. In the computation on waves, the ship is in fully captured condition because shorter waves, λ/ L pp <0.6, are assumed.

  4. The bow and arrow in northern North America.

    PubMed

    Maschner, Herbert; Mason, Owen K

    2013-01-01

    There were at least four waves of bow and arrow use in northern North America. These occurred at 12000, 4500, 2400, and after about 1300 years ago. But to understand the role of the bow and arrow in the north, one must begin in the eighteenth century, when the Russians first arrived in the Aleutian Islands. At that time, the Aleut were using both the atlatl and dart and the bow and arrow (Fig. ). This is significant for two particular and important reasons. First, there are few historic cases in which both technologies were used concurrently; second, the bow and arrow in the Aleutian Islands were used almost exclusively in warfare. The atlatl was a critical technology because the bow and arrow are useless for hunting sea mammals. One cannot launch an arrow from a kayak because it is too unstable and requires that both hands remain on a paddle. To use an atlatl, it is necessary only to stabilize the kayak with a paddle on one side and launch the atlatl dart with the opposite hand. The Aleut on the Alaska Peninsula did indeed use the bow and arrow to hunt caribou there. However, in the 1,400 km of the Aleutian Islands, there are no terrestrial mammals except humans and the bow was reserved almost exclusively for conflicts among them. The most significant event in the history of the bow and arrow is not its early introduction, but rather the Asian War Complex 1300 years ago, when the recurve and backed bows first entered the region, altering regional and hemispheric political dynamics forever. [Figure: see text].

  5. The static response of a bowed inclined hot wire

    NASA Technical Reports Server (NTRS)

    Smits, A. J.

    1984-01-01

    The directional sensitivity of a bowed, inclined hot wire is investigated using a simple model for the convective heat transfer. The static response is analyzed for subsonic and supersonic flows. It is shown that the effects of both end conduction and wire bowing are greater in supersonic flow. Regardless of the Mach number, however, these two phenomena have distinctly different effects; end conduction appears to be responsible for reducing the nonlinearity of the response, whereas bowing increases the directional sensitivity. Comparison with the available data suggests that the analysis is useful for interpreting the experimental results.

  6. Structural changes in cuticles on violin bow hair caused by wear.

    PubMed

    Yamamoto, Tomoko; Sugiyama, Shigeru

    2010-01-01

    A bow with horse tail hair is used to play the violin. New and worn-out bow hairs were observed by atomic force microscopy. The cuticles of the new bow hair were already damaged by bleach and delipidation, however the worn-out bow hairs were much more damaged and broken off by force, which relates to wearing out.

  7. NIR flaring of the QSO PKS 2233-148

    NASA Astrophysics Data System (ADS)

    Carrasco, L.; Luna, A.; Mayya, D. Y.; Porras, A.; Recillas, E.; Carraminana, A.

    2012-10-01

    We have observed a recent NIR brightening of the flat spectrum QSO PKS2233-148 (z=0.325), a gamma ray source 2FGL J2236.5-1431. On September 26th, 2012, epoch JD2456196.813507, we determined the flux in the H band to be 13.096 +/- 0.04. That is 2 magnitudes brighter than the flux determined by the 2mass survey. Observations were carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera.

  8. NIR brightening of the Quasar PKS0507+17

    NASA Astrophysics Data System (ADS)

    Carrasco, L.; Luna, A.; Escobedo, G.; Mayya, D. Y.; Porras, A.; Recillas, E.; Carraminana, A.

    2012-10-01

    We have observed a recent NIR brightening of the quasar PKS0507+17 (z=0.416), a gamma ray source 1FGL J0510.0+1800. On October 28th,2012, epoch JD2456228.98800, we determined the flux in the H band to be 13.077 +/- 0.05. That is 2.5 magnitudes brighter than the flux determined by the 2mass survey. Observations were carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera.

  9. NIR flaring of the blazar PKS0048-097

    NASA Astrophysics Data System (ADS)

    Carrasco, L.; Carramiñana, A.; Recillas, E.; Porras, A.; Escobedo, G.; Mayya, Y. D.; Valdes, J. R.

    2011-01-01

    We call attention on our recent NIR observations of the gamma ray source 1FGL J0050.6-0928, an intermediate redshift Blazar PKS0048-097 (z=0.634), also known as FBQS J0050-0929. The observations were carried out with the CANICA NIR camera on the 2.1m telescope at the Observatorio Astrofísico Guillermo Haro, located in Cananea, Mexico. We found this blazar to be in outburst. It shows fluxes about 1.7 magnitudes brighter than our previous NIR photometry (JD2455450.944784, H = 14.427 ± 0.11).

  10. NIR brightening of the Blazar PKS1550-242

    NASA Astrophysics Data System (ADS)

    Carrasco, L.; Porras, A.; Escobedo, G.; Recillas, E.; Carraminana, A.

    2013-04-01

    We call attention on our recent NIR observations of the Gamma Ray source 1FGLJ1553.4-2425, (cross correlated in position with the radio source PKS1550-242) with the CANICA NIR camera on the 2.1m telescope at the Observatorio Astrofisico Guillermo Haro, located in Cananea, Mexico. On April 5th, 2013 (JD2456387.0006), we found this blazar to be in a new outburst. It showed fluxes about 0.7 magnitudes brighter than our previous NIR photometry.

  11. Laser vibrometry measurements of vibration and sound fields of a bowed violin

    NASA Astrophysics Data System (ADS)

    Gren, Per; Tatar, Kourosh; Granström, Jan; Molin, N.-E.; Jansson, Erik V.

    2006-04-01

    Laser vibrometry measurements on a bowed violin are performed. A rotating disc apparatus, acting as a violin bow, is developed. It produces a continuous, long, repeatable, multi-frequency sound from the instrument that imitates the real bow-string interaction for a 'very long bow'. What mainly differs is that the back and forward motion of the real bow is replaced by the rotating motion with constant velocity of the disc and constant bowing force (bowing pressure). This procedure is repeatable. It is long lasting and allows laser vibrometry techniques to be used, which measure forced vibrations by bowing at all excited frequencies simultaneously. A chain of interacting parts of the played violin is studied: the string, the bridge and the plates as well as the emitted sound field. A description of the mechanics and the sound production of the bowed violin is given, i.e. the production chain from the bowed string to the produced tone.

  12. 3. VIEW, LOOKING EAST, SHOWING BOW END OF VESSEL 37, ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    3. VIEW, LOOKING EAST, SHOWING BOW END OF VESSEL 37, STERN OF VESSEL 38 WITH COLLAPSING LIVING QUARTERS TO RIGHT Susan Kardas, photographer, November 1984 - Shooters Island, Ships Graveyard, Vessel No. 37, Newark Bay, Staten Island (subdivision), Richmond County, NY

  13. Geology and sediment accumulation rates at Carrie Bow Cay, Belize

    USGS Publications Warehouse

    Shinn, Eugene A.; Hudson, J. Harold; Halley, Robert B.; Lidz, Barbara H.; Robbin, Daniel M.; Macintyre, Ian G.; Ruetzler, Klaus; Macintyre, Ian G.

    1982-01-01

    Two other rotary cores were drilled landward of the reef crest. One was drilled on the reef flat to a depth of 8.8 m, and the other was drilled on the southwest tip of Carrie Bow Cay to a depth of 17.7 m. Both cores encountered essentially uncemented carbonate reef sands with some coral rubble. Of the four rotary cores, only the Carrie Bow Cay core encountered Pleistocene bedrock. Radiocarbon dating of a large head of Siderastrea siderea, growing on bedrock from the Carrie Bow Cay core at a depth of 15.04 m below sea level, gave an age of 6960±110 years. The leached calcitic coralline bedrock, at a depth of 15.7 m below sea level in the Carrie Bow Cay core, contained root marks, and iron staining indicative of subaerial exposure.

  14. 3. VIEW NORTHEAST OF PORT BOW OF JFK IN DRYDOCK ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    3. VIEW NORTHEAST OF PORT BOW OF JFK IN DRYDOCK NO. 5; PAINTERS WORKING APPLYING ANTI-FOULING PAINT BELOW WATER LINE. - Naval Base Philadelphia-Philadelphia Naval Shipyard, Dry Dock No. 5, League Island, Philadelphia, Philadelphia County, PA

  15. 3. CAP; CONICAL CAP HAS BOWED RAFTERS MORTISED INTO A ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    3. CAP; CONICAL CAP HAS BOWED RAFTERS MORTISED INTO A BOSS; ALSO SEEN ARE THE BRAKE WHEEL, WINDSHAFT AND TOP BEARING OF THE UPRIGHT SHAFT - Hayground Windmill, Windmill Lane, East Hampton, Suffolk County, NY

  16. Analysis of the Giacobini-Zinner bow wave

    SciTech Connect

    Smith, E.J.; Slavin, J.A.; Bame, S.J.; Thomsen, M.F.; Cowley, S.W.H.; Richardson, I.G.; Hovestadt, D.; Ipavich, F.M.; Ogilvie, K.W.; Coplan, M.A.

    1986-01-01

    The cometary bow wave of P/Giacobini-Zinner has been analyzed using the complete set of ICE field and particle observations to determine if it is a shock. Changes in the magnetic field and plasma flow velocities from upstream to downstream have been analyzed to determine the direction of the normal and the propagation velocity of the bow wave. The velocity has then been compared with the fast magnetosonic wave speed upstream to derive the Mach number and establish whether it is ''supersonic'', i.e., a shock, or ''subsonic,'' i.e., a large amplitude wave. The various measurements have also been compared with values derived from a Rankine-Hugoniot analysis. The results indicate that, inbound, the bow wave is a shock with M = 1.5. Outbound, a subsonic mach number is obtained, however, arguments are presented that the bow wave is also likely to be a shock at this location. 11 refs., 4 figs., 2 tabs.

  17. 46 CFR 154.1870 - Bow and stern loading.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... vapors with inert gas. (c) The person in charge of cargo transfer shall ensure that entrances, forced or... STANDARDS FOR SELF-PROPELLED VESSELS CARRYING BULK LIQUEFIED GASES Operations § 154.1870 Bow and...

  18. 15. Detail, northeast facade, operator's bow window and tower, showing ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    15. Detail, northeast facade, operator's bow window and tower, showing knee braces carried on stone ancons used to support eaves, view to northwest, 90mm lens. - Southern Pacific Depot, 559 El Camino Real, San Carlos, San Mateo County, CA

  19. 4. View of bow from port side, forward, vessel is ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    4. View of bow from port side, forward, vessel is on marine railway. Hooper Strait Lighthouse beyond. - Two-Sail Bateau E. C. COLLIER, Chesapeake Bay Maritime Museum, Mills Street, Saint Michaels, Talbot County, MD

  20. A comparative review of bow shocks and magnetopauses

    NASA Technical Reports Server (NTRS)

    Lepping, R. P.

    1984-01-01

    Bow shock and magnetopauses formation is discussed. Plasma and magnetic field environments of all the planets from Mercury to Saturn were measured. It was found that all the planets have bow shocks and almost all have a magnetopause. Venus is the only planet with no measurable intrinsic magnetic field and the solar wind interacts directly with Venus' ionosphere. The bow shock characteristics depend on the changing solar wind conditions. The shape of a magnetopause or any obstacle to flow depends on the three dimensional pressure profile that it presents to the solar wind. Jupiter is unusual because of the considerable amount of plasma which is contained in its magnetosphere. Magnetopause boundaries in ecliptic plane projection are modelled by segments of ellipses, matched to straight lines for the magnetotool boundaries or parabolas. Specific properties of known planetary bow shocks and magnetopauses are reviewed.

  1. 6. FORECASTLE DECK VIEW FROM PORT LOOKING FORWARD WITH BOW ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    6. FORECASTLE DECK VIEW FROM PORT LOOKING FORWARD WITH BOW DETAILS, CATHEAD FOR ANCHOR IN FOREGROUND, BOWSPRIT IN BACKGROUND. - Ship "Falls of Clyde", Hawaii Maritime Center,Pier 7, Honolulu, Honolulu County, HI

  2. Sub-10 nm nanoimprint lithography by wafer bowing.

    PubMed

    Wu, Wei; Tong, William M; Bartman, Jonathan; Chen, Yufeng; Walmsley, Robert; Yu, Zhaoning; Xia, Qiangfei; Park, Inkyu; Picciotto, Carl; Gao, Jun; Wang, Shih-Yuan; Morecroft, Deborah; Yang, Joel; Berggren, Karl K; Williams, R Stanley

    2008-11-01

    We introduce the concept of wafer bowing to affect nanoimprinting. This approach allows a design that can fit the key imprinting mechanism into a compact module, which we have constructed and demonstrated with an overlay and resolution of <0.5 microm and <10 nm, respectively. In the short term, this wafer bowing approach makes nanoimprint lithography much more accessible to a broad range of researchers. More importantly, this approach eliminates machine movement other than wafer bowing and shortens the mechanical path; these will enable the achievement of excellent patterning and overlay at a much lower cost. In the long term, wafer bowing is extensible to step-and-repeat printing for volume manufacturing.

  3. Analysis of the Giacobini-Zinner bow wave

    NASA Technical Reports Server (NTRS)

    Smith, E. J.; Slavin, J. A.; Bame, S. J.; Thomsen, M. F.; Cowley, S. W. H.; Richardson, I. G.; Hovestadt, D.; Ipavich, F. M.; Ogilvie, K. W.; Coplan, M. A.

    1986-01-01

    The cometary bow wave of P/Giacobini-Zinner has been analyzed using the complete set of ICE field and particle observations to determine if it is a shock. Changes in the magnetic field and plasma flow velocities from upstream to downstream have been analyzed to determine the direction of the normal and the propagation velocity of the bow wave. The velocity has then been compared with the fast magnetosonic wave speed upstream to derive the Mach number and establish whether it is supersonic, i.e., a shock, or subsonic, i.e., a large amplitude wave. The various measurements have also been compared with values derived from a Rankine-Hugoniot analysis. The results indicate that, inbound, the bow wave is a shock with M = 1.5. Outbound, a subsonic Mach number is obtained, however, arguments are presented that the bow wave is also likely to be a shock at this location.

  4. 17. SAME ROOMVIEW SOUTH TOWARDS TWO SKIFFS UNDER CONSTRUCTION (BOW ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    17. SAME ROOM-VIEW SOUTH TOWARDS TWO SKIFFS UNDER CONSTRUCTION (BOW VIEW SHOWING CLAMPING JIG MOUNTED TO BEAMS ABOVE/PROFILE VIEW IN BACKGROUND SHOWING JIG). - Lowell's Boat Shop, 459 Main Street, Amesbury, Essex County, MA

  5. 17. DECK ABOVE CO'S STATEROOM, LOOKING TOWARDS BOW AT DECK ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    17. DECK ABOVE CO'S STATEROOM, LOOKING TOWARDS BOW AT DECK ABOVE PILOT HOUSE. - U.S. Coast Guard Cutter WHITE HEATH, USGS Integrated Support Command Boston, 427 Commercial Street, Boston, Suffolk County, MA

  6. 18. DECK ABOVE PILOT HOUSE, LOOKING TOWARDS BOW, SHOWING DETAIL, ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    18. DECK ABOVE PILOT HOUSE, LOOKING TOWARDS BOW, SHOWING DETAIL, OF MAST. - U.S. Coast Guard Cutter WHITE HEATH, USGS Integrated Support Command Boston, 427 Commercial Street, Boston, Suffolk County, MA

  7. 15. PORT SIDE OF FLYBRIDGE WING, LOOKING TOWARDS BOW AT ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    15. PORT SIDE OF FLYBRIDGE WING, LOOKING TOWARDS BOW AT SHIP'S CONTROLS AND IN BACKGROUND IS COMPASS. - U.S. Coast Guard Cutter WHITE HEATH, USGS Integrated Support Command Boston, 427 Commercial Street, Boston, Suffolk County, MA

  8. VIEW EAST SHOWING THE WEST SIDE OF THE FORWARD (BOW) ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    VIEW EAST SHOWING THE WEST SIDE OF THE FORWARD (BOW) SECTION - Rosie the Riveter National Historical Park, Rosie the Riveter Memorial, Off Regatta at Melville Square in Marina Park, Richmond, Contra Costa County, CA

  9. VIEW SOUTH FROM WITHING THE FORWARD (BOW) SECTION Rosie ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    VIEW SOUTH FROM WITHING THE FORWARD (BOW) SECTION - Rosie the Riveter National Historical Park, Rosie the Riveter Memorial, Off Regatta at Melville Square in Marina Park, Richmond, Contra Costa County, CA

  10. VIEW SOUTH SHOWING THE STRUCTURE REPRESENTING THE FORWARD (BOW) SECTION ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    VIEW SOUTH SHOWING THE STRUCTURE REPRESENTING THE FORWARD (BOW) SECTION OF A LIBERTY SHIP - Rosie the Riveter National Historical Park, Rosie the Riveter Memorial, Off Regatta at Melville Square in Marina Park, Richmond, Contra Costa County, CA

  11. Can Porphyritic Chondrules Form in Planetary Embryo Bow Shocks?

    NASA Astrophysics Data System (ADS)

    Perez, A. M.; Desch, S. J.; Schrader, D. L.; Till, C. B.

    2017-05-01

    This work investigates the validity of planetary embryo bow shocks as a possible chondrule formation mechanism. We have conducted experiments to test whether cooling rates > 3000 K/hr can yield porphyritic textures.

  12. 19. DETAIL VIEW OF SKIFF BOW WITH OAK STEM AND ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    19. DETAIL VIEW OF SKIFF BOW WITH OAK STEM AND FRAMES PLANKED IN CEDAR USING COPPER CLINCH NAILS. TRANSOM OF SECOND SKIFF CAN BE SEEN BACKGROUND. - Lowell's Boat Shop, 459 Main Street, Amesbury, Essex County, MA

  13. 6. VIEW OF BOW OF VESSEL FROM STARBOARD SIDE, SHOWING ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    6. VIEW OF BOW OF VESSEL FROM STARBOARD SIDE, SHOWING DOCKING CREW PREPARING TO REMOVE FOREFOOT FROM VESSEL'S STEM IN ORDER TO DRAW VESSEL OFF LIFT DOCK - Bugeye "Louise Travers", Intersection of Routes 2 & 4, Solomons, Calvert County, MD

  14. Femoral bowing plane adaptation to femoral anteversion

    PubMed Central

    Akman, Alp; Demirkan, Fahir; Sabir, Nuran; Oto, Murat; Yorukoglu, Cagdas; Kiter, Esat

    2017-01-01

    Background: Femoral bowing plane (FBP) is the unattended subject in the literature. More over the femoral shaft with its bowing is neglected in established anteversion determination methods. There is limited information about the relationship between FBP and anteversion. Thus we focused on this subject and hypothesized that there could be an adaptation of FBP to anteversion. Materials and Methods: FBP is determined on three-dimensional solid models derived from the left femoral computerized tomography data of 47 patients which were taken before for another reason and comparatively evaluated with anteversion. There were 20 women and 27 men. The mean age of patients was 56 years (range 21–84 years). Results: The anteversion values were found as the angle between a distal condylar axis (DCA) and femoral neck anteversion axis (FNAA) along an imaginary longitudinal femoral axis (LFA) in the true cranio-caudal view. The FBP was determined as a plane that passes through the centre-points of three pre-determinated sections on the femoral shaft. The angles between DCA, FNAA and FBP were comparatively evaluated. The independent samples t-test was used for statistical analysis. At the end, it was found that FBP lies nearly perpendicular to the anteversion axis for the mean of our sample which is around 89° in females and 93° in males (range 78–102°). On the other hand, FBP does not lie close to the sagittal femoral plane (SFP); instead, there is an average 12.5° external rotation relative to the SFP. FBP is correlated well with anteversion in terms of FBP inclination from SFP and femoral torsion (i.e., angle between FBP and femoral neck anteversion axis (P < 0.001; r = 0.680 and r = −0.682, respectively). Combined correlation is perfect (R2 = 1) as the FBP, SFP, and posterior femoral plane forms a triangle in the cranio-caudal view. Conclusions: We found that FBP adapts to anteversion. As FBP lies close to perpendicularity for the mean, femoral component positioning

  15. Tibial Bowing and Pseudarthrosis in Neurofibromatosis Type 1

    DTIC Science & Technology

    2013-04-01

    observed in 5% of children with neurofibromatosis type 1 ( NF1 ), typically identified in infancy. The majority of NF1 individuals with tibial bowing...will sustain a fracture that will not heal (i.e. pseudarthrosis) resulting in multiple surgeries, poor limb function, and amputation. Some NF1 ...pseudarthrosis and better understand its pathophysiology. We have begun recruitment and assessed many individuals with NF1 with and with tibial bowing. QUS

  16. 76. The Silver Bow County Courthouse, 19101912, at West Granite ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    76. The Silver Bow County Courthouse, 1910-1912, at West Granite and Montana Streets, was designed by Link and Haire. The building has a dressed sandstone foundation, brick walls, and sandstone trim, parapet and columns. It was used as a barracks for the State militia when the city was placed under martial law following the dynamiting of the Old Miners' Union Hall in September, 1914. - Butte Historic District, Bounded by Copper, Arizona, Mercury & Continental Streets, Butte, Silver Bow County, MT

  17. Tibial Bowing and Pseudarthrosis in Neurofibromatosis Type 1

    DTIC Science & Technology

    2014-04-01

    bowed tibia. We have extracted DNA from peripheral blood of all individuals with tibial bowing and will continue to monitor them for development of...to improve bone quality prior to fracture in a non-invasive and age specific manner • DNA extraction from peripheral blood for somatic mutation...Johnson B, Rauen KA. Peripheral muscle weakness in RASopathies. Oral presentation at the Western Society for Pediatric Research, Carmel, California

  18. Mesoscale Surface Pressure and Temperature Features Associated with Bow Echoes

    DTIC Science & Technology

    2010-01-01

    contain several bowing segments. These multiple segments could occur at the same time and be located within the same bow, such as the serial derecho ...Examination of derecho environments using proximity soundings. Wea. Forecasting, 16, 329–342. Fovell, R. G., 2002: Upstream influence of numerically...Se- vere Local Storms, Hyannis, MA, Amer. Meteor. Soc., 4.6. Johns, R. H., and W. D. Hirt, 1987: Derechos : Widespread con- vectively induced

  19. Coordination of bowing and fingering in violin playing.

    PubMed

    Baader, Andreas P; Kazennikov, Oleg; Wiesendanger, Mario

    2005-05-01

    Playing string instruments implies motor skills including asymmetrical interlimb coordination. How special is musical skill as compared to other bimanually coordinated, non-musical skillful performances? We succeeded for the first time to measure quantitatively bimanual coordination in violinists playing repeatedly a simple tone sequence. A motion analysis system was used to record finger and bow trajectories for assessing the temporal structure of finger-press, finger-lift (left hand), and bow stroke reversals (right arm). The main results were: (1) fingering consisted of serial and parallel (anticipatory) mechanisms; (2) synchronization between finger and bow actions varied from -12 ms to 60 ms, but these 'errors' were not perceived. The results suggest that (1) bow-finger synchronization varied by about 50 ms from perfect simultaneity, but without impairing auditory perception; (2) the temporal structure depends on a number of combinatorial mechanisms of bowing and fingering. These basic mechanisms were observed in all players, including all amateurs. The successful biomechanical measures of fingering and bowing open a vast practical field of assessing motor skills. Thus, objective assessment of larger groups of string players with varying musical proficiency, or of professional string players developing movement disorders, may be helpful in music education.

  20. Extreme ultraviolet spectroscopy of PKS 2155-304.

    PubMed

    Fruscione, A; Bowyer, S; Konigl, A; Kahn, S M

    1994-02-20

    We present the extreme ultraviolet (75-110 angstroms) spectrum of the BL Lac object PKS 2155-304, the first spectrum of an extragalactic source obtained with the Extreme Ultraviolet Explorer. The spectrum shows a generally smooth continuum, which can be modeled by a single power law plus interstellar absorption, and possibly an absorption feature at approximately 80 angstroms. The best fit to the data suggests that the EUV spectrum can be interpreted as a simple extrapolation of the X-ray continuum, with an energy index alpha approximately 1.6; however, shallower or steeper power laws with indices between -0.4 and 2.7 cannot be ruled out by the existing EUV data alone. The data provide strong constraints on the interstellar neutral H and He along the line of sight. Using a column density of 1.36 x 10(20) cm-2 for the Galactic neutral hydrogen along the PKS 2155-304 line of sight, the neutral helium column density is constrained to be 9%-10% of the hydrogen amount.

  1. CRTS detection of optical outburst of PKS 2023-07

    NASA Astrophysics Data System (ADS)

    Mahabal, A. A.; Djorgovski, S. G.; Drake, A. J.; Graham, M. J.; Williams, R.; Catelan, M.; Beshore, E. C.; Larson, S. M.; Christensen, E.

    2009-08-01

    We report on the discovery of an optical outburst associated with PKS 2023-07 by the Catalina Real-Time Transient Survey (CRTS). Recently, Gasparrini et al. ATel#2175 noted the Fermi LAT detection of a GeV flare from blazar PKS 2023-07. On Aug 29.17 UT CRTS automatically detected and alerted that this object was undergoing a significant optical outburst with V~15.2.

    ID Detection DateRADecMagVOEvent ID
    CSS090829:202541-073553 2009-08-29 UT 04:15:36 20:25:40.63-07:35:52.7 15.2 908290071094126135
    Past photometry dating back to April 2005 suggests that this blazar is highly variable often showing wild variations in brightness over relatively short periods, and is in that sense unlike most blazars.

  2. 75 FR 40820 - City of Broken Bow, Oklahoma; Project No. 12470-001-Oklahoma Broken Bow Re-Regulation Dam...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-07-14

    ... Managing Properties Included in or Eligible for Inclusion in the National Register of Historic Places July... included in, or eligible for inclusion in, the National Register of Historic Places at the Broken Bow Re...

  3. CT analysis of bowed stringed instruments.

    PubMed

    Sirr, S A; Waddle, J R

    1997-06-01

    To determine the utility of computed tomography (CT) for the noninvasive evaluation of bowed stringed instruments. Thirty-seven instruments that ranged in quality from student instruments to exquisite Stradivarius violins were analyzed with CT. Accuracy of thickness measurements was determined from 24 measurements of cross-sectional pieces sawed from a student violin. Accuracy of density measurements was determined from 328 CT attenuation measurements of 16 woods used in stringed instruments. Substantial differences of normal structure were noted between the masterpieces crafted in Cremona, Italy, and factory-produced student instruments. Unexpected defects were detected in nine of 14 instruments older than 100 years and ranged from a few wormholes (eight instruments) to many wormholes and extensive repair (one violin). CT thickness and attenuation measurements correlated well to the line of identity with actual measurements (P < .0001). Two cellos and a viola have been constructed from CT-derived information. The viola was awarded a gold medal at a recent international competition. CT provides the modern luthier and acoustic scientist with a unique tool for characterization of normal structure, defects, and repair and for accurate measurements of wood thickness and density. CT-derived information aids in the replication of original masterpieces. CT evaluation may have an important role in the valuation, insurance, and identification of valuable stringed instruments.

  4. Antituberculosis thiophenes define a requirement for Pks13 in mycolic acid biosynthesis

    PubMed Central

    Wilson, Regina; Kumar, Pradeep; Parashar, Vijay; Vilchèze, Catherine; Veyron-Churlet, Romain; Freundlich, Joel S.; Barnes, S. Whitney; Walker, John R.; Szymonifka, Michael J.; Marchiano, Emily; Shenai, Shubhada; Colangeli, Roberto; Jacobs, William R.; Neiditch, Matthew B.; Kremer, Laurent

    2013-01-01

    We report a new class of thiophene (TP) compounds that kill Mycobacterium tuberculosis (Mtb) by the novel mechanism of Pks13 inhibition. An F79S mutation near the catalytic Ser-55 site in Pks13 conferred TP-resistance in Mtb. Over-expression of wild-type pks13 resulted in TP-resistance and over-expression of the F79S pks13 mutant conferred high-level resistance. In vitro, TP inhibited fatty acyl-AMP loading onto Pks13. TP inhibited mycolic acid biosynthesis in wild-type Mtb, but to a much lesser extent in TP-resistant Mtb. TP treatment was bactericidal and equivalent to the first-line drug isoniazid, but it was less likely to permit emergent resistance. Combined isoniazid and TP treatment exhibited sterilizing activity. Computational-docking identified a possible TP-binding groove within the Pks13 ACP domain. This study confirms that Mtb Pks13 is required for mycolic acid biosynthesis, validates it as a druggable target and demonstrates the therapeutic potential of simultaneously inhibiting multiple targets in the same biosynthetic pathway. PMID:23770708

  5. PKS1 plays a role in red-light-based positive phototropism in roots.

    PubMed

    Molas, Maria Lia; Kiss, John Z

    2008-06-01

    Aerial parts of plants curve towards the light (i.e. positive phototropism), and roots typically grow away from the light (i.e. negative phototropism). In addition, Arabidopsis roots exhibit positive phototropism relative to red light (RL), and this response is mediated by phytochromes A and B (phyA and phyB). Upon light stimulation, phyA and phyB interact with the phytochrome kinase substrate (PKS1) in the cytoplasm. In this study, we investigated the role of PKS1, along with phyA and phyB, in the positive phototropic responses to RL in roots. Using a high-resolution feedback system, we studied the phenotypic responses of roots of phyA, phyB, pks1, phyA pks1 and phyB pks1 null mutants as well as the PKS1-overexpressing line in response to RL. PKS1 emerged as an intermediary in the signalling pathways and appears to promote a negative curvature to RL in roots. In addition, phyA and phyB were both essential for a positive response to RL and act in a complementary fashion. However, either photoreceptor acting without the other results in negative curvature in response to red illumination so that the mode of action differs depending on whether phyA and phyB act independently or together. Our results suggest that PKS1 is part of a signalling pathway independent of phyA and phyB and that PKS1 modulates RL-based root phototropism.

  6. Linear modal stability analysis of bowed-strings.

    PubMed

    Debut, V; Antunes, J; Inácio, O

    2017-03-01

    Linearised models are often invoked as a starting point to study complex dynamical systems. Besides their attractive mathematical simplicity, they have a central role for determining the stability properties of static or dynamical states, and can often shed light on the influence of the control parameters on the system dynamical behaviour. While the bowed string dynamics has been thoroughly studied from a number of points of view, mainly by time-domain computer simulations, this paper proposes to explore its dynamical behaviour adopting a linear framework, linearising the friction force near an equilibrium state in steady sliding conditions, and using a modal representation of the string dynamics. Starting from the simplest idealisation of the friction force given by Coulomb's law with a velocity-dependent friction coefficient, the linearised modal equations of the bowed string are presented, and the dynamical changes of the system as a function of the bowing parameters are studied using linear stability analysis. From the computed complex eigenvalues and eigenvectors, several plots of the evolution of the modal frequencies, damping values, and modeshapes with the bowing parameters are produced, as well as stability charts for each system mode. By systematically exploring the influence of the parameters, this approach appears as a preliminary numerical characterisation of the bifurcations of the bowed string dynamics, with the advantage of being very simple compared to sophisticated numerical approaches which demand the regularisation of the nonlinear interaction force. To fix the idea about the potential of the proposed approach, the classic one-degree-of-freedom friction-excited oscillator is first considered, and then the case of the bowed string. Even if the actual stick-slip behaviour is rather far from the linear description adopted here, the results show that essential musical features of bowed string vibrations can be interpreted from this simple approach

  7. Numerical simulations of Mach stem formation via intersecting bow shocks

    NASA Astrophysics Data System (ADS)

    Hansen, E. C.; Frank, A.; Hartigan, P.; Yirak, K.

    2015-12-01

    Hubble Space Telescope observations show bright knots of Hα emission within outflowing young stellar jets. Velocity variations in the flow create secondary bow shocks that may intersect and lead to enhanced emission. When the bow shocks intersect at or above a certain critical angle, a planar shock called a Mach stem is formed. These shocks could produce brighter Hα emission since the incoming flow to the Mach stem is parallel to the shock normal. In this paper we report first results of a study using 2-D numerical simulations designed to explore Mach stem formation at the intersection of bow shocks formed by hypersonic ;bullets; or ;clumps;. Our 2-D simulations show how the bow shock shapes and intersection angles change as the adiabatic index γ changes. We show that the formation or lack of a Mach stem in our simulations is consistent with the steady-state Mach stem formation theory. Our ultimate goal, which is part of an ongoing research effort, is to characterize the physical and observational consequences of bow shock intersections including the formation of Mach stems.

  8. Social complexity and the bow in the Eastern Woodlands.

    PubMed

    Blitz, John H; Porth, Erik S

    2013-01-01

    Bingham and Souza have presented an evolutionary theory that specifies a causal relationship between the advent of powerful projectile weapons such as the bow and radical rearrangements in social relations and histories. They propose that the acquisition of weapons that permitted humans to kill at ever-increasing distances provided the coercive means to suppress conflicts of interest among nonkin, self-interested individuals in social groups, thus paving the way for greater social complexity. An unprecedented reduction in projectile point size identifies the arrival of the bow ca. A.D. 300 in the Eastern Woodlands of North America, which initiated a causal chain of cultural changes. In the Midwest, the bow, combined with food production, precipitated the decline of Hopewell by conferring household autonomy and dispersal, which at first suppressed social complexity, but later created conditions favorable to maize intensification. In the lower Southeast, where food production was unimportant, populations aggregated at concentrated wild-food sources, and the bow did not confer household autonomy. The relationship between the bow and social complexity varied under different environmental, social, and historical conditions.

  9. Bow-tie diagrams for risk management in anaesthesia.

    PubMed

    Culwick, M D; Merry, A F; Clarke, D M; Taraporewalla, K J; Gibbs, N M

    2016-11-01

    Bow-tie analysis is a risk analysis and management tool that has been readily adopted into routine practice in many high reliability industries such as engineering, aviation and emergency services. However, it has received little exposure so far in healthcare. Nevertheless, its simplicity, versatility, and pictorial display may have benefits for the analysis of a range of healthcare risks, including complex and multiple risks and their interactions. Bow-tie diagrams are a combination of a fault tree and an event tree, which when combined take the shape of a bow tie. Central to bow-tie methodology is the concept of an undesired or 'Top Event', which occurs if a hazard progresses past all prevention controls. Top Events may also occasionally occur idiosyncratically. Irrespective of the cause of a Top Event, mitigation and recovery controls may influence the outcome. Hence the relationship of hazard to outcome can be viewed in one diagram along with possible causal sequences or accident trajectories. Potential uses for bow-tie diagrams in anaesthesia risk management include improved understanding of anaesthesia hazards and risks, pre-emptive identification of absent or inadequate hazard controls, investigation of clinical incidents, teaching anaesthesia risk management, and demonstrating risk management strategies to third parties when required.

  10. Egret detection of the blazar PKS 0420-014

    NASA Technical Reports Server (NTRS)

    Radecke, H.-D.; Bertsch, D. L.; Dingus, B. L.; Fichtel, C. E.; Hartman, R. C.; Hunter, S. D.; Kanbach, G.; Kniffen, D. A.; Lin, Y. C.; Mattox, J. R.

    1995-01-01

    During its full-sky survey, the Energetic Gamma Ray Experiment Telescope (EGRET) high-energy instrument aboard the Compton Gamma-Ray Observatory detected gamma-ray emission in the energy range above 30 MeV from a source identified as the blazar PKS 0420-014. This object was observed during two separate viewing periods in 1992 February/March and May/June. An intensity decrease above 100 MeV of a factor of at least 1.5 from a maximum of (5.0 +/- 1.4) x 10(exp -7) photons 1 sq cm/s was observed during that time interval indicating extensive variability. The photon spectrum in the range between 30 and 10,000 MeV at the time of the maximum intensity is well represented by a power law with an exponent of -1.9 +/- 0.3. Some similarities with other EGRET detected blazars are briefly discussed.

  11. Egret detection of the blazar PKS 0420-014

    NASA Technical Reports Server (NTRS)

    Radecke, H.-D.; Bertsch, D. L.; Dingus, B. L.; Fichtel, C. E.; Hartman, R. C.; Hunter, S. D.; Kanbach, G.; Kniffen, D. A.; Lin, Y. C.; Mattox, J. R.

    1995-01-01

    During its full-sky survey, the Energetic Gamma Ray Experiment Telescope (EGRET) high-energy instrument aboard the Compton Gamma-Ray Observatory detected gamma-ray emission in the energy range above 30 MeV from a source identified as the blazar PKS 0420-014. This object was observed during two separate viewing periods in 1992 February/March and May/June. An intensity decrease above 100 MeV of a factor of at least 1.5 from a maximum of (5.0 +/- 1.4) x 10(exp -7) photons 1 sq cm/s was observed during that time interval indicating extensive variability. The photon spectrum in the range between 30 and 10,000 MeV at the time of the maximum intensity is well represented by a power law with an exponent of -1.9 +/- 0.3. Some similarities with other EGRET detected blazars are briefly discussed.

  12. Time delay in the Einstein ring PKS 1830-211

    NASA Technical Reports Server (NTRS)

    Van Ommen, T. D.; Jones, D. L.; Preston, R. A.; Jauncey, D. L.

    1995-01-01

    We present radio observations of the gravitational lens PKS 1830-211 at 8.4 and 15 GHz acquired using the Very Large Array. The observations were made over a 13 month period. Significant flux density changes over this period provide strong constraints on the time delay between the two lensed images and suffest a value of 44 +/- 9 days. This offers new direct evidence that this source is indeed a gravitational lens. The lens distance is dependent upon the model chosen, but reasonable limits on the mass of the lensing galaxy suggest that it is unlikely to be at a redshift less than a few tenths, and may well be significantly more distant.

  13. Multifrequency observations of the BL Lacertae object PKS 0537 - 441

    NASA Technical Reports Server (NTRS)

    Maraschi, L.; Treves, A.; Schwartz, D. A.; Tanzi, E. G.

    1985-01-01

    PKS 0537 - 441 was repeatedly observed in the UV band with the International Ultraviolet Explorer and in the X-ray with the Einstein Observatory. On September 27, 1980, simultaneous observations in the two bands were obtained. Near-infrared photometry preceding and following the simultaneous observations by about one month is available from the literature, as is radio monitoring at 408 and 5000 MHz. Comparison of the observed X-ray flux with that predicted by the standard synchrotron self-Compton formalism, with a source dimension deduced from radio variability at 5 GHz, indicates that this component of the radio emission must be moving at relativistic speed with an effective projected Doppler beaming factor of about 10.

  14. Renewed Gamma-Ray Emission from the blazar PKS 1510-089 Detected by AGILE

    NASA Astrophysics Data System (ADS)

    Munar-Adrover, P.; Pittori, C.; Bulgarelli, A.; Lucarelli, F.; Verrecchia, F.; Piano, G.; Fioretti, V.; Zoli, A.; Tavani, M.; Vercellone, S.; Minervini, G.; Striani, E.; Cardillo, M.; Gianotti, F.; Trifoglio, M.; Giuliani, A.; Mereghetti, S.; Caraveo, P.; Perotti, F.; Chen, A.; Argan, A.; Costa, E.; Del Monte, E.; Donnarumma, I.; Evangelista, Y.; Feroci, M.; Lazzarotto, F.; Lapshov, I.; Pacciani, L.; Soffitta, P.; Sabatini, S.; Vittorini, V.; Pucella, G.; Rapisarda, M.; Di Cocco, G.; Fuschino, F.; Galli, M.; Labanti, C.; Marisaldi, M.; Pellizzoni, A.; Pilia, M.; Trois, A.; Barbiellini, G.; Vallazza, E.; Longo, F.; Morselli, A.; Picozza, P.; Prest, M.; Lipari, P.; Zanello, D.; Cattaneo, P. W.; Rappoldi, A.; Colafrancesco, S.; Parmiggiani, N.; Ferrari, A.; Antonelli, A.; Giommi, P.; Salotti, L.; Valentini, G.; D'Amico, F.

    2016-09-01

    AGILE is currently detecting enhanced gamma-ray emission above 100 MeV from a source which position is consistent with the blazar PKS 1510-089. (the last activity of this source was reported in ATel #9350).

  15. Pallister-Killian Syndrome (PKS) as a Cause of Mental Retardation.

    PubMed

    Shamdeen, A; Meyer, S; Gottschling, S; Oehl-Jaschkowitz, B; Gortner, L; Shamdeen, M G

    2009-01-01

    Pallister-Killian syndrome (PKS; OMIM: # 601803) is a rare sporadic syndrome of multiple congenital anomalies attributable to the presence of a de novo mosaic supernumerary isochromosome 12p [i(12p)]. The syndrome presents with a recognizable pattern of findings including: pigmentary skin changes, characteristic facial features (sparse anterior scalp hair, flattened midface, macrostomia, and coarsening of the facial features), and developmental delay. The developmental phenotype of PKS is quite variable, but most are considered to fall into the profound range of developmental retardation. We report on two individuals with classical features of PKS. Notably, in one child the neuropsychological development was significantly more favourable than commonly reported in the literature. This illustrates the loose correlation between geno- and phenotype in PKS.

  16. Bright optical flare in Gamma-source PKS 1510-089

    NASA Astrophysics Data System (ADS)

    Jankowsky, F.; Mohamed, M.; Schwemmer, S.; Wagner, S.; Zacharias, M.

    2016-09-01

    Optical observations of the VHE gamma-ray bright, flat-spectrum radio quasar PKS 1510-089 (z=0.36) with the Automatic Telescope for Optical Monitoring (ATOM) in Namibia reveal a significant brightening.

  17. Electrostatic waves in the bow shock at Uranus

    SciTech Connect

    Moses, S.L.; Coroniti, F.V.; Kennel, C.F.; Scarf, F.L. ); Bagenal, F. ); Lepping, R.P. ); Quest, K.B. ); Kurth, W.S. )

    1989-10-01

    Electrostatic emissions measured by the Voyager 2 plasma wave detector (PWS) during the inbound crossing of the Uranian bow shock are shown to differ in some aspects from the waves measured during bow shock crossings at Jupiter and Saturn. The wave amplitudes in the foot of the bow shock at Uranus are in general much lower than those detected at the other out planets due to the unusually enhanced solar wind ion temperature during the crossing. This reduces the effectiveness of wave-particle interactions in heating the incoming electrons. Strong wave emissions are observed in the shock ramp that possibly arise from currents producing a Buneman mode instability. Plasma instrument (PLS) and magnetometer (MAG) measurements reveal a complicated shock structure reminiscent of computer simulations of high-Mach number shocks when the effects of anomalous resistivity are reduced, and are consistent with high ion temperatures restricting the growth of electrostatic waves.

  18. Featured Image: A Search for Stellar Bow Shock Nebulae

    NASA Astrophysics Data System (ADS)

    Kohler, Susanna

    2017-02-01

    These dynamic infrared images (click for the full view!) reveal what are known as bow shock nebulae nebulae that form at the interface between the interstellar medium and the stellar wind from a high-speed star zipping through the galaxy (the arrows show the direction of motion of the star). When the relative speed between the two is supersonic, an arc-shaped bow shock forms ahead of the star, like the six prototypical ones pictured here. A team of scientists led by Henry Kobulnicky (University of Wyoming) has recently searched through survey data from the Spitzer Space Telescope and the Wide Field Infrared Explorer (WISE) to build a catalog of more than 700 such bow-shock nebula candidates, the vast majority of which are new discoveries. To find out more about their sample, check out the paper below!CitationHenry A. Kobulnicky et al 2016 ApJS 227 18. doi:10.3847/0067-0049/227/2/18

  19. Foreshock ions observed behind the Martian bow shock

    NASA Astrophysics Data System (ADS)

    Frahm, R. A.; Yamauchi, M.; Winningham, J. D.; Lundin, R.; Sharber, J. R.; Nilsson, H.; Coates, A. J.

    2016-08-01

    The Mars Express Analyzer of Space Plasmas and Energetic Atoms experiment contains ion and electron instruments for conducting plasma measurements. On January 23, 2012, during in-bound travel of Mars Express in the southern hemisphere of Mars from its dawn side toward periapsis at dusk, the plasma instruments measured foreshock-like ion beams extending from outside the bow shock and into the magnetosphere, continuing to a distance of about a proton gyroradius from the bow shock. These ion beams were mostly protons, were observed to have energies greater than solar wind protons, and were not gyrating, in agreement with reflections of the solar wind proton beam. Furthermore, in the foreshock region the ion energy gradually decreased toward the magnetosheath, in agreement with an acceleration by outward-directed electric field in the bowshock. The observations also suggest that this electric field exists even inside the magnetosheath within the distance of a proton gyroradius from the bow shock.

  20. [Correction of bowing in Paget's disease (author's transl)].

    PubMed

    Postel, M; Senly, G

    1978-12-01

    Thirteen tibiae and seven femora suffering from bowing due to Paget's disease have been streightened operatively. In the tibiae, the deformities were of metaphysial genu varum with bowing in the sagittal plane of an average of 30 degrees combined with some medial rotation. In the femora, the main curve was anterolateral with some medial rotation and coxa vara. Seventeen cases united uneventfully after osteotomy. In three cases, there were septic complications, union occurred after removal of the internal fixation. Bowing recurred in three cases. The recurrence appeared to be related to incomplete correction leading to persistent mechanical strain on bones affected by rapid bone turnover. Inadequate internal fixation may also be a factor. All other cases were functionally improved by correction. Oblique osteotomy is indicated for the correction of tibial deformity when there is moderate medial rotation. Transverse osteotomy with fixation by intramedullary nailing is indicated for correction of femoral deformities.

  1. Bow and Oblique Shock Formation in Soap Film

    NASA Astrophysics Data System (ADS)

    Kim, Ildoo; Mandre, Shreyas; Sane, Aakash

    2015-11-01

    In recent years, soap films have been exploited primarily to approximate two-dimensional flows while their three-dimensional character is relatively unattended. An example of the three-dimensional character of the flow in a soap film is the observed Marangoni shock wave when the flow speed exceeds the wave speed. In this study, we investigated the formation of bow and oblique shocks in soap films generated by wedges with different deflection angles. When the wedge deflection angle is small and the film flows fast, oblique shocks are observed. When the oblique shock cannot exists, bow shock is formed upstream the wedge. We characterized the oblique shock angle as a function of the wedge deflection angle and the flow speed, and we also present the criteria for transition between bow and oblique Marangoni shocks in soap films.

  2. EVAPORATION OF ICY PLANETESIMALS DUE TO BOW SHOCKS

    SciTech Connect

    Tanaka, Kyoko K.; Yamamoto, Tetsuo; Tanaka, Hidekazu; Miura, Hitoshi; Nagasawa, Makiko; Nakamoto, Taishi

    2013-02-20

    We present the novel concept of evaporation of planetesimals as a result of bow shocks associated with planetesimals orbiting with supersonic velocities relative to the gas in a protoplanetary disk. We evaluate the evaporation rates of the planetesimals based on a simple model describing planetesimal heating and evaporation by the bow shock. We find that icy planetesimals with radius {approx}>100 km evaporate efficiently even outside the snow line in the stage of planetary oligarchic growth, where strong bow shocks are produced by gravitational perturbations from protoplanets. The obtained results suggest that the formation of gas giant planets is suppressed owing to insufficient accretion of icy planetesimals onto the protoplanet within the {approx}<5 AU disk region.

  3. PksS from Bacillus subtilis is a cytochrome P450 involved in bacillaene metabolism

    SciTech Connect

    Reddick, Jason J. . E-mail: jjreddic@uncg.edu; Antolak, Stephanie A.; Raner, Gregory M.

    2007-06-22

    As part of the pksX gene cluster of Bacillus subtilis strain 168, pksS has been preliminarily annotated as a cytochrome P450 homolog that hydroxylates the polyketide product of this cluster, which was recently shown to be involved in the biosynthesis of bacillaene and dihydrobacillaene. Here we report that there is a frame-shift error in the reported sequence for pksS, and that we have successfully cloned, overexpressed, and purified the protein encoded by the corrected sequence. By utilizing electronic absorption spectrophotometry, we have observed that the ferrous CO complex of PksS absorbs maximally near 450 nm, which confirms the annotation that this protein is a cytochrome P450. We have also established a cell-free system derived from crude cytosolic B. subtilis protein extracts which provides reductase activity essential to sustaining the putative catalytic cycle of PksS. Using LC-MS analysis we have collected data which suggests that the substrate for PksS is dihydrobacillaene.

  4. Polarization Signatures of Bow Shocks in Stellar Winds

    NASA Astrophysics Data System (ADS)

    Shrestha, M.; Hoffman, J. L.

    2015-12-01

    Bow shocks around massive stars provide important information regarding the motion of the star, the stellar wind properties, and the density of the surrounding interstellar medium. We use a Monte Carlo radiative transfer code to investigate the polarization created when photons from a central star scatter from electrons or dust grains in a surrounding bow shock. We discuss the behavior of the polarization with respect to viewing angle as a function of parameters such as optical depth and scattering medium in both the resolved and unresolved cases.

  5. 76 FR 13666 - Pitney Bowes, Inc., Mailing Solutions Management, Global Engineering Group, Including On-Site...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-03-14

    ... Solutions Management Division, Engineering Quality Assurance, Shelton, Connecticut. The Department's Notice... Employment and Training Administration Pitney Bowes, Inc., Mailing Solutions Management, Global Engineering... firm worker group should read: Pitney Bowes, Inc., Mailing Solutions Management, Global...

  6. 26 CFR 48.4161(b)-1 - Imposition and rates of tax; bows and arrows.

    Code of Federal Regulations, 2011 CFR

    2011-04-01

    ... 26 Internal Revenue 16 2011-04-01 2011-04-01 false Imposition and rates of tax; bows and arrows... § 48.4161(b)-1 Imposition and rates of tax; bows and arrows. (a) Imposition of tax. Section 4161(b...) Any bow that has a draw weight of 10 pounds or more; (2) Any arrow that measures 18 inches overall or...

  7. 26 CFR 48.4161(b)-1 - Imposition and rates of tax; bows and arrows.

    Code of Federal Regulations, 2013 CFR

    2013-04-01

    ... 26 Internal Revenue 16 2013-04-01 2013-04-01 false Imposition and rates of tax; bows and arrows... § 48.4161(b)-1 Imposition and rates of tax; bows and arrows. (a) Imposition of tax. Section 4161(b...) Any bow that has a draw weight of 10 pounds or more; (2) Any arrow that measures 18 inches overall or...

  8. 26 CFR 48.4161(b)-1 - Imposition and rates of tax; bows and arrows.

    Code of Federal Regulations, 2012 CFR

    2012-04-01

    ... 26 Internal Revenue 16 2012-04-01 2012-04-01 false Imposition and rates of tax; bows and arrows... § 48.4161(b)-1 Imposition and rates of tax; bows and arrows. (a) Imposition of tax. Section 4161(b...) Any bow that has a draw weight of 10 pounds or more; (2) Any arrow that measures 18 inches overall or...

  9. Forces and the Potential Energy Function for a Bow-and-Arrow System

    NASA Astrophysics Data System (ADS)

    Taylor, Ken; Coutant, Blaine; Crow, Tatum; James, Austin

    2008-03-01

    The experiments described here consist of a series of investigations into the dynamics of a bow as it is bent (and released) under the influence of a stretched string. The bow is ``student-friendly'' and has no pulleys for facilitating stretch. The presentation will discuss the various approaches to characterizing the bow, the string, and its energy efficiency.

  10. The Contemplative Bow in Teaching and Learning Pastoral Care

    ERIC Educational Resources Information Center

    Koppel, Michael S.

    2013-01-01

    This article elucidates theoretical underpinnings for the use of one's self in the pastoral theological classroom. The contemplative bow is developed as a capacious metaphor to describe appropriate self use and its necessary importance in the teaching and learning of pastoral arts in a theological curriculum. Central to the argument is the…

  11. Threequarter view of port bow of White Holly (WLM 543) ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    Three-quarter view of port bow of White Holly (WLM 543) on left, White Sage (WLM 544) on right. Note differences between the two. - U.S. Coast Guard Cutter WHITE HOLLY, U.S. Coast Guard 8th District Base, 4640 Urquhart Street, New Orleans, Orleans Parish, LA

  12. 4. DETAIL VIEW, LOOKING SOUTH, ACROSS HULL NEAR BOW END, ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    4. DETAIL VIEW, LOOKING SOUTH, ACROSS HULL NEAR BOW END, TOP OF FORWARD STARBOARD CARGO HATCH IN FOREGROUND, OPENING FOR PORT HATCH BEYOND Edward Larrabee, photographer, November 1984 - Shooters Island, Ships Graveyard, Vessel No. 54, Newark Bay, Staten Island (subdivision), Richmond County, NY

  13. 41. AUGUST 9, 1948 BOW STARBOARD VIEW. TAKEN SOON AFTER ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    41. AUGUST 9, 1948 BOW STARBOARD VIEW. TAKEN SOON AFTER COMMISSIONING INTO U.S. COAST GUARD. NOTE ORIGINAL CRANE AND HOISTING MECHANISM AND TWO ADDITIONAL PILES (SPUDS) THAT DROPPED INTO THE MUD BOTTOM TO STEADY THE VESSEL WHILE WORKING. - U.S. Coast Guard Cutter WHITE PINE, U.S. Coast Guard 8th District Base, South Broad Street, Mobile, Mobile County, AL

  14. 18. FROM DECK ABOVE CO'S STATEROOM, LOOKING TOWARDS BOW, AT ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    18. FROM DECK ABOVE CO'S STATEROOM, LOOKING TOWARDS BOW, AT DECK ABOVE PILOT HOUSE AND BEYOND IS MAST. - U.S. Coast Guard Cutter WHITE LUPINE, U.S. Coast Guard Station Rockland, east end of Tillson Avenue, Rockland, Knox County, ME

  15. 20. FROM DECK ABOVE CREW'S BERTHING, LOOKING TOWARDS THE BOW, ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    20. FROM DECK ABOVE CREW'S BERTHING, LOOKING TOWARDS THE BOW, SHOWING WINCH FIDLY, STACK, AND UPPER DECKS. TO EITHER SIDE OF THE FIDLY IS A RHI (RIGID HULL INFLATABLE) AND CRANES. - U.S. Coast Guard Cutter WHITE LUPINE, U.S. Coast Guard Station Rockland, east end of Tillson Avenue, Rockland, Knox County, ME

  16. A Study of Uranus' Bow Shock Motions Using Langmuir Waves

    NASA Technical Reports Server (NTRS)

    Xue, S.; Cairns, I. H.; Smith, C. W.; Gurnett, D. A.

    1996-01-01

    During the Voyager 2 flyby of Uranus, strong electron plasma oscillations (Langmuir waves) were detected by the plasma wave instrument in the 1.78-kHz channel on January 23-24, 1986, prior to the inbound bow shock crossing. Langmuir waves are excited by energetic electrons streaming away from the bow shock. The goal of this work is to estimate the location and motion of Uranus' bow shock using Langmuir wave data, together with the spacecraft positions and the measured interplanetary magnetic field. The following three remote sensing analyses were performed: the basic remote sensing method, the lag time method, and the trace-back method. Because the interplanetary magnetic field was highly variable, the first analysis encountered difficulties in obtaining a realistic estimation of Uranus' bow shock motion. In the lag time method developed here, time lags due to the solar wind's finite convection speed are taken into account when calculating the shock's standoff distance. In the new trace-back method, limits on the standoff distance are obtained as a function of time by reconstructing electron paths. Most of the results produced by the latter two analyses are consistent with predictions based on the standard theoretical model and the measured solar wind plasma parameters. Differences between our calculations and the theoretical model are discussed.

  17. 30. View of main deck at bow (looking aft from ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    30. View of main deck at bow (looking aft from samson post, upper deck removed), showing anchor windlass (left foreground), head (right foregound), and forward deckhouse; weather canopy overhead not an original or permanent feature - Schooner WAWONA, 1018 Valley Street, Seattle, King County, WA

  18. 16. Detail, northeast facade, operator's bow window and tower; note ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    16. Detail, northeast facade, operator's bow window and tower; note condition of slates on tower skirt roof, missing section of gutter at left side of skirt roof, missing window panes; note also knee braces carried on masonry ancons; view to southwest, 90mm lens. - Southern Pacific Depot, 559 El Camino Real, San Carlos, San Mateo County, CA

  19. Forest resources of the Medicine Bow National Forest

    Treesearch

    Jim Steed

    2008-01-01

    The Interior West Forest Inventory and Analysis (IWFIA) Program of the USDA Forest Service, Rocky Mountain Research Station, as part of our National Forest System cooperative inventories, conducted a forest resource inventory on the Medicine Bow National Forest using a nationally standardized mapped-plot design (for more details see "Inventory methods"...

  20. A Study of Uranus' Bow Shock Motions Using Langmuir Waves

    NASA Technical Reports Server (NTRS)

    Xue, S.; Cairns, I. H.; Smith, C. W.; Gurnett, D. A.

    1996-01-01

    During the Voyager 2 flyby of Uranus, strong electron plasma oscillations (Langmuir waves) were detected by the plasma wave instrument in the 1.78-kHz channel on January 23-24, 1986, prior to the inbound bow shock crossing. Langmuir waves are excited by energetic electrons streaming away from the bow shock. The goal of this work is to estimate the location and motion of Uranus' bow shock using Langmuir wave data, together with the spacecraft positions and the measured interplanetary magnetic field. The following three remote sensing analyses were performed: the basic remote sensing method, the lag time method, and the trace-back method. Because the interplanetary magnetic field was highly variable, the first analysis encountered difficulties in obtaining a realistic estimation of Uranus' bow shock motion. In the lag time method developed here, time lags due to the solar wind's finite convection speed are taken into account when calculating the shock's standoff distance. In the new trace-back method, limits on the standoff distance are obtained as a function of time by reconstructing electron paths. Most of the results produced by the latter two analyses are consistent with predictions based on the standard theoretical model and the measured solar wind plasma parameters. Differences between our calculations and the theoretical model are discussed.

  1. 126. AERIAL FORWARD VIEW OF ENCLOSED HURRICANE BOW WITH FLIGHT ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    126. AERIAL FORWARD VIEW OF ENCLOSED HURRICANE BOW WITH FLIGHT DECK GUN MOUNTS REMOVED AND ANGLED FLIGHT DECK. 1 OCTOBER 1956. (NATIONAL ARCHIVES NO. 80-G-1001445) - U.S.S. HORNET, Puget Sound Naval Shipyard, Sinclair Inlet, Bremerton, Kitsap County, WA

  2. Application of Bow-tie methodology to improve patient safety.

    PubMed

    Abdi, Zhaleh; Ravaghi, Hamid; Abbasi, Mohsen; Delgoshaei, Bahram; Esfandiari, Somayeh

    2016-05-09

    Purpose - The purpose of this paper is to apply Bow-tie methodology, a proactive risk assessment technique based on systemic approach, for prospective analysis of the risks threatening patient safety in intensive care unit (ICU). Design/methodology/approach - Bow-tie methodology was used to manage clinical risks threatening patient safety by a multidisciplinary team in the ICU. The Bow-tie analysis was conducted on incidents related to high-alert medications, ventilator associated pneumonia, catheter-related blood stream infection, urinary tract infection, and unwanted extubation. Findings - In total, 48 potential adverse events were analysed. The causal factors were identified and classified into relevant categories. The number and effectiveness of existing preventive and protective barriers were examined for each potential adverse event. The adverse events were evaluated according to the risk criteria and a set of interventions were proposed with the aim of improving the existing barriers or implementing new barriers. A number of recommendations were implemented in the ICU, while considering their feasibility. Originality/value - The application of Bow-tie methodology led to practical recommendations to eliminate or control the hazards identified. It also contributed to better understanding of hazard prevention and protection required for safe operations in clinical settings.

  3. Hierarchical modularity of nested bow-ties in metabolic networks.

    PubMed

    Zhao, Jing; Yu, Hong; Luo, Jian-Hua; Cao, Zhi-Wei; Li, Yi-Xue

    2006-08-18

    The exploration of the structural topology and the organizing principles of genome-based large-scale metabolic networks is essential for studying possible relations between structure and functionality of metabolic networks. Topological analysis of graph models has often been applied to study the structural characteristics of complex metabolic networks. In this work, metabolic networks of 75 organisms were investigated from a topological point of view. Network decomposition of three microbes (Escherichia coli, Aeropyrum pernix and Saccharomyces cerevisiae) shows that almost all of the sub-networks exhibit a highly modularized bow-tie topological pattern similar to that of the global metabolic networks. Moreover, these small bow-ties are hierarchically nested into larger ones and collectively integrated into a large metabolic network, and important features of this modularity are not observed in the random shuffled network. In addition, such a bow-tie pattern appears to be present in certain chemically isolated functional modules and spatially separated modules including carbohydrate metabolism, cytosol and mitochondrion respectively. The highly modularized bow-tie pattern is present at different levels and scales, and in different chemical and spatial modules of metabolic networks, which is likely the result of the evolutionary process rather than a random accident. Identification and analysis of such a pattern is helpful for understanding the design principles and facilitate the modelling of metabolic networks.

  4. 25. VIEW OF ALABAMA (ALABAMIAN) FROM OFF PORT BOW; VESSEL ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    25. VIEW OF ALABAMA (ALABAMIAN) FROM OFF PORT BOW; VESSEL AT ANCHOR ON STATION IN GULF OF MEXICO WITH MOTOR BOAT TIED AT STERN Original 4-3/4'x6-3/4' photograph taken c. 1930? - Pilot Schooner "Alabama", Moored in harbor at Vineyard Haven, Vineyard Haven, Dukes County, MA

  5. 23. VIEW FROM STARBOARD BOW OF ALABAMA AS 'ALABAMIAN.' Uncopyrighted ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    23. VIEW FROM STARBOARD BOW OF ALABAMA AS 'ALABAMIAN.' Uncopyrighted 3-1/2'x5-5/8' postcard; image taken on station in Gulf of Mexico, c. 1930? - Pilot Schooner "Alabama", Moored in harbor at Vineyard Haven, Vineyard Haven, Dukes County, MA

  6. Search for systemic mass loss in Algols with bow shocks

    NASA Astrophysics Data System (ADS)

    Mayer, A.; Deschamps, R.; Jorissen, A.

    2016-03-01

    Aims: Various studies indicate that interacting binary stars of Algol type evolve non-conservatively. However, direct detections of systemic mass loss in Algols have been scarce so far. We study the systemic mass loss in Algols by looking for the presence of infrared excesses originating from the thermal emission of dust grains, which is linked to the presence of a stellar wind. Methods: In contrast to previous studies, we make use of the fact that stellar and interstellar material is piled up at the edge of the astrosphere where the stellar wind interacts with the interstellar medium. We analyse WISE W3 12 μm and WISE W4 22 μm data of Algol-type binary Be and B[e] stars and the properties of their bow shocks. From the stand-off distance of the bow shock we are able to determine the mass-loss rate of the binary system. Results: Although the velocities of the stars with respect to the interstellar medium are quite low, we find bow shocks present in two systems, namely π Aqr, and ϕ Per; a third system, CX Dra, shows a more irregular circumstellar environment morphology which might somehow be related to systemic mass loss. The properties of the two bow shocks point to mass-loss rates and wind velocities typical of single B stars, which do not support an enhanced systemic mass loss.

  7. 41. BOW SPACES (YN OFFICES, AYN OFFICES & DECK SHOP, ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    41. BOW SPACES (YN OFFICES, AYN OFFICES & DECK SHOP, LAUNDRY & BOS'N STORES), WITH HATCH TO PAINT LOCKER AT LEFT. - U.S. Coast Guard Cutter WHITE HEATH, USGS Integrated Support Command Boston, 427 Commercial Street, Boston, Suffolk County, MA

  8. 20. DECK ABOVE CREW'S BERTHING, LOOKING TOWARDS THE BOW, SHOWING ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    20. DECK ABOVE CREW'S BERTHING, LOOKING TOWARDS THE BOW, SHOWING BOAT WINCH IN FOREGROUND, BEHIND IT IS THE FIDLY AND TO EITHER SIDE OF THE FIDLY IS A RHI (RIGID HULL INFLATABLE). - U.S. Coast Guard Cutter WHITE HEATH, USGS Integrated Support Command Boston, 427 Commercial Street, Boston, Suffolk County, MA

  9. Detail of bow showing new frames and planking on starboard ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    Detail of bow showing new frames and planking on starboard side. Note oak trunnels used to fasten the planks to the frames. Frames are oak; planking is yellow pine. - Schooner ERNESTINA, New Bedford Whaling National Historical Park State Pier, New Bedford, Bristol County, MA

  10. Linker Flexibility Facilitates Module Exchange in Fungal Hybrid PKS-NRPS Engineering

    PubMed Central

    Nielsen, Maria Lund; Isbrandt, Thomas; Petersen, Lene Maj; Mortensen, Uffe Hasbro; Andersen, Mikael Rørdam; Hoof, Jakob Blæsbjerg; Larsen, Thomas Ostenfeld

    2016-01-01

    Polyketide synthases (PKSs) and nonribosomal peptide synthetases (NRPSs) each give rise to a vast array of complex bioactive molecules with further complexity added by the existence of natural PKS-NRPS fusions. Rational genetic engineering for the production of natural product derivatives is desirable for the purpose of incorporating new functionalities into pre-existing molecules, or for optimization of known bioactivities. We sought to expand the range of natural product diversity by combining modules of PKS-NRPS hybrids from different hosts, hereby producing novel synthetic natural products. We succeeded in the construction of a functional cross-species chimeric PKS-NRPS expressed in Aspergillus nidulans. Module swapping of the two PKS-NRPS natural hybrids CcsA from Aspergillus clavatus involved in the biosynthesis of cytochalasin E and related Syn2 from rice plant pathogen Magnaporthe oryzae lead to production of novel hybrid products, demonstrating that the rational re-design of these fungal natural product enzymes is feasible. We also report the structure of four novel pseudo pre-cytochalasin intermediates, niduclavin and niduporthin along with the chimeric compounds niduchimaeralin A and B, all indicating that PKS-NRPS activity alone is insufficient for proper assembly of the cytochalasin core structure. Future success in the field of biocombinatorial synthesis of hybrid polyketide-nonribosomal peptides relies on the understanding of the fundamental mechanisms of inter-modular polyketide chain transfer. Therefore, we expressed several PKS-NRPS linker-modified variants. Intriguingly, the linker anatomy is less complex than expected, as these variants displayed great tolerance with regards to content and length, showing a hitherto unreported flexibility in PKS-NRPS hybrids, with great potential for synthetic biology-driven biocombinatorial chemistry. PMID:27551732

  11. Double tibial osteotomy for bow leg patients: A case series

    PubMed Central

    Nazem, Khalilollah; Fouladi, Arash; Chinigarzadeh, Mozhdeh

    2013-01-01

    Background: High tibia osteotomy (HTO) is a common surgical operation for correction of genu varum deformity. In some patients, there are concurrent tibia vara and genu varum (bow leg). This study aimed to consider the possibility of better correction of bow leg deformity after double level tibial osteotomy (DLTO). Materials and Methods: A case series of 10 patients of genu varum in addition to tibia vara (bow leg) deformity who were referred to orthopedic ward of an academic hospital of Isfahan- Iran during 2009–2011 were included in the study. The mean age was 17.3 ± 3.1 years and all of them underwent DLTO. The results of treatment have been assessed based on clinical and radiological parameters before and after surgery. Results: The mean pre- and post operative values for Tibia-Femoral Angle, Medial Proximal of Tibia Angle (MPTA), and Lateral Distal of Tibia Angle (LDTA) were 18.13 ± 3.05° vs. 3.93 ± 0.66°, 79.13 ± 3.4° vs. 89.7 ± 1.8° and 96.40 ± 1.8° vs. 88.73 ± 3.0° respectively (P < 0.05). Improvement of all radiological parameters was meaningful. Seventy three percent of patients had normal mechanical axis of limb after surgery. The remaining cases had varus deformity in distal femur that was corrected by valgus supracondylar osteotomy in an additional operation. Limited range of motion (ROM) near knee and ankle was not observed. Conclusion: DLTO correct bow leg deformity in the point of alignment of limb and paralleling of knee and ankle joint more effectively. This method can be used in metabolic and congenital bow leg which deformities are present in throughout of the lower limb. We described this technique for the first time. PMID:24523802

  12. Static model of a violin bow: influence of camber and hair tension on mechanical behavior.

    PubMed

    Ablitzer, Frédéric; Dalmont, Jean-Pierre; Dauchez, Nicolas

    2012-01-01

    Experienced bow makers empirically know the influence of wood, tapering, and camber on the playing and tonal qualities of a bow. However, the way each parameter affects the bow mechanical behavior is not clearly established. An in-plane finite element model is developed to highlight the link between the adjustable design parameters and the mechanical behavior of a bow. This model takes into account geometric nonlinearity as well as compliance of the hair. Its validity is discussed from measurements on a bow. Results from simulations are compared to experimental results from previous studies. The consequences of adjusting hair tension and camber are then investigated.

  13. Coordinated Multiwavelength Observations of PKS 0528+134 in Quiescence

    NASA Astrophysics Data System (ADS)

    Boettcher, Markus; Palma, N.

    2011-01-01

    We report results of an intensive multiwavelength campaign on the prominent high-redshift (z = 2.06) gamma-ray bright blazar PKS 0528+134 in September - October 2009. The campaign was centered on four 30 ksec pointings with XMM-Newton, supplemented with ground-based optical (MDM, Perkins) and radio (UMRAO, Medicina, Metsaehovi, Noto, SMA) observations as well as long-term X-ray monitoring with RXTE and gamma-ray monitoring by Fermi. We find significant variability on 1 day time scales in the optical regime, accompanied by a weak redder-when-brighter trend. X-ray variability is found on longer ( 1 week) time scales, while the Fermi light curve shows no evidence for variability, neither in flux nor spectral index. We constructed four simultaneous spectral energy distributions, which can all be fit satisfactorily with a one-zone leptonic jet model. This work was supported by NASA through XMM-Newton Guest Observer Grant NNX09AV45G.

  14. 75 FR 33802 - City of Broken Bow, OK; Broken Bow Re-Regulation Dam; Hydropower Project; Notice of Proposed...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-06-15

    ... in or Eligible for Inclusion in the National Register of Historic Places June 8, 2010. Rule 2010 of... eligible for inclusion in, the National Register of Historic Places at the Broken Bow Re-Regulation Dam... list for the above-captioned proceeding may request inclusion on the restricted service list, or may...

  15. The Nearest GHz Peaked-Spectrum Radio Galaxy, PKS 1718-649

    NASA Technical Reports Server (NTRS)

    Tingay, S. J.; Jauncey, D. L.; Reynolds, J. E.; Tzioumis, A. K.; King, E. A.; Preston, R. A.; Lovell, J. E.; McCulloch, P. M.; Costa, M. E.; Nicolson, G.

    1997-01-01

    In this paper we identify PKS 1718-649, at a distance of 56 Mpc (z = 0.014; H(sub o) = 75 km/s/Mpc, q(sub o) = 0), as the nearest GHz peaked-spectrum (GPS) radio galaxy, more than four times closer than any previously known. Extensive observations at radio wavelengths with the Australia Telescope Compact Array, the Southern Hemisphere VLBI Experiment array, and the Swedish-ESO Submillimetre Telescope have allowed us to determine the properties of the radio source: PKS 1718-649 consists of two compact sub-pc-scale components separated by approximately 2 pc, the overall radio polarization is low, and the radio spectrum is peaked near 3 GHz. Order-of-magnitude agreement between the quantitative model for GPS sources of Bicknell et al. and the radio data we present, as well as data at optical wavelengths from the literature, raises the interesting possibility that PKS 1718-649 may be frustrated in its development by the nuclear environment of its host galaxy, NGC 6328. The model of Bicknell et al. suggests free-free absorption as an explanation of the PKS 1718-649 radio spectrum. However, both free-free absorption and synchrotron self-absorption mechanisms are plausible for this source and both may contribute to the overall radio spectrum. PKS 1718-649 provides evidence to strengthen the speculative suggestion that GPS sources arise as a consequence of galaxy merger activity.

  16. Post-PKS tailoring steps of the spiramycin macrolactone ring in Streptomyces ambofaciens.

    PubMed

    Nguyen, Hoang-Chuong; Darbon, Emmanuelle; Thai, Robert; Pernodet, Jean-Luc; Lautru, Sylvie

    2013-08-01

    Spiramycins are clinically important 16-member macrolide antibiotics produced by Streptomyces ambofaciens. Biosynthetic studies have established that the earliest lactonic intermediate in spiramycin biosynthesis, the macrolactone platenolide I, is synthesized by a type I modular polyketide synthase (PKS). Platenolide I then undergoes a series of post-PKS tailoring reactions yielding the final products, spiramycins I, II, and III. We recently characterized the post-PKS glycosylation steps of spiramycin biosynthesis in S. ambofaciens. We showed that three glycosyltransferases, Srm5, Srm29, and Srm38, catalyze the successive attachment of the three carbohydrates mycaminose, forosamine, and mycarose, respectively, with the help of two auxiliary proteins, Srm6 and Srm28. However, the enzymes responsible for the other tailoring steps, namely, the C-19 methyl group oxidation, the C-9 keto group reduction, and the C-3 hydroxyl group acylation, as well as the timing of the post-PKS tailoring reactions, remained to be established. In this study, we show that Srm13, a cytochrome P450, catalyzes the oxidation of the C-19 methyl group into a formyl group and that Srm26 catalyzes the reduction of the C-9 keto group, and we propose a timeline for spiramycin-biosynthetic post-PKS tailoring reactions.

  17. Post-PKS Tailoring Steps of the Spiramycin Macrolactone Ring in Streptomyces ambofaciens

    PubMed Central

    Nguyen, Hoang-Chuong; Darbon, Emmanuelle; Thai, Robert; Pernodet, Jean-Luc

    2013-01-01

    Spiramycins are clinically important 16-member macrolide antibiotics produced by Streptomyces ambofaciens. Biosynthetic studies have established that the earliest lactonic intermediate in spiramycin biosynthesis, the macrolactone platenolide I, is synthesized by a type I modular polyketide synthase (PKS). Platenolide I then undergoes a series of post-PKS tailoring reactions yielding the final products, spiramycins I, II, and III. We recently characterized the post-PKS glycosylation steps of spiramycin biosynthesis in S. ambofaciens. We showed that three glycosyltransferases, Srm5, Srm29, and Srm38, catalyze the successive attachment of the three carbohydrates mycaminose, forosamine, and mycarose, respectively, with the help of two auxiliary proteins, Srm6 and Srm28. However, the enzymes responsible for the other tailoring steps, namely, the C-19 methyl group oxidation, the C-9 keto group reduction, and the C-3 hydroxyl group acylation, as well as the timing of the post-PKS tailoring reactions, remained to be established. In this study, we show that Srm13, a cytochrome P450, catalyzes the oxidation of the C-19 methyl group into a formyl group and that Srm26 catalyzes the reduction of the C-9 keto group, and we propose a timeline for spiramycin-biosynthetic post-PKS tailoring reactions. PMID:23716060

  18. Involvement of both PKS and NRPS in antibacterial activity in Lysobacter enzymogenes OH11

    PubMed Central

    Zhang, Juan; Du, Liangcheng; Liu, Fengquan; Xu, Feifei; Hu, Baishi; Venturi, Vittorio; Qian, Guoliang

    2014-01-01

    Polyketides and nonribosomal peptides represent two large families of natural products (NPs) with diverse structures and important functions. They are synthesized by polyketide synthase (PKS) and nonribosomal peptide synthetase (NRPS), respectively. Lysobacter enzymogenes is emerging as a novel biocontrol agent against pathogens of crop plants and a new source of bioactive NPs, such as antibacterial antibiotic WAP-8294A2 and antifungal antibiotic HSAF. Genome survey of strain OH11, a Chinese L. enzymogenes isolate, detected four novel PKS, NRPS or hybrid gene clusters, designed as cluster A to D. We further individually mutated five genes (PKS or NRPS) located in these four gene clusters, and showed that a PKS gene in cluster A and an NRPS gene in cluster D were involved in the antibacterial activity via a WAP-8294A2 dependent way. The data also showed that none of the five genes was associated with antifungal activity and the regulation of HSAF biosynthesis. Our results reveal the unusual regulatory role of these PKS and NRPS genes that were discovered from genome mining in L. enzymogenes. PMID:24801439

  19. The Nearest GHz Peaked-Spectrum Radio Galaxy, PKS 1718-649

    NASA Technical Reports Server (NTRS)

    Tingay, S. J.; Jauncey, D. L.; Reynolds, J. E.; Tzioumis, A. K.; King, E. A.; Preston, R. A.; Lovell, J. E.; McCulloch, P. M.; Costa, M. E.; Nicolson, G.

    1997-01-01

    In this paper we identify PKS 1718-649, at a distance of 56 Mpc (z = 0.014; H(sub o) = 75 km/s/Mpc, q(sub o) = 0), as the nearest GHz peaked-spectrum (GPS) radio galaxy, more than four times closer than any previously known. Extensive observations at radio wavelengths with the Australia Telescope Compact Array, the Southern Hemisphere VLBI Experiment array, and the Swedish-ESO Submillimetre Telescope have allowed us to determine the properties of the radio source: PKS 1718-649 consists of two compact sub-pc-scale components separated by approximately 2 pc, the overall radio polarization is low, and the radio spectrum is peaked near 3 GHz. Order-of-magnitude agreement between the quantitative model for GPS sources of Bicknell et al. and the radio data we present, as well as data at optical wavelengths from the literature, raises the interesting possibility that PKS 1718-649 may be frustrated in its development by the nuclear environment of its host galaxy, NGC 6328. The model of Bicknell et al. suggests free-free absorption as an explanation of the PKS 1718-649 radio spectrum. However, both free-free absorption and synchrotron self-absorption mechanisms are plausible for this source and both may contribute to the overall radio spectrum. PKS 1718-649 provides evidence to strengthen the speculative suggestion that GPS sources arise as a consequence of galaxy merger activity.

  20. The Polyketide Synthase Gene pks4 of Trichoderma reesei Provides Pigmentation and Stress Resistance

    PubMed Central

    Atanasova, Lea; Knox, Benjamin P.; Kubicek, Christian P.; Baker, Scott E.

    2013-01-01

    Species of the fungal genus Trichoderma (Hypocreales, Ascomycota) are well-known for their production of various secondary metabolites. Nonribosomal peptides and polyketides represent a major portion of these products. In a recent phylogenomic investigation of Trichoderma polyketide synthase (PKS)-encoding genes, the pks4 from T. reesei was shown to be an orthologue of pigment-forming PKSs involved in synthesis of aurofusarin and bikaverin in Fusarium spp. In this study, we show that deletion of this gene in T. reesei results in loss of green conidial pigmentation and in pigmentation alteration of teleomorph structures. It also has an impact on conidial cell wall stability and the antagonistic abilities of T. reesei against other fungi, including formation of inhibitory metabolites. In addition, deletion of pks4 significantly influences the expression of other PKS-encoding genes of T. reesei. To our knowledge, this is the first indication that a low-molecular-weight pigment-forming PKS is involved in defense, mechanical stability, and stress resistance in fungi. PMID:24036343

  1. The polyketide synthase gene pks4 of Trichoderma reesei provides pigmentation and stress resistance.

    PubMed

    Atanasova, Lea; Knox, Benjamin P; Kubicek, Christian P; Druzhinina, Irina S; Baker, Scott E

    2013-11-01

    Species of the fungal genus Trichoderma (Hypocreales, Ascomycota) are well-known for their production of various secondary metabolites. Nonribosomal peptides and polyketides represent a major portion of these products. In a recent phylogenomic investigation of Trichoderma polyketide synthase (PKS)-encoding genes, the pks4 from T. reesei was shown to be an orthologue of pigment-forming PKSs involved in synthesis of aurofusarin and bikaverin in Fusarium spp. In this study, we show that deletion of this gene in T. reesei results in loss of green conidial pigmentation and in pigmentation alteration of teleomorph structures. It also has an impact on conidial cell wall stability and the antagonistic abilities of T. reesei against other fungi, including formation of inhibitory metabolites. In addition, deletion of pks4 significantly influences the expression of other PKS-encoding genes of T. reesei. To our knowledge, this is the first indication that a low-molecular-weight pigment-forming PKS is involved in defense, mechanical stability, and stress resistance in fungi.

  2. The polyketide synthase gene pks4 is essential for sexual development and regulates fruiting body morphology in Sordaria macrospora.

    PubMed

    Schindler, Daniel; Nowrousian, Minou

    2014-07-01

    Filamentous ascomycetes have long been known as producers of a variety of secondary metabolites, many of which have toxic effects on other organisms. However, the role of these metabolites in the biology of the fungi that produce them remains in most cases enigmatic. A major group of fungal secondary metabolites are polyketides. They are chemically diverse, but have in common that their chemical scaffolds are synthesized by polyketide synthases (PKSs). In a previous study, we analyzed development-dependent expression of pks genes in the filamentous ascomycete Sordaria macrospora. Here, we show that a deletion mutant of the pks4 gene is sterile, producing only protoperithecia but no mature perithecia, whereas overexpression of pks4 leads to enlarged, malformed fruiting bodies. Thus, correct expression levels of pks4 are essential for wild type-like perithecia formation. The predicted PKS4 protein has a domain structure that is similar to homologs in other fungi, but conserved residues of a methyl transferase domain present in other fungi are mutated in PKS4. Expression of several developmental genes is misregulated in the pks4 mutant. Surprisingly, the development-associated app gene is not downregulated in the mutant, in contrast to all other previously studied mutants with a block at the protoperithecial stage. Our data show that the polyketide synthase gene pks4 is essential for sexual development and plays a role in regulating fruiting body morphology. Copyright © 2014 Elsevier Inc. All rights reserved.

  3. In silicio expression analysis of PKS genes isolated from Cannabis sativa L.

    PubMed Central

    2010-01-01

    Cannabinoids, flavonoids, and stilbenoids have been identified in the annual dioecious plant Cannabis sativa L. Of these, the cannabinoids are the best known group of this plant's natural products. Polyketide synthases (PKSs) are responsible for the biosynthesis of diverse secondary metabolites, including flavonoids and stilbenoids. Biosynthetically, the cannabinoids are polyketide substituted with terpenoid moiety. Using an RT-PCR homology search, PKS cDNAs were isolated from cannabis plants. The deduced amino acid sequences showed 51%-73% identity to other CHS/STS type sequences of the PKS family. Further, phylogenetic analysis revealed that these PKS cDNAs grouped with other non-chalcone-producing PKSs. Homology modeling analysis of these cannabis PKSs predicts a 3D overall fold, similar to alfalfa CHS2, with small steric differences on the residues that shape the active site of the cannabis PKSs. PMID:21637580

  4. Gamma-Ray and Optical Oscillations in PKS 0537-441

    NASA Astrophysics Data System (ADS)

    Sandrinelli, A.; Covino, S.; Treves, A.

    2016-03-01

    We have considered the Fermi γ-ray light curve of the blazar PKS 0537-441 during a high state extending from 2008 August 10 to 2011 August 27. The periodogram exhibits a peak at T ˜ 280 days, with a significance of ˜99.7%. A peak of similar relevance at \\frac{1}{2}T is found in the optical light curves. Considering the entire duration of the Fermi light curve 2008-2015, no significant peak is revealed, while the optical one remains meaningful. Comparing with recent observations of PKS 2155-304 and PG 1553+113 it seems that month-year oscillations can characterize some blazars. Month-scale oscillations can also show up only during phases of enhanced or bursting emission, such as in the case of PKS 0537-441.

  5. The Absorption Spectrum of PKS 1756+237

    NASA Astrophysics Data System (ADS)

    Bauer, J. M.; Roth, K. C.; Jim, K. T. C.

    1998-05-01

    We are involved in a program to investigate the relationship between damped Lyalpha absorption systems and the interstellar medium of our own galaxy and nearby galaxies. This ultimately requires the proper identification of the systems responsible for the absorption so that a connection may be drawn between the absorption characteristics and the physical characteristics of the absorber, such as galaxy morphology, size, brightness, and separation from the QSO line of sight (see Jim & Roth, Kolhatkar et al., and Roth et al. also presenting here). PKS 1756+237 is a relatively bright QSO (m_V~18.0) with an emission redshift of z=1.721. There are two strong intervening absorption line systems at redshifts of 1.426 and 1.673. Both systems exhibit strong low-ionization lines, and so are believed to originate in the inner regions of galactic systems at some stage of formation. We obtained two hours of high quality HIRES spectra on the Keck 10m telescope for this QSO in May, 1997. The 6.5 km/s (0.09 Angstroms FWHM) resolution of this data is a ten-fold improvement over existing data, providing kinematic information as well as significantly improved column density measurements. Preliminary analysis of the data suggests the existence of significant Ni II abundance at z=1.67, possibly indicating a damped absorber system. The spectra cover the C II and Si II lines, enabling us to search for associated fine-structure excitation. These spectra also cover several additional low and high-ionization species from which we derive abundance and kinematic information. Images of this QSO, acquired at the UH 2.2m telescope using the QUIRC infrared and Tek2048 optical cameras with UH's tip-tilt system, show possible candidates for absorber systems.

  6. Hot flow anomaly observed at Jupiter's bow shock

    NASA Astrophysics Data System (ADS)

    Valek, P. W.; Thomsen, M. F.; Allegrini, F.; Bagenal, F.; Bolton, S.; Connerney, J.; Ebert, R. W.; Gladstone, R.; Kurth, W. S.; Levin, S.; Louarn, P.; Mauk, B.; McComas, D. J.; Pollock, C.; Reno, M.; Szalay, J. R.; Weidner, S.; Wilson, R. J.

    2017-08-01

    A Hot Flow Anomaly (HFA) is created when an interplanetary current sheet interacts with a planetary bow shock. Previous studies have reported observing HFAs at Earth, Mercury, Venus, Mars, and Saturn. During Juno's approach to Jupiter, a number of its instruments operated in the solar wind. Prior to crossing into Jupiter's magnetosphere, Juno observed an HFA at Jupiter for the first time. This Jovian HFA shares most of the characteristics of HFAs seen at other planets. The notable exception is that the Jovian HFA is significantly larger than any HFA seen before. With an apparent size greater than 2 × 106 km the Jovian HFA is orders of magnitude larger than those seen at the other planets. By comparing the size of the HFAs at the other planets with the Jovian HFA, we conclude that HFAs size scales with the size of planetary bow shocks that the interplanetary current sheet interacts with.

  7. Hot, diamagnetic cavities upstream from the earth's bow shock

    NASA Technical Reports Server (NTRS)

    Thomsen, M. F.; Gosling, J. T.; Fuselier, S. A.; Bame, S. J.; Russell, C. T.

    1986-01-01

    On eight occasions the ISEE 1 and 2 spacecraft registered peculiar plasma structures upstream of the earth's bow shock. The events exhibit a temporary, strong reduction in the magnitude of the magnetic field and strong enhancements of the field strength bordering the reduction zone. The low field strength regions featured temperatures from 1-10 million k and pressure an order of magnitude greater than the solar wind. The pressure gradients exceeded the magnetic tension around the structures, although the field of the cavities may be a closed structure. A model is proposed of hot, expanding diamagnetic plasma cavities with scales on the order of a few earth radii. Speculations on the interaction and origin or impetus for the cavities within the bow shock, foreshock, the magnetosphere and the solar wind are discussed. Similarities between the phenomena detected and signatures obtained with the AMPTE releases of chemicals in the solar wind are noted.

  8. Magnetohydrodynamic and gasdynamic theories for planetary bow waves

    NASA Technical Reports Server (NTRS)

    Spreiter, J. R.; Stahara, S. S.

    1983-01-01

    A bow wave was previously observed in the solar wind upstream of each of the first six planets. The observed properties of these bow waves and the associated plasma flows are outlined, and those features identified that can be described by a continuum magnetohydrodynamic flow theory. An account of the fundamental concepts and current status of the magnetohydrodynamic and gas dynamic theories for solar wind flow past planetary bodies is provided. This includes a critical examination of: (1) the fundamental assumptions of the theories; (2) the various simplifying approximations introduced to obtain tractable mathematical problems; (3) the limitations they impose on the results; and (4) the relationship between the results of the simpler gas dynamic-frozen field theory and the more accurate but less completely worked out magnetohydrodynamic theory. Representative results of the various theories are presented and compared.

  9. Cassini Observations of Saturn's High-Mach Number Bow Shock

    NASA Astrophysics Data System (ADS)

    Masters, A.; Sulaiman, A.; Sergis, N.; Stawarz, L.; Fujimoto, M.; Coates, A. J.; Dougherty, M. K.

    2016-12-01

    The leading explanation for the origin of galactic cosmic rays is particle acceleration at the shocks surrounding young supernova remnants (SNRs), although crucial aspects of the acceleration process are unclear. The similar collisionless plasma shocks frequently encountered by spacecraft in the solar wind are generally far weaker (lower Mach number) than these SNR shocks. However, the Cassini spacecraft has shown that the shock standing in the solar wind sunward of Saturn (Saturn's bow shock) can occasionally reach this high-Mach number astrophysical regime. In this regime Cassini has provided the first in situ evidence for electron acceleration under quasi-parallel upstream magnetic conditions. Here we review the most recent published work based on Cassini data taken at Saturn's bow shock. We then present an interpretation and discussion of the sum of the Cassini findings to date, with emphasis on the implications for shock-acceleration of charged particles. Future directions for work in this area are outlined.

  10. MESSENGER Observations of Mercury's Bow Shock and Magnetopause

    NASA Technical Reports Server (NTRS)

    Slavin, James A.; Boardsen, S. A.; Sarantos, M.; Acuna, M. H.; Anderson, B. J.; Baker, D. N.; Benna, M.; Gloeckler, G.; Gold, R. E.; Ho, G. C.; Korth, H.; Krimigis, S. M.; Livi, S. A.; McNutt, R. L., Jr.; Raines, J. M.; Schriver, D.; Solomon, S. C.; Travnicek, P.; Zurbuchen, T. H.

    2008-01-01

    MESSENGER'S 14 January 2008 encounter with Mercury will provide the first new observations of the solar wind interaction with this planet since the Mariner 10 flybys that took place over 30 years ago. The closest approach distance for this first MESSENGER flyby is targeted for an altitude of 200 km as compared with the 707 km and 327 km attained by Mariner 10 on 29 March 1974 and 16 March 1975, respectively. The locations of the bow shock and magnetopause boundaries observed by MESSENGER will be examined and compared against those found in the earlier Mariner 10 measurements and the predictions of theoretical models and numerical simulations. The structure of the magnetopause will be investigated for the presence of flux transfer events or other evidence of magnetic reconnection as will the more general implications of these new MESSENGER bow shock and magnetopause observations for the global solar wind interaction with Mercury.

  11. Energy band bowing parameter in MgZnO alloys

    SciTech Connect

    Wang, Xu; Saito, Katsuhiko; Tanaka, Tooru; Nishio, Mitsuhiro; Guo, Qixin; Nagaoka, Takashi; Arita, Makoto

    2015-07-13

    We report on bandgap bowing parameters for wurtzite and cubic MgZnO alloys from a study of high quality and single phase films in all Mg content range. The Mg contents in the MgZnO films were accurately determined using the energy dispersive spectrometer and X-ray photoelectron spectroscopy (XPS). The measurement of bandgap energies by examining the onset of inelastic energy loss in core-level atomic spectra from XPS is proved to be valid for determining the bandgap of MgZnO films. The dependence of the energy bandgap on Mg content is found to deviate downwards from linearity. Fitting of the bandgap data resulted in two bowing parameters of 2.01 ± 0.04 eV and 1.48 ± 0.11 eV corresponding to wurtzite and cubic MgZnO films, respectively.

  12. Bow-corridor local integrated resource plan: Draft plan

    SciTech Connect

    Not Available

    1990-01-01

    This plan presents the Government of Alberta's resource management policy for public lands and resources within the Bow Corridor. Resource potentials and opportunities for development are identified to assist in the economic progress of the province. The plan includes identification of its purpose and scope and the context in which it is presented; and resource management objectives and guidelines for ecological and aesthetic resources, fisheries, forests, historical resources, minerals, range land, settlement, tourism/recreation, water and watersheds and wildlife.

  13. Cold ions at the Martian bow shock - PHOBOS observations

    NASA Astrophysics Data System (ADS)

    Dubinin, E.; Lundin, R.; Koskinen, H.; Norberg, O.

    1993-04-01

    Measurements carried out by the plasma spectrometer ASPERA aboard the Phobos 2 spacecraft show that the Martian bow shock is characterized by a sudden increase of ionization of the neutral corona. It acts as a source of new ions that can strongly modify the process of ion heating behind the shock front. The loss of momentum of solar wind protons due to their interaction with exospheric ions may lead to an increase in the effective scale of the obstacle.

  14. Mercury's magnetopause and bow shock from MESSENGER Magnetometer observations

    NASA Astrophysics Data System (ADS)

    Winslow, Reka M.; Anderson, Brian J.; Johnson, Catherine L.; Slavin, James A.; Korth, Haje; Purucker, Michael E.; Baker, Daniel N.; Solomon, Sean C.

    2013-05-01

    We have established the average shape and location of Mercury's magnetopause and bow shock from orbital observations by the MESSENGER Magnetometer. We fit empirical models to midpoints of boundary crossings and probability density maps of the magnetopause and bow shock positions. The magnetopause was fit by a surface for which the position R from the planetary dipole varies as [1 + cos(θ)]-α, where θ is the angle between R and the dipole-Sun line, the subsolar standoff distance Rss is 1.45 RM (where RM is Mercury's radius), and the flaring parameter α = 0.5. The average magnetopause shape and location were determined under a mean solar wind ram pressure PRam of 14.3 nPa. The best fit bow shock shape established under an average Alfvén Mach number (MA) of 6.6 is described by a hyperboloid having Rss = 1.96 RM and an eccentricity of 1.02. These boundaries move as PRam and MA vary, but their shapes remain unchanged. The magnetopause Rss varies from 1.55 to 1.35 RM for PRam in the range of 8.8-21.6 nPa. The bow shock Rss varies from 2.29 to 1.89 RM for MA in the range of 4.12-11.8. The boundaries are well approximated by figures of revolution. Additional quantifiable effects of the interplanetary magnetic field are masked by the large dynamic variability of these boundaries. The magnetotail surface is nearly cylindrical, with a radius of ~2.7 RM at a distance of 3 RM downstream of Mercury. By comparison, Earth's magnetotail flaring continues until a downstream distance of ~10 Rss.

  15. VLBI Monitoring of the Bright Gamma-Ray Blazar PKS 0537-441

    DTIC Science & Technology

    2010-06-01

    Fermi/LAT monitored SOUl’ce list and is also in the LAT I-year Point Source Catalog ( Abdo et al. (2010c». Fig. 1. 8.4 G Hz radio images for PKS 0537...unclassified b. ABSTRACT unclassified c. THIS PAGE unclassified Standard Form 298 (Rev. 8-98) Prescribed by ANSI Std Z39-18 200 F. Hungwe ct . a1...Fig.4. Radio light curve for PKS 0537-441. Note that these data cover a much shorter time compared to the gamma-ray light curve. 202 F. Hungwe ct

  16. Fermi LAT detection of a new gamma-ray flare from FSRQ PKS 0502+049

    NASA Astrophysics Data System (ADS)

    Ojha, Roopesh; Dutka, Michael

    2013-03-01

    The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux from a source positionally consistent with the flat spectrum radio quasar PKS 0502+049 (also known as 2FGL J0505.5+0501, Nolan et al. 2012 ApJS, 199, 31). PKS 0502+049 has coordinates RA=05h05m23.1847s DEC=+04d59m42.725s, J2000, (Johnston et al. 1995, AJ, 110, 880) and redshift z=0.954 (Drinkwater et al.

  17. Fermi LAT detection of a GeV flare from the blazar PKS 0250-225

    NASA Astrophysics Data System (ADS)

    Dutka, Michael; Ojha, Roopesh

    2012-11-01

    The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux from a source positionally consistent with the flat spectrum radio quasar PKS 0250-225 (also known as 2FGL J0252.7-2218, Nolan et al. 2012 ApJS, 199, 31). PKS 0250-225 has the coordinates RA=02h52m47.9536s, DEC=-22d19m25.465s, J2000, (Beasley et al. 2002 ApJS, 141, 13) and redshift z=1.419 (Shaw et al.

  18. Increased Gamma-ray Activity from the FSRQ PKS 1424-41

    NASA Astrophysics Data System (ADS)

    Ojha, Roopesh; Dutka, Michael

    2012-10-01

    The Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope has observed increased gamma-ray emission from a source positionally coincident with the flat spectrum radio quasar PKS 1424-41 (1424-418; 2FGL J1428.0-4206, Nolan et al. 2012, ApJS, 199, 31). PKS 1424-41 has the coordinates RA=14h27m56.3s, DEC= -42d06'19.4", J2000, (Johnston et al. 1995, AJ, 110, 880).

  19. Fermi LAT Detection of a GeV Flare from FSRQ PKS 2320-035

    NASA Astrophysics Data System (ADS)

    Carpenter, Bryce; Ojha, Roopesh

    2013-04-01

    The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux from a source positionally consistent with the flat spectrum radio quasar PKS 2320-035 (also known as 2FGL J2323.6-0316, Nolan et al. 2012, ApJS, 199, 31). PKS 2320-035 has coordinates RA=23h23m31.9537s DEC=-03d17m05.023s, J2000, (Johnston et al. 1995, AJ, 110, 880) and redshift z=1.41 (Browne et al.

  20. PLANETARY EMBRYO BOW SHOCKS AS A MECHANISM FOR CHONDRULE FORMATION

    SciTech Connect

    Mann, Christopher R.; Boley, Aaron C.; Morris, Melissa A.

    2016-02-20

    We use radiation hydrodynamics with direct particle integration to explore the feasibility of chondrule formation in planetary embryo bow shocks. The calculations presented here are used to explore the consequences of a Mars-size planetary embryo traveling on a moderately excited orbit through the dusty, early environment of the solar system. The embryo’s eccentric orbit produces a range of supersonic relative velocities between the embryo and the circularly orbiting gas and dust, prompting the formation of bow shocks. Temporary atmospheres around these embryos, which can be created via volatile outgassing and gas capture from the surrounding nebula, can non-trivially affect thermal profiles of solids entering the shock. We explore the thermal environment of solids that traverse the bow shock at different impact radii, the effects that planetoid atmospheres have on shock morphologies, and the stripping efficiency of planetoidal atmospheres in the presence of high relative winds. Simulations are run using adiabatic and radiative conditions, with multiple treatments for the local opacities. Shock speeds of 5, 6, and 7 km s{sup −1} are explored. We find that a high-mass atmosphere and inefficient radiative conditions can produce peak temperatures and cooling rates that are consistent with the constraints set by chondrule furnace studies. For most conditions, the derived cooling rates are potentially too high to be consistent with chondrule formation.

  1. Planetary Embryo Bow Shocks as a Mechanism for Chondrule Formation

    NASA Astrophysics Data System (ADS)

    Mann, Christopher R.; Boley, Aaron C.; Morris, Melissa A.

    2016-02-01

    We use radiation hydrodynamics with direct particle integration to explore the feasibility of chondrule formation in planetary embryo bow shocks. The calculations presented here are used to explore the consequences of a Mars-size planetary embryo traveling on a moderately excited orbit through the dusty, early environment of the solar system. The embryo’s eccentric orbit produces a range of supersonic relative velocities between the embryo and the circularly orbiting gas and dust, prompting the formation of bow shocks. Temporary atmospheres around these embryos, which can be created via volatile outgassing and gas capture from the surrounding nebula, can non-trivially affect thermal profiles of solids entering the shock. We explore the thermal environment of solids that traverse the bow shock at different impact radii, the effects that planetoid atmospheres have on shock morphologies, and the stripping efficiency of planetoidal atmospheres in the presence of high relative winds. Simulations are run using adiabatic and radiative conditions, with multiple treatments for the local opacities. Shock speeds of 5, 6, and 7 km s-1 are explored. We find that a high-mass atmosphere and inefficient radiative conditions can produce peak temperatures and cooling rates that are consistent with the constraints set by chondrule furnace studies. For most conditions, the derived cooling rates are potentially too high to be consistent with chondrule formation.

  2. Planetary Embryo Bow Shocks as a Mechanism for Chondrule Formation

    NASA Astrophysics Data System (ADS)

    Mann, Christopher; Boley, Aaron C.; Morris, Melissa A.

    2015-01-01

    We investigate the plausibility of a planetary embryo bow shock as a mechanism for chondrule formation in the early solar system. A Mars-size planetary embryo traveling on a moderately excited orbit through the dusty early environment of the solar system will experience supersonic velocities relative to the circularly orbiting gas and dust. The resulting bow shock can thermally process solids that pass through it, with a wide range of possible conditions depending on impact radius. Volatile outgassing by the embryo along with some gas capture from the surrounding nebula can produce temporary atmospheres. We use radiation hydrodynamics simulations with direct particle integration to model the consequences of solids that encounter a bow shock produced by a 3000 km embryo with relative speeds to the gas of 5, 6, and 7 km/s. The embryos are envisaged to be surrounded by low- and high-mass atmospheres (0.75 and 6.25 Martian-mass atmospheres, respectively), and we explore different opacities for the gas. We find that a high-mass atmosphere and low dust opacity can produce peak temperatures and cooling rates that are most consistent with constraints set by chondrule furnace studies for plausible shock speeds.

  3. Bow shocks and magnetotails of Venus and Mars - A comparison

    NASA Technical Reports Server (NTRS)

    Russell, C. T.; Ong, M.; Luhmann, J. G.; Schwingenschuh, K.; Riedler, W.; Eroshenko, E.

    1992-01-01

    Observations of the bow shock location and the structure of the magnetotail of Mars by the Phobos spacecraft and of Venus by the Pioneer Venus Orbiter reveal the solar wind interactions with these two planets to be quite similar. The subsolar bow shocks of both Venus and Mars lie at 1.47 planetary radii while at the terminator they are at 2.40 and 2.65 planetary radii, respectively. Both bow shocks have oval cross sections when viewed from the sun whose major axes are controlled by the orientation of the interplanetary magnetic field. The tail lobes of both planets are similarly controlled by the IMF orientation. The strength of the solar/antisolar component of the magnetic field is 17 nT at Venus and 14 nT at Mars. The component perpendicular to the tail axis is about 1/2 the corresponding IMF component at Venus and 2 times this component at Mars. However, when these measurements are compared in terms of the distance down the tail at which each were taken, the data from the two planets are quite consistent. Hence both Venus and Mars have principally induced magnetospheres and magnetotails which stand off the solar wind flow.

  4. On the interaction of the PKS B1358–113 radio galaxy with the A1836 cluster

    SciTech Connect

    Stawarz, Ł.; Simionescu, A.; Hagino, K.; Szostek, A.; Kozieł-Wierzbowska, D.; Ostrowski, M.; Cheung, C. C.; Siemiginowska, A.; Harris, D. E.; Werner, N.; Madejski, G.; Begelman, M. C.

    2014-10-20

    Here we present the analysis of multifrequency data gathered for the Fanaroff-Riley type-II (FR II) radio galaxy PKS B1358-113, hosted in the brightest cluster galaxy in the center of A1836. The galaxy harbors one of the most massive black holes known to date, and our analysis of the acquired optical data reveals that this black hole is only weakly active, with a mass accretion rate M-dot {sub acc}∼2×10{sup −4} M-dot {sub Edd}∼0.02 M{sub ⊙} yr{sup –1}. Based on analysis of new Chandra and XMM-Newton X-ray observations and archival radio data, and assuming the well-established model for the evolution of FR II radio galaxies, we derive the preferred range for the jet kinetic luminosity L {sub j} ∼ (1-6) × 10{sup –3} L {sub Edd} ∼ (0.5-3) × 10{sup 45} erg s{sup –1}. This is above the values implied by various scaling relations proposed for radio sources in galaxy clusters, being instead very close to the maximum jet power allowed for the given accretion rate. We also constrain the radio source lifetime as τ{sub j} ∼ 40-70 Myr, meaning the total amount of deposited jet energy E {sub tot} ∼ (2-8) × 10{sup 60} erg. We argue that approximately half of this energy goes into shock heating of the surrounding thermal gas, and the remaining 50% is deposited into the internal energy of the jet cavity. The detailed analysis of the X-ray data provides indication for the presence of a bow shock driven by the expanding radio lobes into the A1836 cluster environment. We derive the corresponding shock Mach number in the range M{sub sh}∼2--4, which is one of the highest claimed for clusters or groups of galaxies. This, together with the recently growing evidence that powerful FR II radio galaxies may not be uncommon in the centers of clusters at higher redshifts, supports the idea that jet-induced shock heating may indeed play an important role in shaping the properties of clusters, galaxy groups, and galaxies in formation. In this context, we speculate on

  5. On the Interaction of the PKS B1358-113 Radio Galaxy with the A1836 Cluster

    NASA Astrophysics Data System (ADS)

    Stawarz, Ł.; Szostek, A.; Cheung, C. C.; Siemiginowska, A.; Kozieł-Wierzbowska, D.; Werner, N.; Simionescu, A.; Madejski, G.; Begelman, M. C.; Harris, D. E.; Ostrowski, M.; Hagino, K.

    2014-10-01

    Here we present the analysis of multifrequency data gathered for the Fanaroff-Riley type-II (FR II) radio galaxy PKS B1358-113, hosted in the brightest cluster galaxy in the center of A1836. The galaxy harbors one of the most massive black holes known to date, and our analysis of the acquired optical data reveals that this black hole is only weakly active, with a mass accretion rate \\dot{M}_acc ˜ 2 × 10-4 \\dot{M}_Edd ˜ 0.02 M⊙ yr-1. Based on analysis of new Chandra and XMM-Newton X-ray observations and archival radio data, and assuming the well-established model for the evolution of FR II radio galaxies, we derive the preferred range for the jet kinetic luminosity L j ~ (1-6) × 10-3 L Edd ~ (0.5-3) × 1045 erg s-1. This is above the values implied by various scaling relations proposed for radio sources in galaxy clusters, being instead very close to the maximum jet power allowed for the given accretion rate. We also constrain the radio source lifetime as τj ~ 40-70 Myr, meaning the total amount of deposited jet energy E tot ~ (2-8) × 1060 erg. We argue that approximately half of this energy goes into shock heating of the surrounding thermal gas, and the remaining 50% is deposited into the internal energy of the jet cavity. The detailed analysis of the X-ray data provides indication for the presence of a bow shock driven by the expanding radio lobes into the A1836 cluster environment. We derive the corresponding shock Mach number in the range {M}_sh ˜ 2{--}4, which is one of the highest claimed for clusters or groups of galaxies. This, together with the recently growing evidence that powerful FR II radio galaxies may not be uncommon in the centers of clusters at higher redshifts, supports the idea that jet-induced shock heating may indeed play an important role in shaping the properties of clusters, galaxy groups, and galaxies in formation. In this context, we speculate on a possible bias against detecting stronger jet-driven shocks in poorer environments

  6. Similarities and Differences between the Termination Foreshock/ Bow Shock and Planetary Bow Shocks

    NASA Astrophysics Data System (ADS)

    Krimigis, S. M.; Decker, R. B.; Roelof, E. C.; Hill, M. E.

    2006-05-01

    It is now evident that Voyager 1 (V1) entered the termination foreshock (TFS) at ~~85 AU in mid-2002, exited this region in early 2003 and re-entered in the late 2003-early 2004 time frame, before finally crossing the termination shock (TS) at ~~94 AU on December 16, 2004. The TFS region is characterized by large intensities of tangentially outward-moving beams of energetic ions E > 40 keV, and generally isotropic electron intensity increases E > 350 keV (Krimigis et al, 2003; Decker et al, 2005). Elevated magnetic field intensities were observed throughout these periods (Burlaga et al, 2003, 2005) and comparison with particle pressures showed this region to be a high-beta plasma (Krimigis et al, 2004, 2005). Proximity of the TS was also evident from occasional electron plasma oscillations seen as early as 91 AU (Gurnett and Kurth, 2005). In this paper we examine the extent to which the TFS and TS exhibit properties seen in planetary bow shocks using data from Voyager?s flyby of the outer planets and Cassini data in the vicinity of Saturn. Magnetic field distributions in these high-beta regions appear to be Gaussian. A possible source for the TSF particles is the supertherma1 population residing in the heliosheath, similar to upstream ions observed leaking from planetary magnetospheres. Krimigis, S.M. et al, Nature, 426, pg 45-48, 2003. Decker, R. B. et al, Science, 309, 2020- 2024, 2005. Burlaga et al, Geophys. Res. Lett., 30, NO. 20, 2072, doi:10.1029/2003GL018291, 2003. Burlaga, L. F, et al, Science, 309, 2027-2029, 2005 Krimigis S. M., et al, V. Florinski, N. V. Pogorelov, and G. P. Zank (eds) CP719, American Institute of Physics, 0-7354-0199-3/04, 133-138, 2004. Krimigis, S. M., et al, Proceedings of the Solar Wind 11 / SOHO 16 Conference,12-17 June 2005, Whistler, Canada, , B. Fleck & T.H. Zurbuchen (eds), (ESA SP-592, September 2005) Gurnett, D. A., and W. S. Kurth, Science, 309, 2025- 2027, 2005

  7. Resolving the Shocks in Radio Galaxy Nebulae: Hubble Space Telescope and Radio Imaging of 3C 171, 3C 277.3, and PKS 2250-41

    NASA Astrophysics Data System (ADS)

    Tilak, Avanti; O'Dea, Christopher P.; Tadhunter, Clive; Wills, Karen; Morganti, Raffaella; Baum, Stefi A.; Koekemoer, Anton M.; Dallacasa, Daniele

    2005-12-01

    We present the results of Hubble Space Telescope (HST) WFPC2 medium-band and narrowband imaging and Very Large Array and MERLIN2 radio imaging of three powerful radio galaxies: 3C 171, 3C 277.3, and PKS 2250-41. We obtained images of the rest frame [O III] λ5007 and [O II] λ3727 line emission using the linear ramp filters on WFPC2. The correlations of the emission-line morphology and the [O III]/[O II] line ratios with the radio emission seen in ground-based observations are clarified by the HST imaging. We confirm that the radio lobes and hot spots are preferentially associated with lower ionization gas. The galaxy 3C 171 exhibits high surface brightness emission-line gas mainly along the radio source axis. The lowest ionization gas is seen at the eastern hot spot. In 3C 277.3 there is bright high-ionization gas (and continuum) offset just to the east of the radio knot K1. Our observations are consistent with previous work suggesting that this emission is produced by precursor gas ionized by the shock being driven into the cloud by the deflected radio jet. In PKS 2250-41 we resolve the emission-line arc that wraps around the outer rim of the western lobe. The lower ionization [O II] emission is nested just interior to the higher ionization [O III] emission, suggesting that we have resolved the cooling region behind the bow shock. We also detect possible continuum emission from the secondary hot spot. Thus, our observations support the hypothesis that in these sources the interaction between the expanding radio source and the ambient gas strongly influences the morphology, kinematics, and ionization of the gas. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. These observations are associated with program 6657 (principal investigator C. Tadhunter).

  8. Dependence of sound characteristics on the bowing position in a violin

    NASA Astrophysics Data System (ADS)

    Roh, YuJi; Kim, Young H.

    2014-12-01

    A quantitative analysis of violin sounds produced for different bowing positions over the full length of a violin string has been carried out. An automated bowing machine was employed in order to keep the bowing parameters constant. A 3-dimensional profile of the frequency spectrum was introduced in order to characterize the violin's sound. We found that the fundamental frequency did not change for different bowing positions, whereas the frequencies of the higher harmonics were different. Bowing the string at 30 mm from the bridge produced musical sounds. The middle of the string was confirmed to be a dead zone, as reported in previous works. In addition, the quarter position was also found to be a dead zone. Bowing the string 90 mm from the bridge dominantly produces a fundamental frequency of 864 Hz and its harmonics.

  9. Biosynthesis of the Allylmalonyl-CoA Extender Unit for the FK506 Polyketide Synthase (PKS) Proceeds Through a Dedicated PKS and Facilitates the Mutasynthesis of Novel Analogs

    PubMed Central

    Mo, SangJoon; Kim, Dong Hwan; Lee, Jong Hyun; Park, Je Won; Basnet, Devi B.; Ban, Yeon Hee; Yoo, Young Ji; Chen, Shu-wei; Park, Sung Ryeol; Choi, Eun Ae; Kim, Eunji; Jin, Ying-Yu; Lee, Sung-Kwon; Park, Ju Yeol; Liu, Yuan; Lee, Mi Ok; Lee, Keum Soon; Kim, Sang Jun; Kim, Dooil; Park, Byoung Chul; Lee, Sang-gi; Kwon, Ho Jeong; Suh, Joo-Won; Moore, Bradley S.; Lim, Si-Kyu; Yoon, Yeo Joon

    2011-01-01

    The allyl moiety of the immunosuppressive agent FK506 is structurally unique amongst polyketides and critical for its potent biological activity. Here, we detail the biosynthetic pathway to allylmalonyl-coenzyme A (CoA), from which the FK506 allyl group is derived, based on a comprehensive chemical, biochemical and genetic interrogation of three FK506 gene clusters. A discrete polyketide synthase (PKS) with noncanonical domain architecture presumably in coordination with the fatty acid synthase pathway of the host catalyzes a multi-step enzymatic reaction to allylmalonyl-CoA via trans-2-pentenyl-acyl carrier protein. Characterization of this discrete pathway facilitated the engineered biosynthesis of novel allyl group-modified FK506 analogs, namely 36-fluoro-FK520 and 36-methyl-FK506, the latter of which exhibits improved neurite outgrowth activity. This unique feature of FK506 biosynthesis, in which a dedicated PKS provides an atypical extender unit for the main modular PKS, illuminates a new strategy for the combinatorial biosynthesis of designer macrolide scaffolds as well as FK506 analogs. PMID:21175203

  10. The Largest Open Reading Frame (pks12) in the Mycobacterium tuberculosis Genome Is Involved in Pathogenesis and Dimycocerosyl Phthiocerol Synthesis

    PubMed Central

    Sirakova, Tatiana D.; Dubey, Vinod S.; Kim, Hwa-Jung; Cynamon, Michael H.; Kolattukudy, Pappachan E.

    2003-01-01

    The cell wall lipids in Mycobacterium tuberculosis are probably involved in pathogenesis. The largest open reading frame in the genome of M. tuberculosis H37Rv, pks12, is unique in that it encodes two sets of domains needed to produce fatty acids. A pks12-disrupted mutant was produced, and disruption was confirmed by both PCR analysis and Southern blotting. Sodium dodecyl sulfate-polyacrylamide gel electrophoresis (SDS-PAGE) analysis showed that a 430-kDa protein band present in the wild type was missing in the mutant. Matrix-assisted laser desorption ionization-time of flight mass spectrometry (MS) and liquid chromatography (LC)-MS analysis of tryptic peptides showed that 54 peptides distributed throughout this protein matched the pks12-encoded sequence. Biochemical analysis using [1-14C]propionate as the radiotracer showed that the pks12 mutant was deficient in the synthesis of dimycocerosyl phthiocerol (DIM). SDS-PAGE, immunoblot analysis of proteins, and analysis of fatty acids showed that the mutant can produce mycocerosic acids. Thus, the pks12 gene is probably involved in the synthesis of phthiocerol, the diol required for DIM synthesis. Growth of the pks12 mutant was attenuated in mouse alveolar macrophage cell line MH-S, and the virulence of the mutant in vivo was highly attenuated in a murine model. Thus, pks12 probably participates in DIM production and its expression is involved in pathogenesis. PMID:12819062

  11. Emitting electron spectra and acceleration processes in the jet of PKS 0447-439

    NASA Astrophysics Data System (ADS)

    Zhou, Yao; Yan, Dahai; Dai, Benzhong; Zhang, Li

    2014-02-01

    We investigate the electron energy distributions (EEDs) and the corresponding acceleration processes in the jet of PKS 0447-439, and estimate its redshift through modeling its observed spectral energy distribution (SED) in the frame of a one-zone synchrotron-self Compton (SSC) model. Three EEDs formed in different acceleration scenarios are assumed: the power-law with exponential cut-off (PLC) EED (shock-acceleration scenario or the case of the EED approaching equilibrium in the stochastic-acceleration scenario), the log-parabolic (LP) EED (stochastic-acceleration scenario and the acceleration dominating), and the broken power-law (BPL) EED (no acceleration scenario). The corresponding fluxes of both synchrotron and SSC are then calculated. The model is applied to PKS 0447-439, and modeled SEDs are compared to the observed SED of this object by using the Markov Chain Monte Carlo method. The results show that the PLC model fails to fit the observed SED well, while the LP and BPL models give comparably good fits for the observed SED. The results indicate that it is possible that a stochastic acceleration process acts in the emitting region of PKS 0447-439 and the EED is far from equilibrium (acceleration dominating) or no acceleration process works (in the emitting region). The redshift of PKS 0447-439 is also estimated in our fitting: z = 0.16 ± 0.05 for the LP case and z = 0.17 ± 0.04 for BPL case.

  12. Multifrequency Monitoring of 3C 120, 3C 279, and PKS 1510--089

    NASA Technical Reports Server (NTRS)

    Jorstad, S. G.; Marscher, A. P.; Aller, M. F.; Balonek, T. J.; Gomez, J.-L.; McHardy, I. M.; Terasranta, H.; Raiteri, C.; Tosti, G.

    2001-01-01

    We analyze contemporaneous X-ray, optical, and radio light curves of 3C 120, ABC 279, and PKS 1510-089 on timescales from a few to hundreds of days over a 3-5 year period. The results show the diverse connections between variability properties at different frequencies for different blazers.

  13. Multiwavelength observations of the gamma-ray blazar PKS 0528+134 in quiescence

    DOE PAGES

    Palma, N. I.; Böttcher, M.; de la Calle, I.; ...

    2011-06-16

    Here, we present multiwavelength observations of the ultraluminous blazar-type radio loud quasar PKS 0528+134 in quiescence during the period July to December 2009. Four Target-of-Opportunity (ToO) observations with the XMM-Newton Satellite in the 0.2 – 10 keV range were supplemented with optical observations.

  14. Multiwavelength observations of the gamma-ray blazar PKS 0528+134 in quiescence

    SciTech Connect

    Palma, N. I.; Böttcher, M.; de la Calle, I.; Agudo, I.; Aller, M.; Aller, H.; Bach, U.; Benítez, E.; Buemi, C. S.; Escande, L.; Gómez, J. L.; Gurwell, M. A.; Heidt, J.; Hiriart, D.; Jorstad, S. G.; Joshi, M.; Lähteenmäki, A.; Larionov, V. M.; Leto, P.; Li, Y.; López, J. M.; Lott, B.; Madejski, G.; Marscher, A. P.; Morozova, D. A.; Raiteri, C. M.; Roberts, V.; Tornikoski, M.; Trigilio, C.; Umana, G.; Villata, M.; Wylezalek, D.

    2011-06-16

    Here, we present multiwavelength observations of the ultraluminous blazar-type radio loud quasar PKS 0528+134 in quiescence during the period July to December 2009. Four Target-of-Opportunity (ToO) observations with the XMM-Newton Satellite in the 0.2 – 10 keV range were supplemented with optical observations.

  15. Characterisation of pks15/1 in clinical isolates of Mycobacterium tuberculosis from Mexico

    PubMed Central

    Zenteno-Cuevas, Roberto; Silva-Hernández, Francisco X; Mendoza-Damián, Fabiola; Ramírez-Hernández, Maria Dolores; Vázquez-Medina, Karen; Widrobo-García, Lorena; Cuellar-Sanchez, Aremy; Muñíz-Salazar, Raquel; Enciso-Moreno, Leonor; Pérez-Navarro, Lucia Monserrat; Enciso-Moreno, José Antonio

    2013-01-01

    Tuberculosis (TB) is an infectocontagious respiratory disease caused by members of the Mycobacterium tuberculosis complex. A 7 base pair (bp) deletion in the locus polyketide synthase (pks)15/1 is described as polymorphic among members of the M. tuberculosis complex, enabling the identification of Euro-American, Indo-Oceanic and Asian lineages. The aim of this study was to characterise this locus in TB isolates from Mexico. One hundred twenty clinical isolates were recovered from the states of Veracruz and Estado de Mexico. We determined the nucleotide sequence of a ± 400 bp fragment of the locus pks15/1, while genotypic characterisation was performed by spoligotyping. One hundred and fifty isolates contained the 7 bp deletion, while five had the wild type locus. Lineages X (22%), LAM (18%) and T (17%) were the most frequent; only three (2%) of the isolates were identified as Beijing and two (1%) EAI-Manila. The wild type pks15/1 locus was observed in all Asian lineage isolates tested. Our results confirm the utility of locus pks15/1 as a molecular marker for identifying Asian lineages of the M. tuberculosis complex. This marker could be of great value in the epidemiological surveillance of TB, especially in countries like Mexico, where the prevalence of such lineages is unknown. PMID:24037193

  16. A possible extreme scattering event in progress in PKS B1322-110

    NASA Astrophysics Data System (ADS)

    Bannister, Keith; Bignall, Hayley; Johnston, Simon; Reynolds, Cormac; Stevens, Jamie; Tuntsov, Artem; Walker, Mark

    2017-01-01

    We report the ATCA discovery of an extremely variable radio source PKS B1322-110 (RA=13h25m13.220s dec=-11d17m38.00s J2000), which may be undergoing an extreme scattering event (ESE; Fiedler et al. 1987, Bannister et al. 2016).

  17. Another NIR flare of the Blazar PKS1550-242A

    NASA Astrophysics Data System (ADS)

    Carrasco, L.; Porras, A.; Escobedo, G.; Recillas, E.; Carraminana, A.

    2014-06-01

    We call attention on our recent observation of the Gamma Ray source 1FGLJ1553.4-2425 also known as PKS1550-242 with the CANICA NIR camera on the 2.1m telescope at the Observatorio Astrofisico Guillermo Haro, located in Cananea, Mexico. ...

  18. GROND+Swift/UVOT photometric redshift for the flaring blazar PKS 2123-463

    NASA Astrophysics Data System (ADS)

    Rau, A.; Schady, P.; Greiner, J.; Kann, D. A.

    2011-12-01

    Following the report of the Fermi/LAT detected brightening (Orienti et al. 2011, ATel #3808) we initiated simultaneous g'r'i'zJHK GROND (Greiner et al. 2008, PASP, 120, 405) observations of the flat spectrum radio quasar PKS 2123-463 on December 18th, 2011, at 01:21 UT. We measured the following AB magnitudes.

  19. Fermi LAT detection of renewed gamma-ray activity from PKS 2142-75

    NASA Astrophysics Data System (ADS)

    Ciprini, Stefano

    2014-05-01

    The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed high-level gamma-ray activity from a source positionally consistent with the flat spectrum radio quasar PKS 2142-75 (R.A.: 326.80304 deg, Dec.: -75.60367 deg, J2000, Johnston et al. ...

  20. Fermi LAT detection of a new Gamma-ray Source PKS B1251-713

    NASA Astrophysics Data System (ADS)

    Buson, S.

    2015-10-01

    The Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope, has observed strong gamma-ray emission from a source positionally consistent with the radio source PKS B1251-713 with coordinates RA=193.7496721 deg, Dec=-71.6384544 deg (J2000; Johnston et al. 1995, AJ, 110, 880).

  1. [Diversity of polyketide synthase genes (PKS) in metagenomic community of the freshwater sponge].

    PubMed

    Kaliuzhnaia, O V; Kulakova, N V; Itskovich, B V

    2012-01-01

    Screening of metagenomic DNA of microbial community, associated with Baikalian sponge Lubomirskia baicalensis, was made to show the presence of polyketide synthase genes (PKS). PKS enzymatic systems take part in synthesis of a great number of biologically-active substances. Cloning and sequencing of amplified products of the ketosynthase domain section of PKS gene cluster has revealed 15 fragments of PKS genes differing from each other's on 35-65% by aminoacid sequences. BLASTX analysis has shown that all these sequences belong to the KS-domains identified in various groups of microorganisms: alpha-, beta-, delta-Proteobacteria, Verrucomicrobia, Cyanobacteria, Chlorophyta. Some sequences were related to the genes which are taking part in biosynthesis of curacin A (CurI, CurJ), stigmatellin (StiC, StiG), nostophycin (NpnB), and cryptophycins (CrpB). The homology of the found sequences with those of the EMBL database varies within 50-82% confirming the presence in fresh-water sponge community the genes for synthesis of the new, yet not studied polyketide substances, possessing the biotechnological potential.

  2. Swift/XRT follow-up of the flaring blazar PKS 1424-41

    NASA Astrophysics Data System (ADS)

    D'Ammando, F.; Orienti, M.

    2013-01-01

    Following the optical and gamma-ray flaring activity of the flat spectrum radio quasar PKS 1424-41 (also known as 2FGL J1428.0-4206, Nolan et al. 2012, ApJS, 199, 31) detected by ATOM and Fermi LAT on 2013 January 6 (ATel #4714), a Swift target of opportunity observation was performed on January 7.

  3. Swift detection of an X-ray flare from the flaring blazar PKS 0502+049

    NASA Astrophysics Data System (ADS)

    Ojha, Roopesh; Dutka, Michael

    2013-03-01

    Following the recent gamma-ray flaring activity of the flat spectrum radio quasar PKS 0502+049 (also known as 2FGL J0505.5+0501, Nolan et al. 2012, ApJS, 199, 31), detected by Fermi LAT on 2013 March 2 (ATel#4858), a Swift target of opportunity observation was performed on March 13.

  4. X-Ray Absorption Toward the Einstein Ring Source PKS 1830-211

    NASA Technical Reports Server (NTRS)

    Mathur, Smita; Nair, Sunita

    1997-01-01

    PKS 1830-211 is an unusually radio-loud gravitationally lensed quasar. In the radio spectrum, the system appears as two compact, dominant features surrounded by relatively extended radio emission that forms an Einstein ring. As the line of sight to it passes close to our Galactic center, PKS 1830-211 has not been detected in wave bands other than the radio and X-ray so far. Here we present X-ray data of PKS 1830-211 observed with ROSAT Position Sensitive Proportional Counter. The X-ray spectrum shows that absorption in excess of the Galactic contribution is highly likely, which at the redshift of the lensing galaxy (z(sub t)=0.886) corresponds to N(sub H)=3.5((sup 0.6)(sub -0.5))x10(exp 22) atoms sq cm. The effective optical extinction is large, A(sub V)(observed) is greater than or approximately 5.8. When corrected for this additional extinction, the two-point optical to X-ray slope alpha(sub ox) of PKS 1830-211 lies just within the observed range of quasars. It is argued here that both compact images must be covered by the X-ray absorber(s) that we infer to be the lensing galaxy (galaxies). The dust-to-gas ratio along the line of sight within the lensing galaxy is likely to be somewhat larger than for our Galaxy.

  5. Medium-resolution far-ultraviolet spectroscopy of PKS 2155-304

    NASA Technical Reports Server (NTRS)

    Appenzeller, I.; Mandel, H.; Krautter, J.; Bowyer, S.; Hurwitz, M.; Grewing, M.; Kramer, G.; Kappelmann, N.

    1995-01-01

    Using the Berkeley spectrometer of the Orbiting Retrievable Far and Extreme Ultraviolet Spectrometer (ORFEUS) we observed the 87-117 nm UV spectrum of the BL Lac object PKS 2155-304 with about 0.5 A resolution. In addition to the expected interstellar lines we detected higher quantum number counterparts of the intergalactic Lyman alpha lines discovered earlier with IUE and the Hubble Space Telescope (HST) in the direction of PKS 2155-304. The Lyman discontinuities indicate for three of the redshifted clouds a combined H I column density of 2-5 x 10(exp 16)/sq cm, while the column density for another cloud appears to be well below 5 x 10(exp 15)/sq cm. No siginificant O VI absorption in the galactic halo toward PKS 2155-304 could be detected from our data. Assuming that saturation effects are negligible for these weak features, we obtain for the O VI column density toward PKS 2155-304 a 3 sigma upper limit of 2.7 x 10(exp 14)/sq cm.

  6. The influence of IMF clock angle on the cross section of the tail bow shock

    NASA Astrophysics Data System (ADS)

    Wang, M.; Lu, J. Y.; Kabin, K.; Yuan, H. Z.; Ma, X.; Liu, Z.-Q.; Yang, Y. F.; Zhao, J. S.; Li, G.

    2016-11-01

    We study effects of the interplanetary magnetic field (IMF) orientation on the terrestrial tail bow shock location and shape by using global MHD magnetosphere model and empirical bow shock models. It is shown that the tail bow shock cross section is well approximated by an ellipse with the direction of the major axis roughly perpendicular to the IMF clock angle direction. With the increasing IMF clock angle, the eccentricity of the bow shock cross section increases for northward IMF but decreases for southward IMF.

  7. Reduced phototropism in pks mutants may be due to altered auxin-regulated gene expression or reduced lateral auxin transport.

    PubMed

    Kami, Chitose; Allenbach, Laure; Zourelidou, Melina; Ljung, Karin; Schütz, Frédéric; Isono, Erika; Watahiki, Masaaki K; Yamamoto, Kotaro T; Schwechheimer, Claus; Fankhauser, Christian

    2014-02-01

    Phototropism allows plants to orient their photosynthetic organs towards the light. In Arabidopsis, phototropins 1 and 2 sense directional blue light such that phot1 triggers phototropism in response to low fluence rates, while both phot1 and phot2 mediate this response under higher light conditions. Phototropism results from asymmetric growth in the hypocotyl elongation zone that depends on an auxin gradient across the embryonic stem. How phototropin activation leads to this growth response is still poorly understood. Members of the phytochrome kinase substrate (PKS) family may act early in this pathway, because PKS1, PKS2 and PKS4 are needed for a normal phototropic response and they associate with phot1 in vivo. Here we show that PKS proteins are needed both for phot1- and phot2-mediated phototropism. The phototropic response is conditioned by the developmental asymmetry of dicotyledonous seedlings, such that there is a faster growth reorientation when cotyledons face away from the light compared with seedlings whose cotyledons face the light. The molecular basis for this developmental effect on phototropism is unknown; here we show that PKS proteins play a role at the interface between development and phototropism. Moreover, we present evidence for a role of PKS genes in hypocotyl gravi-reorientation that is independent of photoreceptors. pks mutants have normal levels of auxin and normal polar auxin transport, however they show altered expression patterns of auxin marker genes. This situation suggests that PKS proteins are involved in auxin signaling and/or lateral auxin redistribution. © 2013 The Authors The Plant Journal © 2013 John Wiley & Sons Ltd.

  8. Molecular epidemiology and phylogenetic distribution of the Escherichia coli pks genomic island.

    PubMed

    Johnson, James R; Johnston, Brian; Kuskowski, Michael A; Nougayrede, Jean-Philippe; Oswald, Eric

    2008-12-01

    Epidemiological and phylogenetic associations of the pks genomic island of extraintestinal pathogenic Escherichia coli (ExPEC), which encodes the genotoxin colibactin, are incompletely defined. clbB and clbN (as markers for the 5' and 3' regions of the pks island, respectively), clbA and clbQ (as supplemental pks island markers), and 12 other putative ExPEC virulence genes were newly sought by PCR among 131 published E. coli isolates from hospitalized veterans (62 blood isolates and 69 fecal isolates). Blood and fecal isolates and clbB-positive and -negative isolates were compared for 66 newly and previously assessed traits. Among the 14 newly sought traits, clbB and clbN (colibactin polyketide synthesis system), hra (heat-resistant agglutinin), and vat (vacuolating toxin) were significantly associated with bacteremia. clbB and clbN identified a subset within phylogenetic group B2 with extremely high virulence scores and a high proportion of blood isolates. However, by multivariable analysis, other traits were more predictive of blood source than clbB and clbN were; indeed, among the newly sought traits, only pic significantly predicted bacteremia (negative association). By correspondence analysis, clbB and clbN were closely associated with group B2 and multiple B2-associated traits; by principal coordinate analysis, clbB and clbN partitioned the data set better than did blood versus fecal source. Thus, the pks island was significantly associated with bacteremia, multiple ExPEC-associated virulence genes, and group B2, and within group B2, it identified an especially high-virulence subset. This extends previous work regarding the pks island and supports investigation of the colibactin system as a potential therapeutic target.

  9. Discovery Of An Infrared Bow Shock Associated With Delta Cephei

    NASA Astrophysics Data System (ADS)

    Remage Evans, Nancy; Marengo, M.; Barmby, P.; Matthews, L. D.; Bono, G.; Welch, D. L.; Romaniello, M.; Huelsman, D.; Su, K. Y. L.; Fazio, G.

    2010-05-01

    We have obtained Spitzer Infrared Array Camera (IRAC) and Multiband Infrared Photometer for Spitzer (MIPS) observations of a sample of classical Cepheids both to derive infrared Leavitt Laws (Period-Luminosity Relations) and to look for evidence of mass loss in the spectral energy distributions. The MIPS 24 and 70 micron images of Delta Cep were particularly striking, since they show an arc of emission offset about an arcmin from Delta Cep. The emission is shaped like a bow shock and is aligned with the space motion of the Cepheid, implying it is physically related to the star. Bow shock structures of this kind can be formed when ram pressure of the ambient ISM balances the wind from a mass-losing star, raising the intriguing possibility that delta Cep is undergoing mass-loss during the Cepheid phase. Circumstellar emission is not a general feature of our Cepheid observations, but 2 unusual circumstances may make it visible around Delta Cep. If the Cepheid was already surrounded by interstellar matter, mass loss from the star could have created the bow shock. Second, Delta Cep has a physical companion 40" to the South, HD 213317, itself a binary. This B7-8 III-IV star is hot enough that it may produce infrared emission by heating dust within the ejected material. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. P. B. and D. W. both acknowledge research support through Discovery Grants from the Natural Sciences and Engineering Research Council of Canada. N. R. E. acknowledges support from the Chandra X-Ray Center grant NAS8-03060.

  10. Modal Analysis of Reflector Backed Hybrid Printed Bow Tie Antenna

    NASA Astrophysics Data System (ADS)

    Singh, Dhiraj K.; Pande, D. C.; Bhattacharya, A.

    A reflector-backed hybrid of bow tie and elliptical antenna was designed and developed for UWB radar applications like ground-penetrating radar (GPR) and through-wall imaging radar (TWIR). Radiation pattern bandwidth of the antenna is found to be lesser than measured impedance bandwidth of the antenna. This anomaly was analyzed using characteristics modes of the antenna. Method of moments (MOM) using RWG basis function was used to calculate impedance matrix at each spot; frequencies and eigencurrents found were used to establish the optimum bandwidth of the antenna.

  11. SIS quasiparticle mixers with bow-tie antennas

    NASA Astrophysics Data System (ADS)

    Li, Xizhi; Richards, P. L.; Lloyd, F. L.

    1988-02-01

    Planar lithographed W-band SIS mixers with bow-tie antennas and several different RF coupling structures have been designed. Single junctions with inductive microstrips and five-junction arrays with parallel wire inductors showed good coupling over bandwiths of about 5 and 25 percent, respectively. Good agreement is obtained between design calculations based on a simple equivalent circuit and measurements of the frequency dependence of the mixer gain. No systematic difference was noted in the performance of Pb-In-Au/Pb-Bi junctions and Nb/Pb-In-Au junctions with similar capacitance and resistance.

  12. Work-place homicide by bow and arrow.

    PubMed

    Eriksson, A; Georén, B; Oström, M

    2000-07-01

    Arrow wounds represent an unusual class of wounds rarely seen by most forensic pathologists. In this paper we present a case of homicide by bow and arrow and the characteristics of such injuries. The essential characteristics of the lesions obtained from conically-tapered field points and from hunting broadhead tips are described and discussed in relation to injuries caused by firearm bullets. In the present case, three arrows struck the victim, and the order in which the injuries were sustained are analyzed. We also discuss the possibilities of localizing the shooter relative to the victim by analysis of the trajectories.

  13. Microinstabilities associated with a high Mach number, perpendicular bow shock

    NASA Technical Reports Server (NTRS)

    Wu, C. S.; Winske, D.; Tanaka, M.; Papadopoulos, K.; Akimoto, K.; Goodrich, C. C.; Zhou, Y. M.; Tsai, S. T.; Rodriguez, P.; Lin, C. S.

    1984-01-01

    Instability analyses incorporating insights gained through ISEE observations and hybrid simulations are used in an examination of the instabilities associated with a high Mach number perpendicular shock akin to the earth's bow shock. In the regions in front of, and at, the shock transition the cross-field instabilities are subdivided into the ion-ion streaming, kinetic cross-field streaming, and drift lower hybrid instability low frequency modes, as well as the electron cyclotron drift, ion sound, and electron whisker instability high frequency modes. Further downstream, ion ring-like and anisotropy-driven instabilities are considered. The implications of these results for wave signatures, plasma heating and acceleration are noted.

  14. Data Recorded as Juno Crossed Jovian Bow Shock

    NASA Image and Video Library

    2016-06-30

    This chart presents data that the Waves investigation on NASA's Juno spacecraft recorded as the spacecraft crossed the bow shock just outside of Jupiter's magnetosphere on June 24, 2016, while approaching Jupiter. Audio accompanies the animation, with volume and pitch correlated to the amplitude and frequency of the recorded waves. The graph is a frequency-time spectrogram with color coding to indicate wave amplitudes as a function of wave frequency (vertical axis, in hertz) and time (horizontal axis, with a total elapsed time of two hours). During the hour before Juno reached the bow shock, the Waves instrument was detecting mainly plasma oscillations just below 10,000 hertz (10 kilohertz). The frequency of these oscillations is related to the local density of electrons; the data yield an estimate of approximately one electron per cubic centimeter (about 16 per cubic inch) in this region just outside Jupiter's bow shock. The broadband burst of noise marked "Bow Shock" is the region of turbulence where the supersonic solar wind is heated and slowed by encountering the Jovian magnetosphere. The shock is analogous to a sonic boom generated in Earth's atmosphere by a supersonic aircraft. The region after the shock is called the magnetosheath. The vertical bar to the right of the chart indicates the color coding of wave amplitude, in decibels (dB) above the background level detected by the Waves instrument. Each step of 10 decibels marks a tenfold increase in wave power. When Juno collected these data, the distance from the spacecraft to Jupiter was about 5.56 million miles (8.95 million kilometers), indicated on the chart as 128 times the radius of Jupiter. Jupiter's magnetic field is tilted about 10 degrees from the planet's axis of rotation. The note of 22 degrees on the chart indicates that at the time these data were recorded, the spacecraft was 22 degrees north of the magnetic-field equator. The "LT" notation is local time on Jupiter at the longitude of the

  15. Properties of bow-shock sources at the Galactic center

    NASA Astrophysics Data System (ADS)

    Sanchez-Bermudez, J.; Schödel, R.; Alberdi, A.; Muzić, K.; Hummel, C. A.; Pott, J.-U.

    2014-07-01

    Context. There exists an enigmatic population of massive stars around the Galactic center (GC) that were formed some Myr ago. A fraction of these stars has been found to orbit the supermassive black hole, Sgr A*, in a projected clockwise disk-like structure, which suggests that they were formed in a formerly existing dense disk around Sgr A*. Aims: We focus on a subgroup of objects, the extended, near-infrared (NIR) bright sources IRS 1W, IRS 5, IRS 10W, and IRS 21, that have been suggested to be young, massive stars that form bow shocks through their interaction with the interstellar medium (ISM). Their nature has impeded accurate determinations of their orbital parameters. We aim at establishing their nature and kinematics to test whether they form part of the clockwise disk. Methods: We performed NIR multiwavelength imaging with NACO/VLT using direct adaptive optics (AO) and AO-assisted sparse aperture masking (SAM). We introduce a new method for self-calibration of the SAM point spread function in dense stellar fields. The emission mechanism, morphology, and kinematics of the targets were examined via 3D models, combined with existing models of the gas flow in the central parsec. Results: We confirm previous findings that IRS 21, IRS 1W, and IRS 5 are bow-shocks created by the interaction between mass-losing stars and the interstellar gas. The nature of IRS 10W remains unclear. Our modeling shows that the bow-shock emission is caused by thermal emission, while the scattering of stellar light does not play a significant role. IRS 1W shows a morphology that is consistent with a bow shock produced by an anisotropic stellar wind or by locally inhomogeneous ISM density. Our best-fit models provide estimates of the local proper motion of the ISM in the Northern Arm that agree with previously published models that were based on radio interferometry and NIR spectroscopy. Assuming that all of the sources are gravitationally tied to Sagittarius A*, their orbital planes

  16. Power aspects of processes in the bow shock region

    NASA Astrophysics Data System (ADS)

    Sedykh, Pavel

    Bow shock is a powerful transformer of the solar wind kinetic energy into the gas dynamic and electromagnetic energy. The solar wind energy also feeds the ion acceleration process, the generation of waves in the region of bow shock, and the energy necessary to build up the foreshock. A jump of the magnetic field tangential component at front crossing means that the front carries an electric current. The solar wind kinetic energy partly transforms to gas kinetic and electromagnetic energy during its passage through the bow shock front. The transition layer (magnetosheath) can use part of this energy for accelerating of plasma, but can conversely spend part its kinetic energy on the electric power generation, which afterwards may be used by the magnetosphere. Thereby, transition layer can be both consumer (sink) and generator (source) of electric power depending upon special conditions. The direction of the current behind the bow shock front depends on the sign of the IMF B _{z}-component. It is this electric current which sets convection of plasma in motion. The process of current penetration into the magnetosphere is two-step. First, a polarization field is formed that penetrates layer-by-layer into the magnetosphere. More exactly, a pulse corresponding to this field penetrates into the plasma. Then, if the system is inhomogeneous, the flow may redistribute the pressure so that gradients appearing in the plasma induce an electric current. In power terms, this electric current is required to maintain convection in the inhomogeneous system. Any change in the external current through the magnetosphere causes a convection restructuring within a time on the order of travel time of the magnetosonic wave from the magnetopause to the center of the system, because the restructuring wave comes from both flanks. Using the expressions obtained in this paper for normal components of the electric current, the flow of matter brought into the magnetosphere can be estimated. A

  17. Mercury's magnetopause and bow shock from MESSENGER observations

    NASA Astrophysics Data System (ADS)

    Winslow, R. M.; Anderson, B. J.; Johnson, C. L.; Slavin, J. A.; Korth, H.; Purucker, M. E.; Baker, D. N.; Solomon, S. C.

    2012-12-01

    We establish the time-averaged shape and location of Mercury's magnetopause and bow shock from orbital observations by the MESSENGER Magnetometer. We fit empirical models to the midpoints of boundary crossings as well as to probability density maps of the magnetopause and bow shock positions. The magnetopause is fit by two different surfaces: (1) a paraboloid, and (2) a surface for which the position R from the planetary dipole varies as [1+cos(θ)]-α, where θ is the angle between R and the dipole-Sun line, and α is a flaring parameter that governs whether the magnetotail is closed (α < 0.5) or open (α ≥ 0.5). The paraboloid magnetopause model is not able to fit simultaneously both the dayside and nightside magnetopause crossings, but the second surface gives the best-fit overall shape to the observations with a subsolar stand-off distance, Rss, of 1.45 RM (where RM is Mercury's radius), and a flaring parameter α = 0.5. The average magnetopause shape and location were determined under a mean solar wind ram pressure, PRam, of 14.3 nPa. The best-fit bow shock shape established under an average Alfvén Mach number (MA ) of 6.6 is described by a hyperboloid having Rss = 1.96 RM and an eccentricity of 1.02. These boundaries move as PRam and MA vary, but their shape remains unchanged. The magnetopause Rss varies from 1.55 RM to 1.35 RM for PRam in the range 8.8 to 21.6 nPa. The bow shock Rss varies from 2.29 RM to 1.89 RM for MA in the range 4.12 to 11.8. To first order, the boundaries are well approximated by figures of revolution. Additional effects of the interplanetary magnetic field are masked by the large dynamic variability of these boundaries. Despite the moderate average magnetic shear conditions at Mercury, the magnetotail surface is nearly cylindrical, with a radius of ~2.7 RM at a distance 3 RM downstream of Mercury. By comparison, Earth's magnetotail flaring continues until a downstream distance of ~10 Rss. This result may indicate that reconnection

  18. Both a PKS and a PPTase are involved in melanin biosynthesis and regulation of Aureobasidium melanogenum XJ5-1 isolated from the Taklimakan desert.

    PubMed

    Jiang, Hong; Liu, Guang-Lei; Chi, Zhe; Wang, Jian-Ming; Zhang, Ly-Ly; Chi, Zhen-Ming

    2017-02-20

    A PKS1 gene responsible for the melanin biosynthesis and a NPG1 gene in Aureobasidium melanogenum XJ5-1 were cloned and characterized. An ORF of the PKS1 gene encoding a protein with 2165 amino acids contained 6495bp while an ORF of the NPG1 gene encoding a protein with 340 amino acids had 1076bp. After analysis of their promoters, it was found that expression of both the PKS1 gene and the NPG1 gene was repressed by nitrogen sources and glucose, respectively. The PKS deduced from the cloned gene consisted of one ketosynthase, one acyl transferase, two acyl carrier proteins, one thioesterase and one cyclase while the PPTase belonged to the family Sfp-type. After disruption of the PKS1 gene and the NPG1 gene, expression of the PKS1 gene and the NPG1 gene and the melanin biosynthesis in the disruptants K5 and DP107 disappeared and expression of the PKS1 gene in the disruptant DP107 was also negatively influenced. However, after the NPG1 gene was complemented in the disruptant DP107, the melanin biosynthesis in the complementary strain BP17 was restored and expression of the PKS1 gene and the NPG1 gene was greatly enhanced, suggesting that the PKS was indeed activated and regulated by the PPTase and expression of the PKS1 gene and the NPG1 gene had a coordinate regulation.

  19. Dissipation Mechanisms and Particle Acceleration at the Earth's Bow Shock

    NASA Astrophysics Data System (ADS)

    Desai, M. I.; Burch, J. L.; Fuselier, S. A.; Genestreti, K. J.; Torbert, R. B.; Ergun, R.; Russell, C.; Wei, H.; Phan, T.; Giles, B. L.; Chen, L. J.; Mauk, B.

    2016-12-01

    Collisionless shocks are a major producer of suprathermal and energetic particles throughout space and astrophysical plasma environments. Theoretical studies combined with in-situ observations during the space age have significantly advanced our understanding of how such shocks are formed, the manner in which they evolve and dissipate their energy, and the physical mechanisms by which they heat the local plasma and accelerate the energetic particles. Launched in March 2015, NASA's Magnetospheric Multiscale (MMS) mission has four spacecraft separated between 10-40 km and equipped with identical state-of-the-art instruments that acquire magnetic and electric field, plasma wave, and particle data at unprecedented temporal resolution to study the fundamental physics of magnetic reconnection in the Earth's magnetosphere. Serendipitously, during Phase 1a, the MMS mission also encountered and crossed the Earth's bow shock more than 300 times. In this paper, we combine and analyze the highest available time resolution MMS burst data during 140 bow shock crossings from October 2015 through December 31, 2015 to shed new light on key open questions regarding the formation, evolution, dissipation, and particle injection and energization at collisionless shocks. In particular, we compare and contrast the differences in shock dissipation and particle acceleration mechanisms at quasi-parallel and quasi-perpendicular shocks.

  20. Evidence for fast Fermi acceleration at the Martian bow shock

    NASA Astrophysics Data System (ADS)

    Mazelle, Christian; Meziane, Karim; Romanelli, Norberto; Mitchell, David L.; Espley, Jared R.; Halekas, Jasper S.; McFadden, James P.

    2017-04-01

    Spikes of energetic electrons up to 1.5 keV are detected by the MAVEN orbiter around Mars. The spikes usually appear following a rotation of the interplanetary magnetic field (IMF). We show that they emanate from a narrow region at the tangency point of the IMF with Martian bow shock. The examination of the pitch angle distribution indicates that these spikes are associated with electrons moving sunward. The 3-dimensional angular measurements from MAVEN-SWEA detector show that for these spikes the values of phase-space density values are maximum on a ring centered about the IMF. There is no clear evidence that the radius of the ring is energy dependent. These features demonstrate for the first time that Mars acts as a fast magnetic mirror which can reflect solar wind electrons to produce high energy electron bursts. A quantitative analysis is carried out and a higher bound of the cross-shock potential of Mars bow shock is estimated.

  1. Lunar Surface Potential Increases during Terrestrial Bow Shock Traversals

    NASA Technical Reports Server (NTRS)

    Collier, Michael R.; Stubbs, Timothy J.; Hills, H. Kent; Halekas, Jasper; Farrell, William M.; Delory, Greg T.; Espley, Jared; Freeman, John W.; Vondrak, Richard R.; Kasper, Justin

    2009-01-01

    Since the Apollo era the electric potential of the Moon has been a subject of interest and debate. Deployed by three Apollo missions, Apollo 12, Apollo 14 and Apollo 15, the Suprathermal Ion Detector Experiment (SIDE) determined the sunlit lunar surface potential to be about +10 Volts using the energy spectra of lunar ionospheric thermal ions accelerated toward the Moon. We present an analysis of Apollo 14 SIDE "resonance" events that indicate the lunar surface potential increases when the Moon traverses the dawn bow shock. By analyzing Wind spacecraft crossings of the terrestrial bow shock at approximately this location and employing current balancing models of the lunar surface, we suggest causes for the increasing potential. Determining the origin of this phenomenon will improve our ability to predict the lunar surface potential in support of human exploration as well as provide models for the behavior of other airless bodies when they traverse similar features such as interplanetary shocks, both of which are goals of the NASA Lunar Science Institute's Dynamic Response of the Environment At the Moon (DREAM) team.

  2. Quasilinear simulations of interplanetary shocks and Earth's bow shock

    NASA Astrophysics Data System (ADS)

    Afanasiev, Alexandr; Battarbee, Markus; Ganse, Urs; Vainio, Rami; Palmroth, Minna; Pfau-Kempf, Yann; Hoilijoki, Sanni; von Alfthan, Sebastian

    2016-04-01

    We have developed a new self-consistent Monte Carlo simulation model for particle acceleration in shocks. The model includes a prescribed large-scale magnetic field and plasma density, temperature and velocity profiles and a self-consistently computed incompressible ULF foreshock under the quasilinear approximation. Unlike previous analytical treatments, our model is time dependent and takes full account of the anisotropic particle distributions and scattering in the wave-particle interaction process. We apply the model to the problem of particle acceleration at traveling interplanetary (IP) shocks and Earth's bow shock and compare the results with hybrid-Vlasov simulations and spacecraft observations. A qualitative agreement in terms of spectral shape of the magnetic fluctuations and the polarization of the unstable mode is found between the models and the observations. We will quantify the differences of the models and explore the region of validity of the quasilinear approach in terms of shock parameters. We will also compare the modeled IP shocks and the bow shock, identifying the similarities and differences in the spectrum of accelerated particles and waves in these scenarios. The work has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 637324 (HESPERIA). The Academy of Finland is thanked for financial support. We acknowledge the computational resources provided by CSC - IT Centre for Science Ltd., Espoo.

  3. Large amplitude MHD waves upstream of the Jovian bow shock

    NASA Technical Reports Server (NTRS)

    Goldstein, M. L.; Smith, C. W.; Matthaeus, W. H.

    1983-01-01

    Observations of large amplitude magnetohydrodynamics (MHD) waves upstream of Jupiter's bow shock are analyzed. The waves are found to be right circularly polarized in the solar wind frame which suggests that they are propagating in the fast magnetosonic mode. A complete spectral and minimum variance eigenvalue analysis of the data was performed. The power spectrum of the magnetic fluctuations contains several peaks. The fluctuations at 2.3 mHz have a direction of minimum variance along the direction of the average magnetic field. The direction of minimum variance of these fluctuations lies at approximately 40 deg. to the magnetic field and is parallel to the radial direction. We argue that these fluctuations are waves excited by protons reflected off the Jovian bow shock. The inferred speed of the reflected protons is about two times the solar wind speed in the plasma rest frame. A linear instability analysis is presented which suggests an explanation for many of the observed features of the observations.

  4. Jovian bow shock and magnetopause encounters by the Juno spacecraft

    NASA Astrophysics Data System (ADS)

    Hospodarsky, G. B.; Kurth, W. S.; Bolton, S. J.; Allegrini, F.; Clark, G. B.; Connerney, J. E. P.; Ebert, R. W.; Haggerty, D. K.; Levin, S.; McComas, D. J.; Paranicas, C.; Rymer, A. M.; Valek, P. W.

    2017-05-01

    The Juno spacecraft has crossed Jupiter's bow shock (BS) and magnetopause (MP) multiple times in the dawn sector (near 0600 local time), both during the approach to Jupiter and during the first three apojove periods. A survey of all of these crossings using the Juno field and particle instruments has been performed, with 51 bow shock and 97 magnetopause crossings being detected. The BS crossings ranged from 92 to 128 RJ with 1 encounter during the approach, 36 during the first apojove period, 0 on the second, and 14 during the third. The MP crossings ranged from 73 to 114 RJ, with 8 MP encounters during the approach, 40 encounters during the first apojove period, 24 encounters on the second, and 46 during the third. During the approach, Juno initially encountered an expanding magnetosphere resulting in a single BS and MP crossing, followed a few days later by a contracting magnetosphere, resulting in 7 more MP crossings and a BS crossing on the first outbound orbit at 92 RJ. The lack of BS crossings and the limited number of MP crossings during the second apojove period suggests a long period of an expanded magnetosphere, likely caused by a prolonged period of low solar wind dynamic pressure associated with a rarefaction region. The detection of BS crossings on the third apojove period suggests another period of a highly compressed magnetosphere.

  5. Low back pain related to bowing posture of greenhouse farmers.

    PubMed

    Maeda, K; Okazaki, F; Suenaga, T; Sakurai, T; Takamatsu, M

    1980-12-01

    Farming by means of greenhouses has spread in different parts of Japan during the past 20 years. Low back pain, an important health problem for farmers, affects those working inside a greenhouse as a result of their taking up particular postures. In order to analyze ergonomic problems of greenhouse farming relevant to low back pain, localized fatigue complaints and parts of the body where fatigue was felt during fruit picking were studied among 49 female farmers engaged in greenhouse strawberry culture and 53 female farmers engaged in greenhouse eggplant culture. Furthermore, the bowing posture for strawberry picking was compared with that of eggplant picking using newly devised posture-pattern recording equipment. More than 50% of strawberry or eggplant farmers complained of fatigue in the lower back and shoulders. The prevalence of low back pain was significantly higher among strawberry farmers than among eggplant farmers, probably due to the deep bowing posture of the farmer during picking work. The new posture-pattern recording equipment proved useful for investigating changes of work postures.

  6. Lunar Surface Potential Increases during Terrestrial Bow Shock Traversals

    NASA Technical Reports Server (NTRS)

    Collier, Michael R.; Stubbs, Timothy J.; Hills, H. Kent; Halekas, Jasper; Farrell, William M.; Delory, Greg T.; Espley, Jared; Freeman, John W.; Vondrak, Richard R.; Kasper, Justin

    2009-01-01

    Since the Apollo era the electric potential of the Moon has been a subject of interest and debate. Deployed by three Apollo missions, Apollo 12, Apollo 14 and Apollo 15, the Suprathermal Ion Detector Experiment (SIDE) determined the sunlit lunar surface potential to be about +10 Volts using the energy spectra of lunar ionospheric thermal ions accelerated toward the Moon. We present an analysis of Apollo 14 SIDE "resonance" events that indicate the lunar surface potential increases when the Moon traverses the dawn bow shock. By analyzing Wind spacecraft crossings of the terrestrial bow shock at approximately this location and employing current balancing models of the lunar surface, we suggest causes for the increasing potential. Determining the origin of this phenomenon will improve our ability to predict the lunar surface potential in support of human exploration as well as provide models for the behavior of other airless bodies when they traverse similar features such as interplanetary shocks, both of which are goals of the NASA Lunar Science Institute's Dynamic Response of the Environment At the Moon (DREAM) team.

  7. Transonic flow past a wedge profile with detached bow wave

    NASA Technical Reports Server (NTRS)

    Vincenti, Walter G; Wagoner, Cleo B

    1952-01-01

    A theoretical study has been made of the aerodynamic characteristics at zero angle of attack of a thin, doubly symmetrical double-wedge profile in the range of supersonic flight speed in which the bow wave is detached. The analysis utilizes the equations of the transonic small-disturbance theory and involves no assumptions beyond those implicit in this theory. The mixed flow about the front half of the profile is calculated by relaxation solution of boundary conditions along the shock polar and sonic line. The purely subsonic flow about the rear of the profile is found by means of the method of characteristics specialized to the transonic small-disturbance theory. Complete calculations were made for four values of the transonic similarity parameter. These were found sufficient to bridge the gap between the previous results of Guderley and Yoshihara at a Mach number of 1 and the results which are readily obtained when the bow wave is attached and the flow is completely supersonic.

  8. Model Simulations For a Potential Bow Shock at Ceres

    NASA Astrophysics Data System (ADS)

    Villarreal, M. N.; Russell, C.; Jia, Y. D.; Prettyman, T. H.; Yamashita, N.; Chi, P. J.; Joy, S. P.

    2016-12-01

    The Gamma Ray and Neutron Detector (GRaND) of the Dawn spacecraft observed bursts of energetic particles in its exterior scintillators during Survey orbit when Dawn was at a distance of 10 Ceres radii from the planet. Despite being coincident with a solar proton event, the particles do not come from the solar direction. Instead, they are due to electron bursts occurring when Ceres is within the field of view of the detectors indicating that the electrons are streaming away from the planet. The electrons have high energies between 20-100 keV and last for 20 minutes in restricted regions that appear to be controlled by the solar wind interaction with the body. The Dawn spacecraft crossing an electron foreshock could explain the temporal behavior, flux, and energy of the electrons. Here we hypothesize that the solar proton event caused enhanced sputtering at the surface creating a temporary bow shock via mass loading as the sputtered atoms were ionized and picked up by the solar wind. We use a single fluid magnetohydrodynamic model to test the transient atmospheric density and bow shock size that would be needed to replicate the geometry of the electrons.

  9. Smashing the Guitar: An Evolving Neutron Star Bow Shock

    NASA Astrophysics Data System (ADS)

    Chatterjee, S.; Cordes, J. M.

    2004-01-01

    The Guitar Nebula is a spectacular example of an Hα bow shock nebula produced by the interaction of a neutron star with its environment. The radio pulsar B2224+65 is traveling at ~800-1600 km s-1 (for a distance of 1-2 kpc), placing it on the high-velocity tail of the pulsar velocity distribution. Here we report time evolution in the shape of the Guitar Nebula, the first such observations for a bow shock nebula, as seen in Hα imaging with the Hubble Space Telescope. The morphology of the nebula provides no evidence for anisotropy in the pulsar wind nor for fluctuations in the pulsar wind luminosity. The nebula shows morphological changes over two epochs spaced by 7 years that imply the existence of significant gradients and inhomogeneities in the ambient interstellar medium. These observations offer astrophysically unique, in situ probes of length scales between 5×10-4 and 0.012 pc. Model fitting suggests that the nebula axis-and thus the three-dimensional velocity vector-lies within 20° of the plane of the sky and also jointly constrains the distance to the neutron star and the ambient density.

  10. DOUBLE BOW SHOCKS AROUND YOUNG, RUNAWAY RED SUPERGIANTS: APPLICATION TO BETELGEUSE

    SciTech Connect

    Mackey, Jonathan; Mohamed, Shazrene; Neilson, Hilding R.; Langer, Norbert; Meyer, Dominique M.-A.

    2012-05-20

    A significant fraction of massive stars are moving supersonically through the interstellar medium (ISM), either due to disruption of a binary system or ejection from their parent star cluster. The interaction of their wind with the ISM produces a bow shock. In late evolutionary stages these stars may undergo rapid transitions from red to blue and vice versa on the Hertzsprung-Russell diagram, with accompanying rapid changes to their stellar winds and bow shocks. Recent three-dimensional simulations of the bow shock produced by the nearby runaway red supergiant (RSG) Betelgeuse, under the assumption of a constant wind, indicate that the bow shock is very young (<30, 000 years old), hence Betelgeuse may have only recently become an RSG. To test this possibility, we have calculated stellar evolution models for single stars which match the observed properties of Betelgeuse in the RSG phase. The resulting evolving stellar wind is incorporated into two-dimensional hydrodynamic simulations in which we model a runaway blue supergiant (BSG) as it undergoes the transition to an RSG near the end of its life. We find that the collapsing BSG wind bubble induces a bow shock-shaped inner shell around the RSG wind that resembles Betelgeuse's bow shock, and has a similar mass. Surrounding this is the larger-scale retreating bow shock generated by the now defunct BSG wind's interaction with the ISM. We suggest that this outer shell could explain the bar feature located (at least in projection) just in front of Betelgeuse's bow shock.

  11. Correlation of bow shock plasma wave turbulence with solar wind parameters

    NASA Technical Reports Server (NTRS)

    Rodriguez, P.; Gurnett, D. A.

    1975-01-01

    The r.m.s. field strengths of electrostatic and electromagnetic turbulence in the earth's bow shock, measured in the frequency range 20 Hz to 200 kHz with IMP-6 satellite, are found to correlate with specific solar wind parameters measured upstream of the bow shock.

  12. 26 CFR 48.4161(b)-1 - Imposition and rates of tax; bows and arrows.

    Code of Federal Regulations, 2010 CFR

    2010-04-01

    ... 26 Internal Revenue 16 2010-04-01 2010-04-01 true Imposition and rates of tax; bows and arrows. 48... Imposition and rates of tax; bows and arrows. (a) Imposition of tax. Section 4161(b) imposes a tax on the... a draw weight of 10 pounds or more; (2) Any arrow that measures 18 inches overall or more in length...

  13. The bowing potential of granitic rocks: rock fabrics, thermal properties and residual strain

    NASA Astrophysics Data System (ADS)

    Siegesmund, S.; Mosch, S.; Scheffzük, Ch.; Nikolayev, D. I.

    2008-10-01

    The bowing of natural stone panels is especially known for marble slabs. The bowing of granite is mainly known from tombstones in subtropical humid climate. Field inspections in combination with laboratory investigations with respect to the thermal expansion and the bowing potential was performed on two different granitoids (Cezlak granodiorite and Flossenbürg granite) which differ in the composition and rock fabrics. In addition, to describe and explain the effect of bowing of granitoid facade panels, neutron time-of-flight diffraction was applied to determine residual macro- and microstrain. The measurements were combined with investigations of the crystallographic preferred orientation of quartz and biotite. Both samples show a significant bowing as a function of panel thickness and destination temperature. In comparison to marbles the effect of bowing is more pronounced in granitoids at temperatures of 120°C. The bowing as well as the thermal expansion of the Cezlak sample is also anisotropic with respect to the rock fabrics. A quantitative estimate was performed based on the observed textures. The effect of the locked-in stresses may also have a control on the bowing together with the thermal stresses related to the different volume expansion of the rock-forming minerals.

  14. Rare Etiology of Bow Hunter’s Syndrome and Systematic Review of Literature

    PubMed Central

    Rastogi, Vaibhav; Rawls, Ashley; Moore, Omar; Victorica, Benjamin; Khan, Sheema; Saravanapavan, Pradeepan; Midivelli, Sunitha; Raviraj, Prathap; Khanna, Anna; Bidari, Sharathchandra; Hedna, Vishnumurthy S

    2015-01-01

    BACKGROUND Bow Hunter’s Syndrome is a mechanical occlusion of the vertebral artery which leads to a reduction in blood flow in posterior cerebral circulation resulting in transient reversible symptomatic vertebrobasilar insufficiency. CASE DESCRIPTION We present a case of Bow Hunter’s syndrome in a 53-year-old male that occurred after the patient underwent surgical correction of a proximal left subclavian artery aneurysm. Shortly after the surgery, the patient began to complain of transient visual changes, presyncopal spells, and dizziness upon turning his head to the left. A transcranial doppler ultrasound confirmed the diagnosis of Bow Hunter’s syndrome. SYSTEMIC REVIEW We analyzed the data on 153 patients with Bow Hunter’s syndrome from the literature. An osteophyte was the most common cause of vertebral artery occlusion, and left vertebral artery was more commonly involved in patients with Bow Hunter’s syndrome. Dynamic angiography was the definitive imaging modality to confirm the diagnosis, and surgery was most successful in alleviating symptoms. CONCLUSION We believe that this is the first case of iatrogenic Bow Hunter’s syndrome after surgical intervention for an aneurysm repair, and the largest review of literature of Bow Hunter’s syndrome. Dynamic angiography is the gold standard for the diagnosis of Bow Hunter’s syndrome. Surgery should be considered as the primary treatment approach in these patients, especially those who have bony compression as the etiology. PMID:26301025

  15. Comparison of Global 3D Bow Shock Models with Different Controlling Parameters

    NASA Astrophysics Data System (ADS)

    Merka, J.; Sibeck, D. G.

    2014-12-01

    Interaction of the supersonic solar wind with Earth's magnetosphere creates fast mode magnetosonic waves that travel back upstream, combine and steepen to form the bow shock wave. The bow shock wave has been studied for more than four decades but existing models are still often inaccurate.Previous studies established that bow shock shape and position are primarily controlled by solar wind pressure, upstream Mach numbers, interplanetary magnetic field orientation and magnetopause shape and position.We have collected a total of 28,287 bow shock crossings identified in observations from the Cluster 1-4, Geotail, IMP-8, Interball-1, MAGION-4, THEMIS A-E and WIND spacecraft and use this database to predict bow shock position as a function of solar wind parameters.The database of bow shock crossings is fitted using a method similar to Peredo et al. [1995] which presumes a general 3D second-order bow shock shape parameterized by the upstream dynamic pressure and Alfven Mach number values. The use of a prescribed shock shape results in a model that provides accurate predictions for Alfven Mach numbers as low as 2 and can be used with confidence up to 40 Re along the magnetotail. For comparison, we apply the same method to create additional global 3D bow shock models parameterized by various parameters such as interplanetary magnetic field magnitude, solar wind proton density, bulk speed, etc. The best model is sought that would be most accurate for a wide range of upstream conditions.

  16. Bow Shock Leads the Way for a Speeding Hot Jupiter

    NASA Astrophysics Data System (ADS)

    Kohler, Susanna

    2015-09-01

    As hot Jupiters whip around their host stars, their speeds can exceed the speed of sound in the surrounding material, theoretically causing a shock to form ahead of them. Now, a study has reported the detection of such a shock ahead of transiting exoplanet HD 189733b, providing a potential indicator of the remarkably strong magnetic field of the planet.Rushing PlanetsDue to their proximity to their hosts, hot Jupiters move very quickly through the stellar wind and corona surrounding the star. When this motion is supersonic, the material ahead of the planet can be compressed by a bow shock and for a transiting hot Jupiter, this shock will cross the face of the host star in advance of the planets transit.In a recent study, a team of researchers by Wilson Cauley of Wesleyan University report evidence of just such a pre-transit. The teams target is exoplanet HD 189733b, one of the closest hot Jupiters to our solar system. When the authors examined high-resolution transmission spectra of this system, they found that prior to the optical transit of the planet, there was a large dip in the transmission of the first three hydrogen Balmer lines. This could well be the absorption of an optically-thick bow shock as it moves past the face of the star.Tremendous MagnetismOperating under this assumption, the authors create a model of the absorption expected from a hot Jupiter transiting with a bow shock ahead of it. Using this model, they show that a shock leading the planet at a distance of 12.75 times the planets radius reproduces the key features of the transmission spectrum.This stand-off distance is surprisingly large. Assuming that the location of the bow shock is set by the point where the planets magnetospheric pressure balances the pressure of the stellar wind or corona that it passes through, the planetary magnetic field would have to be at least 28 Gauss. This is seven times the strength of Jupiters magnetic field!Understanding the magnetic fields of exoplanets is

  17. Effect of Body Structure on Skill Formation in a Force Precision Task Mimicking Cello Bowing Movement

    NASA Astrophysics Data System (ADS)

    Ogihara, Naomichi; Yamazaki, Nobutoshi

    To elucidate the skill formation mechanism in a complex force precision task mimicking cello bowing movements, three-dimensional joint orientations and changes in bowing force are measured for 2 novice and 2 expert subjects. A rigid link model of the human upper limb is constructed in order to calculate changes in joint moment, potential energy and structural inductivity of motion during bowing, and the motions are compared kinetically. Results show that the novices generate low-in-potential energy bowing motion, but not suitable for skillful control of the bow. In contrast, the experts can fulfill a task requirement by skillfully coordinating the musculo-skeletal system, but the motion is not easy as that of the novices. It is suggested that the transition from a novice to an expert may be difficult due to the ease in the initially generated motion, which obstructs the search for the optimal skillful motion.

  18. Evidence-based practice and barriers to compliance: Face bow transfer.

    PubMed

    Shah, Kumar; Koka, Sreenivas

    2016-01-01

    To recapitulate a 2003 study inquiring of US dental schools whether they teach the face bow transfer by means of a survey in order to determine if compliance with clinical evidence has improved. The same 54 dental schools surveyed in 2003 were asked the same question regarding whether they teach the use of the face bow transfer in the complete denture curriculum. Teaching of the face bow transfer has increased in prevalence from 84% of surveyed schools in 2003 to 93.75% of surveyed schools in 2015. This finding is especially interesting in light of the fact that there is no compelling evidence supporting the use of the face bow transfer with regard to improving patient outcomes. With respect to the continued unjustified teaching of the face bow transfer, some possible reasons for non-compliance with best available evidence are presented using the medical literature for reference. Copyright © 2015 Japan Prosthodontic Society. Published by Elsevier Ltd. All rights reserved.

  19. SnPKS19 Encodes the Polyketide Synthase for Alternariol Mycotoxin Biosynthesis in the Wheat Pathogen Parastagonospora nodorum.

    PubMed

    Chooi, Yit-Heng; Muria-Gonzalez, Mariano Jordi; Mead, Oliver L; Solomon, Peter S

    2015-08-15

    Alternariol (AOH) is an important mycotoxin from the Alternaria fungi. AOH was detected for the first time in the wheat pathogen Parastagonospora nodorum in a recent study. Here, we exploited reverse genetics to demonstrate that SNOG_15829 (SnPKS19), a close homolog of Penicillium aethiopicum norlichexanthone (NLX) synthase gene gsfA, is required for AOH production. We further validate that SnPKS19 is solely responsible for AOH production by heterologous expression in Aspergillus nidulans. The expression profile of SnPKS19 based on previous P. nodorum microarray data correlated with the presence of AOH in vitro and its absence in planta. Subsequent characterization of the ΔSnPKS19 mutants showed that SnPKS19 and AOH are not involved in virulence and oxidative stress tolerance. Identification and characterization of the P. nodorum SnPKS19 cast light on a possible alternative AOH synthase gene in Alternaria alternata and allowed us to survey the distribution of AOH synthase genes in other fungal genomes. We further demonstrate that phylogenetic analysis could be used to differentiate between AOH synthases and the closely related NLX synthases. This study provides the basis for studying the genetic regulation of AOH production and for development of molecular diagnostic methods for detecting AOH-producing fungi in the future.

  20. Unequal outer and inner bow configurations: comparing 2 asymmetric headgear systems.

    PubMed

    Brosh, Tamar; Portal, Schay; Sarne, Ofer; Vardimon, Alexander D

    2005-07-01

    Asymmetric headgear is used when different molar distalization forces (MDF) are needed on the right and left sides of the jaw to correct a Class II molar relationship. We investigated 2 asymmetric headgear configurations, the outer-bow and the inner-bow, on cervical-pull headgear. In the first configuration, 5 hooks were soldered on 1 side of the outer bow at 10-mm intervals, making this side shorter; in the other, 4 stops (1.5 mm) were added to 1 side of the inner bow, making this side longer. The right and left MDF and the extraoral force (EF) were measured simultaneously with 2 fork transducers and a testing machine, respectively. A 40-mm difference between the long and short outer bows resulted in a 2.17-fold greater MDF on the long-side molar (7:3 ratio). The 3-4 stop configuration provided the optimal inner-bow arrangement, with stop/no-stop MDF ratios of 7:3 and 10:0, respectively, at 10 N EF. At low-to-medium EF levels, a unilateral MDF developed on the stop side with zero MDF on the no-stop side. The sum of the right and left MDF nearly equaled the EF in the outer-bow asymmetry and was 60% in the inner-bow setting; this suggests strong lateral forces in the latter. Clinically, for a bilateral unequal Class II relationship, the system of choice is outer-bow asymmetric headgear. For a unilateral Class II relationship with 1 side in a Class I molar relationship (Class II subdivision), inner-bow asymmetric headgear is recommended.

  1. 76 FR 2710 - Pitney Bowes, Inc., Mailing Solutions Management Division Including On-Site Leased Workers of...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-01-14

    ... Employment and Training Administration Pitney Bowes, Inc., Mailing Solutions Management Division Including On..., applicable to workers and former workers of Pitney Bowes, Inc., Mailing Solutions Management Division... of workers of Pitney Bowes, Inc., the Mailing Solutions Management Division, located in Shelton...

  2. Twenty-Year Optical Variability of The Blazar PKS 1749+096: Exponential Outbursts?

    NASA Astrophysics Data System (ADS)

    Balonek, Thomas J.; Lam, M. T.; Patrick, P. A.; Scott, E. L.; Kaercher, A. J.; Rupert, J.; Taber, T.; Hegel, P.; Tam, Y. H. N.; Morin, A.; Levandowski, K.; Graber, E. L.; Quirk, T. S.

    2011-01-01

    We present the twenty-year R-band optical variability light curve for the BL Lac type quasar PKS 1749+096. We investigate the characteristic timescales and intensity of outbursts and flares by fitting exponential profiles to the variations. PKS 1749+096 underwent strong optical outbursts during the summers of 2007 and 2008, reaching its brightest optical level in two decades, and exhibited an inactive period during summer 2009. We compare these two outbursts with lower amplitude well-sampled variations in 2000 through 2003. Observations were obtained as part of the intensive blazar variability monitoring program at the Colgate University Foggy Bottom Observatory (FBO). We gratefully acknowledge support for student research through an REU grant to the Keck Northeast Astronomy Consortium from the National Science Foundation, the NASA / New York Space Grant, and the Justus and Jayne Schlichting Student Research Fund at Colgate University.

  3. Spectropolarimetry of PKS 0040-005 and the orientation of broad absorption line quasars

    NASA Astrophysics Data System (ADS)

    Brotherton, M. S.; De Breuck, C.; Schaefer, J. J.

    2006-10-01

    We have used the Very Large Telescope (VLT) to obtain spectropolarimetry of the radio-loud, double-lobed broad absorption line (BAL) quasar PKS 0040-005. We find that the optical continuum of PKS 0040-005 is intrinsically polarized at 0.7 per cent with an electric vector position angle nearly parallel to that of the large-scale radio axis. This result is naturally explained in terms of an equatorial scattering region seen at a small inclination, building a strong case that the BAL outflow is not equatorial. In conjunction with other recent results concerning BAL quasars, the era of simply characterizing these sources as `edge-on' is over. Based on observations collected at the European Southern Observatory, Paranal, project 71.B-0121(A). E-mail: mbrother@uwyo.edu (MSB); cdbreuc@eso.org (CDB); schaefjj@ufl.edu (JJS) ‡ ESO Visitor.

  4. COMPTEL observations of PKS 0208-512 from 1991 to 1998

    NASA Astrophysics Data System (ADS)

    Williams, O. R.; Bennett, K.; Collmar, W.; Iyudin, A. F.; Schönfelder, V.; Steinle, H.; Bloemen, H.; Hermsen, W.; McConnell, M.; Ryan, J.; Stacy, G.

    2001-09-01

    A systematic re-analysis of all observations with the blazar PKS 0208-512 in the COMPTEL field-of-view has been performed. Evidence for a possible spectral peak in the MeV band has been reported previously using data from two observations during May and June 1993. When excluding these observations, we clearly detect a low flux from PKS 0208-512 using the summed data from the remaining eighteen observations. It was also found that the detailed results with respect to the possible MeV peak depend on the range of measured photon scatter angles applied during the background estimation. The impact of this increase in the measurement uncertainties on the interpretation of the data are discussed.

  5. Unusual flaring activity in the blazar PKS 1424-418 during 2008-2011

    SciTech Connect

    Buson, S.; Longo, F.; Larsson, S.; Cutini, S.; Finke, J.; Ciprini, S.; Ojha, R.; D’Ammando, F.; Donato, D.; Thompson, D. J.; Desiante, R.; Bastieri, D.; Wagner, S.; Hauser, M.; Fuhrmann, L.; Dutka, M.; Müller, C.; Kadler, M.; Angelakis, E.; Zensus, J. A.; Stevens, J.; Blanchard, J. M.; Edwards, P. G.; Lovell, J. E. J.; Gurwell, M. A.; Wehrle, A. E.; Zook, A.

    2014-09-01

    Context. Blazars are a subset of active galactic nuclei (AGN) with jets that are oriented along our line of sight. Variability and spectral energy distribution (SED) studies are crucial tools for understanding the physical processes responsible for observed AGN emission. Aims. We report peculiar behaviour in the bright γ-ray blazar PKS 1424-418 and use its strong variability to reveal information about the particle acceleration and interactions in the jet. Methods. Correlation analysis of the extensive optical coverage by the ATOM telescope and nearly continuous γ-ray coverage by the Fermi Large Area Telescope is combined with broadband, time-dependent modeling of the SED incorporating supplemental information from radio and X-ray observations of this blazar. Results. We analyse in detail four bright phases at optical-GeV energies. These flares of PKS 1424-418 show high correlation between these energy ranges, with the exception of one large optical flare that coincides with relatively low γ-ray activity. Although the optical/ γ-ray behaviour of PKS 1424-418 shows variety, the multiwavelength modeling indicates that these differences can largely be explained by changes in the flux and energy spectrum of the electrons in the jet that are radiating. We find that for all flares the SED is adequately represented by a leptonic model that includes inverse Compton emission from external radiation fields with similar parameters. Conclusions. Detailed studies of individual blazars like PKS 1424-418 during periods of enhanced activity in different wavebands are helping us identify underlying patterns in the physical parameters in this class of AGN.

  6. Renewed gamma-ray activity from the blazar PKS 1510-089 detected by AGILE

    NASA Astrophysics Data System (ADS)

    Pittori, C.; Tavani, M.; Lucarelli, F.; Verrecchia, F.; Piano, G.; Munar-Adrover, P.; Bulgarelli, A.; Fioretti, V.; Zoli, A.; Vercellone, S.; Minervini, G.; Striani, E.; Cardillo, M.; Gianotti, F.; Trifoglio, M.; Giuliani, A.; Mereghetti, S.; Caraveo, P.; Perotti, F.; Chen, A.; Argan, A.; Costa, E.; Del Monte, E.; Evangelista, Y.; Feroci, M.; Lazzarotto, F.; Lapshov, I.; Pacciani, L.; Soffitta, P.; Sabatini, S.; Vittorini, V.; Pucella, G.; Rapisarda, M.; Di Cocco, G.; Fuschino, F.; Galli, M.; Labanti, C.; Marisaldi, M.; Pellizzoni, A.; Pilia, M.; Trois, A.; Barbiellini, G.; Vallazza, E.; Longo, F.; Morselli, A.; Picozza, P.; Prest, M.; Lipari, P.; Zanello, D.; Cattaneo, P. W.; Rappoldi, A.; Colafrancesco, S.; Parmiggiani, N.; Ferrari, A.; Antonelli, A.; Giommi, P.; Salotti, L.; Valentini, G.; D'Amico, F.

    2016-08-01

    AGILE is now detecting transient gamma-ray emission above 100 MeV from a source positionally consistent with the blazar PKS 1510-089. Integrating from 2016-08-07 09:00 UT to 2016-08-09 09:00 UT, a preliminary maximum likelihood analysis yields a detection above 100 MeV positioned at Galactic coordinates (l,b) = (350.64,40.32) +/- 0.7 (stat.) +/- 0.1 (syst.).

  7. Multiwavelength observations of a VHE gamma-ray flare from PKS 1510-089 in 2015

    NASA Astrophysics Data System (ADS)

    Ahnen, M. L.; Ansoldi, S.; Antonelli, L. A.; Arcaro, C.; Babić, A.; Banerjee, B.; Bangale, P.; Barres de Almeida, U.; Barrio, J. A.; Bednarek, W.; Bernardini, E.; Berti, A.; Biasuzzi, B.; Biland, A.; Blanch, O.; Bonnefoy, S.; Bonnoli, G.; Borracci, F.; Bretz, T.; Carosi, R.; Carosi, A.; Chatterjee, A.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; Cumani, P.; Da Vela, P.; Dazzi, F.; De Angelis, A.; De Lotto, B.; de Oña Wilhelmi, E.; Di Pierro, F.; Doert, M.; Domínguez, A.; Dominis Prester, D.; Dorner, D.; Doro, M.; Einecke, S.; Eisenacher Glawion, D.; Elsaesser, D.; Engelkemeier, M.; Fallah Ramazani, V.; Fernández-Barral, A.; Fidalgo, D.; Fonseca, M. V.; Font, L.; Fruck, C.; Galindo, D.; García López, R. J.; Garczarczyk, M.; Gaug, M.; Giammaria, P.; Godinović, N.; Gora, D.; Guberman, D.; Hadasch, D.; Hahn, A.; Hassan, T.; Hayashida, M.; Herrera, J.; Hose, J.; Hrupec, D.; Hughes, G.; Ishio, K.; Konno, Y.; Kubo, H.; Kushida, J.; Kuveždić, D.; Lelas, D.; Lindfors, E.; Lombardi, S.; Longo, F.; López, M.; Majumdar, P.; Makariev, M.; Maneva, G.; Manganaro, M.; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martínez, M.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Moralejo, A.; Moretti, E.; Nakajima, D.; Neustroev, V.; Niedzwiecki, A.; Nievas Rosillo, M.; Nilsson, K.; Nishijima, K.; Noda, K.; Nogués, L.; Paiano, S.; Palacio, J.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Paredes-Fortuny, X.; Pedaletti, G.; Peresano, M.; Perri, L.; Persic, M.; Poutanen, J.; Prada Moroni, P. G.; Prandini, E.; Puljak, I.; Garcia, J. R.; Reichardt, I.; Rhode, W.; Ribó, M.; Rico, J.; Saito, T.; Satalecka, K.; Schroeder, S.; Schweizer, T.; Shore, S. N.; Sillanpää, A.; Sitarek, J.; Šnidarić, I.; Sobczynska, D.; Stamerra, A.; Strzys, M.; Surić, T.; Takalo, L.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Torres, D. F.; Torres-Albà, N.; Toyama, T.; Treves, A.; Vanzo, G.; Vazquez Acosta, M.; Vovk, I.; Ward, J. E.; Will, M.; Wu, M. H.; Zarić, D.; Desiante, R.; Becerra González, J.; D'Ammando, F.; Larsson, S.; Raiteri, C. M.; Reinthal, R.; Lähteenmäki, A.; Järvelä, E.; Tornikoski, M.; Ramakrishnan, V.; Jorstad, S. G.; Marscher, A. P.; Bala, V.; MacDonald, N. R.; Kaur, N.; Sameer; Baliyan, K.; Acosta-Pulido, J. A.; Lazaro, C.; Martí-nez-Lombilla, C.; Grinon-Marin, A. B.; Pastor Yabar, A.; Protasio, C.; Carnerero, M. I.; Jermak, H.; Steele, I. A.; Larionov, V. M.; Borman, G. A.; Grishina, T. S.

    2017-07-01

    Context. PKS 1510-089 is one of only a few flat spectrum radio quasars detected in the very-high-energy (VHE, > 100 GeV) gamma-ray band. Aims: We study the broadband spectral and temporal properties of the PKS 1510-089 emission during a high gamma-ray state. Methods: We performed VHE gamma-ray observations of PKS 1510-089 with the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) telescopes during a long, high gamma-ray state in May 2015. In order to perform broadband modeling of the source, we have also gathered contemporaneous multiwavelength data in radio, IR, optical photometry and polarization, UV, X-ray, and GeV gamma-ray ranges. We construct a broadband spectral energy distribution (SED) in two periods, selected according to VHE gamma-ray state. Results: PKS 1510-089 was detected by MAGIC during a few day-long observations performed in the middle of a long, high optical and gamma-ray state, showing for the first time a significant VHE gamma-ray variability. Similarly to the optical and gamma-ray high state of the source detected in 2012, it was accompanied by a rotation of the optical polarization angle and the emission of a new jet component observed in radio. However, owing to large uncertainty on the knot separation time, the association with the VHE gamma-ray emission cannot be firmly established. The spectral shape in the VHE band during the flare is similar to those obtained during previous measurements of the source. The observed flux variability sets constraints for the first time on the size of the region from which VHE gamma rays are emitted. We model the broadband SED in the framework of the external Compton scenario and discuss the possible emission site in view of multiwavelength data and alternative emission models.

  8. PKS 1510-089 in high gamma-ray state as detected by AGILE

    NASA Astrophysics Data System (ADS)

    Minervini, G.; Piano, G.; Munar-Adrover, P.; Verrecchia, F.; Pittori, C.; Lucarelli, F.; Tavani, M.; Donnarumma, I.; Bulgarelli, A.; Fioretti, V.; Zoli, A.; Vercellone, S.; Striani, E.; Cardillo, M.; Gianotti, F.; Trifoglio, M.; Giuliani, A.; Mereghetti, S.; Caraveo, P.; Perotti, F.; Chen, A.; Argan, A.; Costa, E.; Del Monte, E.; Evangelista, Y.; Feroci, M.; Lazzarotto, F.; Lapshov, I.; Pacciani, L.; Soffitta, P.; Sabatini, S.; Vittorini, V.; Pucella, G.; Rapisarda, M.; Di Cocco, G.; Fuschino, F.; Galli, M.; Labanti, C.; Marisaldi, M.; Pellizzoni, A.; Pilia, M.; Trois, A.; Barbiellini, G.; Vallazza, E.; Longo, F.; Morselli, A.; Picozza, P.; Prest, M.; Lipari, P.; Zanello, D.; Cattaneo, P. W.; Rappoldi, A.; Colafrancesco, S.; Parmiggiani, N.; Ferrari, A.; Antonelli, A.; Giommi, P.; Salotti, L.; Valentini, G.; D'Amico, F.

    2016-09-01

    The AGILE-GRID is detecting transient gamma-ray emission above 100 MeV from the blazar PKS 1510-089. Integrating from 2016-09-19 UT 01:00:00 to 2016-09-21 UT 01:00:00, a preliminary likelihood analysis provides a gamma-ray flux F( > 100 MeV) = (3.7 +/- 1.2) x 10^-6 photons/cm^2/s with a significance above 5 sigma.

  9. ATel draft: Fermi LAT detection of a new Gamma-ray Source PKS 2247-131

    NASA Astrophysics Data System (ADS)

    Buson, S.

    2016-07-01

    The Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope, has observed strong gamma-ray emission from a source positionally consistent with the radio source PKS 2247-131 with coordinates RA=342.4983854 deg, Dec=-12.8546736 deg (J2000; Beasley et al. 2002, ApJS, 141, 13). This source is not in any published LAT catalog and was not detected by AGILE or EGRET.

  10. Ultraviolet polarimetry and spectroscopy of the BL Lacertae object PKS 2155-304

    NASA Technical Reports Server (NTRS)

    Allen, Richard G.; Smith, Paul S.; Angel, J. R. P.; Miller, Bryan W.; Anderson, Scott F.; Margon, Bruce

    1993-01-01

    HST and Faint Object Spectrograph spectropolarimetry is presented for the BL Lac object PKS 2155-304; attention is given to the wavelength dependence of the UV linear polarization in a BL Lac object. The UV polarimetry yields evidence that the UV polarized flux is generated by the synchrotron mechanism responsible for optical polarization. Both the UV and optical emission are produced in the same region of the source.

  11. Outburst of PKS J0808-0751 (3EG J0812-0646)

    NASA Astrophysics Data System (ADS)

    Carrasco, L.; Carraminana, A.; Recillas, E.; Porras, A.; Chavuchyan, V.

    2009-04-01

    We call attention on our recent observations of PKS J0808-0751 with the Cananea NIR camera (CANICA) on the 2.1m telescope at the Observatorio Astrofísico Guillermo Haro. We found that this quasar shows a flux increase of 3.5 magnitudes in the Ks bandpass during the past year. Below, we list our photometric results for this period.

  12. High radio fluxes of PKS2023-07 measured with RATAN-600

    NASA Astrophysics Data System (ADS)

    Trushkin, S. A.; Nizhelskij, N. A.; Tsybulev, P. G.

    2016-04-01

    After the AGILE detection the gamma-ray flare from the quasar PSK2023-07 (correctly PKS B2022-077) by Piano et al, ATel #8879 we carried out its observations with the RATAN-600 radio telescope SAO RAS. The measured flux densities are equal to 1.50, 1.96, 2.54 Jy at 4.8, 11.2, 21.7 GHz respectively on 1 Apr 2016.

  13. The High-energy Continuum Emission of the Gamma-Ray Blazar PKS 0528+134

    NASA Technical Reports Server (NTRS)

    Sambruna, Rita M.; Urry, C. Megan; Maraschi, L.; Ghisellini, G.; Mukherjee, R.; Pesce, Joseph E.; Wagner, S. J.; Wehrle, A. E.; Hartman, R. C.; Lin, Y. C.; VonMintigny, C.

    1997-01-01

    We present Advanced Satellite for Cosmology and Astrophysics (ASCA) observations of the gamma-ray blazar PKS 0528 + 134, obtained at two separate epochs in 1994 August and 1995 March. These data represent the first measurement of the X-ray continuum emission of this source in the medium-hard X-ray band. Both ASCA spectra are consistent with a single power law with photon index GAMMA approx. = 1.7-1.8 and column density N(sub H) approx. = 5 x 10(exp 21)/ sq cm, higher than Galactic. The X-ray flux increased by a factor of 4 in approx. 7 months without appreciable change of the spectral shape. During the lower state of 1994 August, PKS 0528 + 134 was observed simultaneously in the optical, X-rays, and at gamma-ray energies with Energetic Gamma Ray Experiment Telescope (EGRET). The gamma-ray intensity is the faintest detected thus far in the source, with a steep spectrum (GAMMA approx. = 2.7). The extrapolation of the X-ray continuum to the gamma-ray range requires a sharp spectral break at approx. 10(exp 22) Hz. We discuss the radio through gamma-ray spectral energy distribution of PKS 0528 + 134, comparing the low state of 1994 August with the flare state of 1993 March. We show that in PKS 0528 + 134, a non-negligible contribution from the external radiation field is present and that, although synchrotron self-Compton scenarios cannot be ruled out, inverse Compton upscattering of thermal seed photons may be the dominant cooling process for the production of the high-energy continuum in this blazar.

  14. The High-Energy Continuum Emission of the Gamma-Ray Blazar PKS 0528+134

    NASA Technical Reports Server (NTRS)

    Sambruna, Rita M.; Urry, C. Megan; Maraschi, L.; Ghisellini, G.; Mukherjee, R.; Pesce, Joseph E.; Wagner, S. J.; Wehrle, A. E.; Hartman, R. C.; Lin, Y. C.

    1997-01-01

    We present Advanced Satellite for Cosmology and Astrophysics (ASCA) observations of the gamma-ray blazar PKS 0528 + 134, obtained at two separate epochs in 1994 August and 1995 March. These data represent the first measurement of the X-ray continuum emission of this source in the medium-hard X-ray band. Both ASCA spectra are consistent with a single power law with photon index GAMMA approximate 1.7-1.8 and column density N(sub H) approximately 5 x 10(exp 21) /sq cm, higher than Galactic. The X-ray flux increased by a factor of 4 in approximately 7 months without appreciable change of the spectral shape. During the lower state of 1994 August, PKS 0528 + 134 was observed simultaneously in the optical, X-rays, and at gamma-ray energies with EGRET. The gamma-ray intensity is the faintest detected thus far in the source, with a steep spectrum (GAMMA approximately 2.7). The extrapolation of the X-ray continuum to the gamma-ray range requires a sharp spectral break at approximately 10(exp 22) Hz. We discuss the radio through gamma-ray spectral energy distribution of PKS 0528 + 134, comparing the low state of 1994 August with the flare state of 1993 March. We show that in PKS 0528 + 134, a non-negligible contribution from the external radiation field is present and that, although synchrotron self-Compton scenarios cannot be ruled out, inverse Compton upscattering of thermal seed photons may be the dominant cooling process for the production of the high-energy continuum in this blazar.

  15. Unusual flaring activity in the blazar PKS 1424-418 during 2008-2011

    DOE PAGES

    Buson, S.; Longo, F.; Larsson, S.; ...

    2014-09-01

    Context. Blazars are a subset of active galactic nuclei (AGN) with jets that are oriented along our line of sight. Variability and spectral energy distribution (SED) studies are crucial tools for understanding the physical processes responsible for observed AGN emission. Aims. We report peculiar behaviour in the bright γ-ray blazar PKS 1424-418 and use its strong variability to reveal information about the particle acceleration and interactions in the jet. Methods. Correlation analysis of the extensive optical coverage by the ATOM telescope and nearly continuous γ-ray coverage by the Fermi Large Area Telescope is combined with broadband, time-dependent modeling of themore » SED incorporating supplemental information from radio and X-ray observations of this blazar. Results. We analyse in detail four bright phases at optical-GeV energies. These flares of PKS 1424-418 show high correlation between these energy ranges, with the exception of one large optical flare that coincides with relatively low γ-ray activity. Although the optical/ γ-ray behaviour of PKS 1424-418 shows variety, the multiwavelength modeling indicates that these differences can largely be explained by changes in the flux and energy spectrum of the electrons in the jet that are radiating. We find that for all flares the SED is adequately represented by a leptonic model that includes inverse Compton emission from external radiation fields with similar parameters. Conclusions. Detailed studies of individual blazars like PKS 1424-418 during periods of enhanced activity in different wavebands are helping us identify underlying patterns in the physical parameters in this class of AGN.« less

  16. Hard-spectrum gamma-ray flare from PKS 0507+17

    NASA Astrophysics Data System (ADS)

    Kreter, M.; Buson, S.

    2016-11-01

    The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux and an unusually hard gamma-ray spectrum from a source positionally consistent with PKS 0507+17 (R.A.= 05h10m02.3691s, Dec.= +18d00m41.582s, J2000.0, Johnston et al. 1995, AJ, 110, 880).

  17. AGILE detection of renewed gamma-ray activity from the blazar PKS 1502+106

    NASA Astrophysics Data System (ADS)

    Pittori, C.; Bulgarelli, A.; Lucarelli, F.; Verrecchia, F.; Fioretti, V.; Tavani, M.; Vercellone, S.; Piano, G.; Striani, E.; Donnarumma, I.; Cardillo, M.; Gianotti, F.; Trifoglio, M.; Giuliani, A.; Mereghetti, S.; Caraveo, P.; Perotti, F.; Chen, A.; Argan, A.; Costa, E.; Del Monte, E.; Evangelista, Y.; Feroci, M.; Lazzarotto, F.; Lapshov, I.; Pacciani, L.; Soffitta, P.; Sabatini, S.; Vittorini, V.; Pucella, G.; Rapisarda, M.; Di Cocco, G.; Fuschino, F.; Galli, M.; Labanti, C.; Marisaldi, M.; Pellizzoni, A.; Pilia, M.; Trois, A.; Barbiellini, G.; Vallazza, E.; Longo, F.; Morselli, A.; Picozza, P.; Prest, M.; Lipari, P.; Zanello, D.; Cattaneo, P. W.; Rappoldi, A.; Colafrancesco, S.; Parmiggiani, N.; Ferrari, A.; Antonelli, A.; Giommi, P.; Salotti, L.; Valentini, G.; D'Amico, F.

    2016-01-01

    The AGILE satellite detects renewed gamma-ray activity from a source positionally consistent with the high-redshift (z=1.8383) blazar PKS 1502+106 (also known as OR 103, S3 1502+10 and 3FGLJ1504.4+1029), with radio coordinates, R.A.: 226.10408 deg, Dec: 10.49422 deg (J2000) (Johnston et al. 1995, AJ, 110, 880).

  18. Swift follow-up of the flaring blazar PKS 0250-225

    NASA Astrophysics Data System (ADS)

    Dutka, Michael; Ojha, Roopesh; Donato, DavidePottschmidt, Katja

    2012-11-01

    Following the gamma-ray flaring activity of the flat spectrum radio quasar PKS 0250-225 (also known as 2FGL J0252.7-2218, Nolan et al. 2012, ApJS, 199, 31) detected by Fermi LAT on 2012 November 13 (ATel #4574) two Swift target of opportunity observations were performed on November 14 and 16. As no significant differences were found between the two epochs the combined results are reported here.

  19. AGILE detects enhanced gamma-ray emission from the FSRQ PKS 0502+049

    NASA Astrophysics Data System (ADS)

    Lucarelli, F.; Pittori, C.; Verrecchia, F.; Tavani, M.; Bulgarelli, A.; Fioretti, V.; Striani, E.; Vercellone, S.; Piano, G.; Donnarumma, I.; Cardillo, M.; Gianotti, F.; Trifoglio, M.; Giuliani, A.; Mereghetti, S.; Caraveo, P.; Perotti, F.; Chen, A.; Argan, A.; Costa, E.; Del Monte, E.; Evangelista, Y.; Feroci, M.; Lazzarotto, F.; Lapshov, I.; Pacciani, L.; Soffitta, P.; Sabatini, S.; Vittorini, V.; Pucella, G.; Rapisarda, M.; Di Cocco, G.; Fuschino, F.; Galli, M.; Labanti, C.; Marisaldi, M.; Pellizzoni, A.; Trois, A.; Pilia, M.; Barbiellini, G.; Vallazza, E.; Longo, F.; Morselli, A.; Picozza, P.; Prest, M.; Lipari, P.; Zanello, D.; Cattaneo, P. W.; Rappoldi, A.; Colafrancesco, S.; Parmiggiani, N.; Ferrari, A.; Giommi, P.; Salotti, L.; Valentini, G.

    2014-09-01

    AGILE is detecting increased gamma-ray emission above 100 MeV from a source positionally consistent with the flat spectrum radio quasar PKS 0502+049. Integrating from 2014-09-08 03:00 UT to 2014-09-10 03:00 UT, a preliminary maximum likelihood analysis yields a detection above 100 MeV positioned at Galactic coordinates (l,b) = (195.47, -20.81) +/- 0.6 (stat.) +/- 0.1 (syst.).

  20. Millimeter radio event emerging in the gamma-ray flaring blazar PKS 0528+134

    NASA Astrophysics Data System (ADS)

    Angelakis, E.; Fuhrmann, L.; Nestoras, I.; Schmidt, R.; Zensus, J. A.; Krichbaum, T. P.; Ungerechts, H.; Sievers, A.; Riquelme, D.

    2011-06-01

    Responding to the ATel #3412 reporting the recent activity of PKS 0528+134 at gamma-rays, we here report its behavior in the cm-to-mm radio bands as observed by the F-GAMMA program. Recent activity: Observations performed with the Effelsberg 100-m and the IRAM 30-m telescope since January 2007 show that the source is following monotonously decaying long term trend.

  1. PKS 2123-463: A Confirmed Gamma-ray Blazar at High Redshift

    NASA Technical Reports Server (NTRS)

    DAmmando, F.; Rau, A.; Schady, P.; Finke, J.; Orienti, M.; Greiner, J.; Kann, D. A.; Ojha, R.; Foley, A. R.; Stevens, J.; Blanchard, J. M.; Edwards, P. G.; Kadler, M.; Lovell, J. E. J.

    2012-01-01

    The flat spectrum radio quasar (FSRQ) PKS 2123-463 was associated in the First Fermi-LAT source catalog with the gamma-ray source 1FGL J2126.1-4603, but when considering the full first two years of Fermi observations, no gamma-ray source at a position consistent with this FSRQ was detected, and thus PKS 2123-463 was not reported in the Second Fermi-LAT source catalog. On 2011 December 14 a gamma-ray source positionally consistent with PKS 2123-463 was detected in flaring activity by Fermi-LAT. This activity triggered radio-to-X-ray observations by the Swift, GROND, ATCA, Ceduna, and KAT-7 observatories. Results of the localization of the gamma-ray source over 41 months of Fermi-LAT operation are reported here in conjunction with the results of the analysis of radio, optical, UV and X-ray data collected soon after the gamma-ray flare. The strict spatial association with the lower energy counterpart together with a simultaneous increase of the activity in optical, UV, X-ray and gamma-ray bands led to a firm identification of the gamma-ray source with PKS 2123-463. A new photometric redshift has been estimated as z = 1.46 +/- 0.05 using GROND and Swift/UVOT observations, in rough agreement with the disputed spectroscopic redshift of z = 1.67. We fit the broadband spectral energy distribution with a synchrotron/external Compton model. We find that a thermal disk component is necessary to explain the optical/UV emis- sion detected by Swift/UVOT. This disk has a luminosity of 1.8x1046 erg s-1, and a fit to the disk emission assuming a Schwarzschild (i.e., nonrotating) black hole gives a mass of 2 x 109 M(solar mass). This is the first black hole mass estimate for this source.

  2. Reproducing the spectral energy distribution of PKS 1424+240: the role of automatic photon quenching

    NASA Astrophysics Data System (ADS)

    Gao, Quan-Gui; Lu, Fang-Wu; Zhang, Li

    2017-01-01

    We present a one-zone homogeneous self-consistent model for the multiwavelength emission features of PKS 1424+240 that allows the effects of automatic photon quenching to be studied. In the model, a steady γ-ray injection rate in the source is assumed and the non-linear time-dependent kinematic equations describing the evolution of both electrons and photons are then acquired; these self-consistently involve photon-photon interaction, synchrotron radiation of electron/positron pairs, inverse Compton scattering and synchrotron self-absorption. The model is applied to reproduce the multiwavelength spectrum of PKS 1424+240; our results indicate that the observed spectral energy distribution (SED) of PKS 1424+240 can be reproduced well in the case of both electron injection and photon injection. The injected electrons mainly influence the SED over radio, optical and X-ray bands and the SED in the high-energy γ-ray band is determined mainly by automatic photon quenching; in particular, the break form of the spectrum in the energy range ≥ a few GeV is caused by this. It should be noted that the observed SED from X-ray to γ-ray bands can be reproduced only through quenching, provided the observed data in the optical band are produced through some other mechanism, e.g. electron synchrotron radiation.

  3. The synchrotron continuum of the highly polarized quasar PKS 1546+027

    NASA Technical Reports Server (NTRS)

    Smith, Paul S.; Schmidt, Gary D.; Jannuzi, Buell T.; Elston, Richard

    1994-01-01

    The wavelength dependence of optical linear polarization of the highly polarized quasar (HPQ) PKS 1546+027 is investigated for the first time. Both spectropolarimetry and broad-band filter polarimetry are presented for a period when the object was undergoing a strong ourburst in flux and polarization. The rapid polarization variations observed argues that an optically thin synchrotron-emitting region, similar in polarization properties to BL Lacertae objects and optically violent variable (OVV) quasars, is the major source of polarized flux from this object. The continuum polarization increases dramatically with wavelength and is about twice as high at 8000 A than at 4000 A. Spectropolarimetry reveals that the emission-line flux from PKS 1546+027 dilutes the continuum polarization and is probably unpolarized. There is no evidence for any variation in polarization position angle with wavelength. The polarized flux spectrum is well-represented by a steep power law with a spectral index of -2.2, supporting the view that the polarized flux has a nonthermal origin. The observed polarization properties of PKS 1546+027 are consistent with a model that has been proposed to explain the optical to ultraviolet continua of several OVVs. In this model the optical to near-UV spectral flux distribution is a combination of light from a polarized synchrotron component plus an unpolarized component with spectral properties typical of low-polarization quasars.

  4. COMPTEL observations of the gamma-ray blazar PKS 1622-297

    NASA Astrophysics Data System (ADS)

    Zhang, S.; Collmar, W.; Bennett, K.; Bloemen, H.; Hermsen, W.; McConnell, M.; Reimer, O.; Schönfelder, V.; Wagner, S. J.; Williams, O. R.

    2002-05-01

    We report results of observations and analyses on the gamma-ray blazar PKS 1622-297, with emphasis on the COMPTEL data (0.75-30 MeV) collected between April 1991 and November 1997. PKS 1622-297 was detected as a source of gamma-rays by the EGRET experiment aboard CGRO in 1995 during a gamma-ray outburst at energies above 100 MeV lasting for five weeks. In this time period the blazar was significantly ( ~ 5.9 sigma) detected by COMPTEL at 10-30 MeV. At lower COMPTEL energies the detection is marginal, resulting in a hard MeV spectrum. The combined COMPTEL/EGRET energy spectrum shows a break at MeV energies. The broad-band spectrum (radio - gamma-rays) shows that the gamma-ray emission dominates the overall power output. On top of the 5-week gamma-ray outburst, EGRET detected a huge flare lasting for >1 day. Enhanced MeV emission (10-30 MeV) is found near the time of this flare, suggesting a possible time delay with respect to the emission above 100 MeV. Outside the 5-week flaring period in 1995, we do not detect MeV emission from PKS 1622-297.

  5. Interkingdom Gene Transfer of a Hybrid NPS/PKS from Bacteria to Filamentous Ascomycota

    PubMed Central

    Lawrence, Daniel P.; Kroken, Scott; Pryor, Barry M.; Arnold, A. Elizabeth

    2011-01-01

    Nonribosomal peptides (NRPs) and polyketides (PKs) are ecologically important secondary metabolites produced by bacteria and fungi using multidomain enzymes called nonribosomal peptide synthetases (NRPSs) and polyketide synthases (PKSs), respectively. Previous phylogenetic analyses of fungal NRPSs and PKSs have suggested that a few of these genes were acquired by fungi via horizontal gene transfer (HGT) from bacteria, including a hybrid NPS/PKS found in Cochliobolus heterostrophus (Dothideomycetes, Ascomycota). Here, we identify this hybrid gene in fungi representing two additional classes of Ascomycota (Aspergillus spp., Microsporum canis, Arthroderma spp., and Trichophyton spp., Eurotiomycetes; Chaetomium spp. and Metarhizium spp., Sordariomycetes) and use phylogenetic analyses of the most highly conserved domains from NRPSs (adenylation (A) domain) and PKSs (ketoacyl synthase (KS) domain) to examine the hypothesis that the hybrid NPS7/PKS24 was acquired by fungi from bacteria via HGT relatively early in the evolution of the Pezizomycotina. Our results reveal a unique ancestry of the A domain and KS domain in the hybrid gene relative to known fungal NRPSs and PKSs, provide strong evidence for HGT of the hybrid gene from a putative bacterial donor in the Burkholderiales, and suggest the HGT event occurred early in the evolution of the filamentous Ascomycota. PMID:22140558

  6. Color Variations of Two Blazars: BL Lac and PKS 0736+017

    NASA Astrophysics Data System (ADS)

    Clements, S. D.

    2002-12-01

    Multi-night campaigns to monitor sources for microvariability were undertaken in the summer of 1997 for BL Lac and in early 2002 for PKS 0736+017. BL Lac was observed at Rosemary Hill Observatory in Bronson, Florida and PKS 0736+017 was observed with the SARA telescope on Kitt Peak in Arizona. Both sources underwent dramatic flares and exhibited substantial microvariability. During each campaign, the source was observed alternately through V and R filters so that color variations could be monitored as well. The most commonly reported behavior for such objects is that they become redder when fainter. This is observed in the BL Lac data. These data do not indicate that the point source varies in color however. Instead, they support the notion that the underlying host galaxy contributes a larger fraction of the total flux when the source is faint than when it is bright. More unusual was the observation that PKS 0736+017 was observed to be redder when brighter. The data support the notion that the observed color variation may be related more to the nature of the variation (flaring, subsiding, or quiescent) than to the flux level.

  7. Intensive optical monitoring of the BL Lacertae object PKS 2155-304

    NASA Technical Reports Server (NTRS)

    Smith, Paul S.; Hall, Patrick B.; Allen, Richard G.; Sitko, Michael L.

    1992-01-01

    Ground-based optical polarimetry and photometry of the BL Lac object PKS 2155-304 conducted just before and during the IUE monitoring program from November 1 to 19, 1991 are presented. The optical observations reveal strong daily variability in both flux and linear polarization. Broadband UBVRI photometry shows that the slope of the optical continuum remained relatively constant even though the object brightened by nearly a magnitude. PKS 2155-304 was near its historical photometric maximum during the last two weeks of November. The degree of polarization varied between 2 and 8 percent, and fluctuations of 2-3 percent were observed in a day. Daily variations in the position angle of the polarization were observed to be as high as 25 percent, though the position angle was observed to lie between 105 and 140 deg throughout the monitoring program. Some of the implications that these optical data have on models of the source of the continuum emission in PKS 2155-304 are discussed.

  8. Possible Ceres bow shock surfaces based on fluid models

    NASA Astrophysics Data System (ADS)

    Jia, Y.-D.; Villarreal, M. N.; Russell, C. T.

    2017-05-01

    The hot electron beams that Dawn detected at Ceres can be explained by fast-Fermi acceleration at a temporary bow shock. A shock forms when the solar wind encounters a temporary atmosphere, similar to a cometary coma. We use a magnetohydrodynamic model to quantitatively reproduce the 3-D shock surface at Ceres and deduce the atmosphere characteristics that are required to create such a shock. Our most simple model requires about 1.8 kg/s, or 6 × 1025/s water vapor production rate to form such a shock. Such an estimate relies on characteristics of the solar wind-Ceres interaction. We present several case studies to show how these conditions affect our estimate. In addition, we contrast these cases with the smaller and narrower shock caused by a subsurface induction. Our multifluid model reveals the asymmetry introduced by the large gyroradius of the heavy pickup ions and further constrains the IMF direction during the events.

  9. The earth's bow shock in an oblique interplanetary field.

    NASA Technical Reports Server (NTRS)

    Shen, W.-W.

    1972-01-01

    The pressure, magnetic field, temperature, particle density, and stream velocity throughout the magnetosheath have been calculated in the plane containing the interplanetary field and solar wind velocity vector for various orientations of the interplanetary magnetic field and various assumed ratios of specific heats of the compressed solar wind. Jump conditions at the bow shock gave initial conditions in the shocked plasma from which the appropriate hydromagnetic equations (for blunt bodies in the subsonic region near the subsolar point and for the method of characteristics in the supersonic region back in the tail) were integrated numerically back to the surface of the magnetosphere. Explicit consideration of the magnetic field shows that a net asymmetrical force on the magnetopause produces a side force, or 'lift' in addition to the well-known drag on the magnetosphere.

  10. On the kinematics and thickness of the terrestrial bow shock

    NASA Astrophysics Data System (ADS)

    Kruparova, Oksana; Krupar, Vratislav; Santolik, Ondrej; Soucek, Jan; Safrankova, Jana; Nemecek, Zdenek; Nemec, Frantisek; Maksimovic, Milan

    2017-04-01

    The bow shock (BS) is formed due to the continuous interaction between the supersonic solar wind and the Earth's magnetosphere ahead of the magnetopause. Thanks to its proximity, BS is a perfect object to study a wide range of phenomena related to collisionless shocks and wave-particle interactions. We have analyzed more than 500 quasi-perpendicular BS crossings between 2001 and 2015 using data retrieved by the magnetometers aboard the four Cluster spacecraft. Applying a simple timing method to four-point measurement, we estimated the BS normal direction and velocity along this direction case by case. Next, we applied the Butterworth filter to numerical derivations of time-intensity profiles to estimate temporal sizes of BS magnetic ramps, and consequently spatial ones using obtained velocities. We have found that BS ramp scales are statistically around 50 km. We discuss relation between the BS ramp scales and both Alfven and magnetosonic Mach numbers.

  11. Hybrid simulation techniques applied to the earth's bow shock

    NASA Technical Reports Server (NTRS)

    Winske, D.; Leroy, M. M.

    1985-01-01

    The application of a hybrid simulation model, in which the ions are treated as discrete particles and the electrons as a massless charge-neutralizing fluid, to the study of the earth's bow shock is discussed. The essentials of the numerical methods are described in detail; movement of the ions, solution of the electromagnetic fields and electron fluid equations, and imposition of appropriate boundary and initial conditions. Examples of results of calculations for perpendicular shocks are presented which demonstrate the need for a kinetic treatment of the ions to reproduce the correct ion dynamics and the corresponding shock structure. Results for oblique shocks are also presented to show how the magnetic field and ion motion differ from the perpendicular case.

  12. A Parsec-Size Bow Shock around Betelgeuse

    NASA Astrophysics Data System (ADS)

    Noriega-Crespo, Alberto; van Buren, Dave; Cao, Yu; Dgani, Ruth

    1997-08-01

    We present new High Resolution IRAS (HiRes) images at 60 and 100 \\mum of a bow shock or shell with a mean radius of 6arcmin surrounding Betelgeuse (alpha Orionis). The outermost section of this structure is at ~ 7arcmin which corresponds to a physical scale of 0.8 pc at a distance of 400 pc. The images were made by applying a relative Burg entropy maximization algorithm to suppress the ringing around bright sources and allow the detection of nearby low surface brightness features. The shell is relatively narrow at 60 \\mum (at the 1arcmin HiRes resolution), asymmetric and oriented along the star's direction of motion. We propose that the shell is confined by the ram pressure of the interstellar medium. Using a shell flux of 110 Jy (at 60 \\mum) within a radius of 7.arcmin5 we estimate mass of 0.14 \\msol for the shell.

  13. CHONDRULE FORMATION IN BOW SHOCKS AROUND ECCENTRIC PLANETARY EMBRYOS

    SciTech Connect

    Morris, Melissa A.; Desch, Steven J.; Athanassiadou, Themis; Boley, Aaron C.

    2012-06-10

    Recent isotopic studies of Martian meteorites by Dauphas and Pourmand have established that large ({approx}3000 km radius) planetary embryos existed in the solar nebula at the same time that chondrules-millimeter-sized igneous inclusions found in meteorites-were forming. We model the formation of chondrules by passage through bow shocks around such a planetary embryo on an eccentric orbit. We numerically model the hydrodynamics of the flow and find that such large bodies retain an atmosphere with Kelvin-Helmholtz instabilities allowing mixing of this atmosphere with the gas and particles flowing past the embryo. We calculate the trajectories of chondrules flowing past the body and find that they are not accreted by the protoplanet, but may instead flow through volatiles outgassed from the planet's magma ocean. In contrast, chondrules are accreted onto smaller planetesimals. We calculate the thermal histories of chondrules passing through the bow shock. We find that peak temperatures and cooling rates are consistent with the formation of the dominant, porphyritic texture of most chondrules, assuming a modest enhancement above the likely solar nebula average value of chondrule densities (by a factor of 10), attributable to settling of chondrule precursors to the midplane of the disk or turbulent concentration. We calculate the rate at which a planetary embryo's eccentricity is damped and conclude that a single planetary embryo scattered into an eccentric orbit can, over {approx}10{sup 5} years, produce {approx}10{sup 24} g of chondrules. In principle, a small number (1-10) of eccentric planetary embryos can melt the observed mass of chondrules in a manner consistent with all known constraints.

  14. Chondrule Formation in Bow Shocks around Eccentric Planetary Embryos

    NASA Astrophysics Data System (ADS)

    Morris, Melissa A.; Boley, Aaron C.; Desch, Steven J.; Athanassiadou, Themis

    2012-06-01

    Recent isotopic studies of Martian meteorites by Dauphas & Pourmand have established that large (~3000 km radius) planetary embryos existed in the solar nebula at the same time that chondrules—millimeter-sized igneous inclusions found in meteorites—were forming. We model the formation of chondrules by passage through bow shocks around such a planetary embryo on an eccentric orbit. We numerically model the hydrodynamics of the flow and find that such large bodies retain an atmosphere with Kelvin-Helmholtz instabilities allowing mixing of this atmosphere with the gas and particles flowing past the embryo. We calculate the trajectories of chondrules flowing past the body and find that they are not accreted by the protoplanet, but may instead flow through volatiles outgassed from the planet's magma ocean. In contrast, chondrules are accreted onto smaller planetesimals. We calculate the thermal histories of chondrules passing through the bow shock. We find that peak temperatures and cooling rates are consistent with the formation of the dominant, porphyritic texture of most chondrules, assuming a modest enhancement above the likely solar nebula average value of chondrule densities (by a factor of 10), attributable to settling of chondrule precursors to the midplane of the disk or turbulent concentration. We calculate the rate at which a planetary embryo's eccentricity is damped and conclude that a single planetary embryo scattered into an eccentric orbit can, over ~105 years, produce ~1024 g of chondrules. In principle, a small number (1-10) of eccentric planetary embryos can melt the observed mass of chondrules in a manner consistent with all known constraints.

  15. SPITZER OBSERVATIONS OF BOW SHOCKS AND OUTFLOWS IN RCW 38

    SciTech Connect

    Winston, E.; Wolk, S. J.; Bourke, T. L.; Spitzbart, B.; Megeath, S. T.; Gutermuth, R.

    2012-01-10

    We report Spitzer observations of five newly identified bow shocks in the massive star-forming region RCW 38. Four are visible at Infrared Array Camera (IRAC) wavelengths, the fifth is only visible at 24 {mu}m. Chandra X-ray emission indicates that winds from the central O5.5 binary, IRS 2, have caused an outflow to the northeast and southwest of the central subcluster. The southern lobe of hot ionized gas is detected in X-rays; shocked gas and heated dust from the shock front are detected with Spitzer at 4.5 and 24 {mu}m. The northern outflow may have initiated the present generation of star formation, based on the filamentary distribution of the protostars in the central subcluster. Further, the bow-shock driving star, YSO 129, is photo-evaporating a pillar of gas and dust. No point sources are identified within this pillar at near- to mid-IR wavelengths. We also report on IRAC 3.6 and 5.8 {mu}m observations of the cluster DBS2003-124, northeast of RCW 38, where 33 candidate young stellar objects (YSOs) are identified. One star associated with the cluster drives a parsec-scale jet. Two Herbig-Haro objects associated with the jet are visible at IRAC and Multiband Imaging Photometer for Spitzer (MIPS) wavelengths. The jet extends over a distance of {approx}3 pc. Assuming a velocity of 100 km s{sup -1} for the jet material gives an age of 3 Multiplication-Sign 10{sup 4} yr, indicating that the star (and cluster) are likely to be very young, with a similar or possibly younger age than RCW 38, and that star formation is ongoing in the extended RCW 38 region.

  16. Violin Pedagogy and the Physics of the Bowed String

    NASA Astrophysics Data System (ADS)

    McLeod, Alexander Rhodes

    The paper describes the mechanics of violin tone production using non-specialist language, in order to present a scientific understanding of tone production accessible to a broad readership. As well as offering an objective understanding of tone production, this model provides a powerful tool for analyzing the technique of string playing. The interaction between the bow and the string is quite complex. Literature reviewed for this study reveals that scientific investigations have provided important insights into the mechanics of string playing, offering explanations for factors which both contribute to and limit the range of tone colours and dynamics that stringed instruments can produce. Also examined in the literature review are significant works of twentieth century violin pedagogy exploring tone production on the violin, based on the practical experience of generations of teachers and performers. Hermann von Helmholtz described the stick-slip cycle which drives the string in 1863, which replaced earlier ideas about the vibration of violin strings. Later, scientists such as John Schelleng and Lothar Cremer were able to demonstrate how the mechanics of the bow-string interaction can create different tone colours. Recent research by Anders Askenfelt, Knut Guettler, and Erwin Schoonderwaldt have continued to refine earlier research in this area. The writings of Lucien Capet, Leopold Auer, Carl Flesch, Paul Rolland, Kato Havas, Ivan Galamian, and Simon Fischer are examined and analyzed. Each author describes a different approach to tone production on the violin, representing a different understanding of the underlying mechanism. Analyzing these writings within the context of a scientific understanding of tone production makes it possible to compare these approaches more consistently, and to synthesize different concepts drawn from the diverse sources evaluated.

  17. Investigating the function of play bows in adult pet dogs (Canis lupus familiaris).

    PubMed

    Byosiere, Sarah-Elizabeth; Espinosa, Julia; Smuts, Barbara

    2016-04-01

    Play bows are a common, highly stereotyped canine behavior widely considered to be a 'play signal,' but only one study has researched their function. Bekoff (1995) found that play bows function as behavioral modifiers to help clarify playful intent before or after easily misinterpretable behaviors, such as bite-shakes. To further examine the function of play bows, the current study analyzed five types of behaviors displayed by the bower and the partner immediately before and after a play bow during dyadic play. We found that play bows most often occurred after a brief pause in play. Synchronous behaviors by the bower and the partner, or vulnerable/escape behaviors by the bower (such as running away) and complementary offensive behaviors by the partner (such as chasing) occurred most often after the play bow. These results indicate that during adult dog dyadic play, play bows function to reinitiate play after a pause rather than to mediate offensive or ambiguous actions. Copyright © 2016 Elsevier B.V. All rights reserved.

  18. Using numerical models of bow shocks to investigate the circumstellar medium of massive stars

    NASA Astrophysics Data System (ADS)

    van Marle, A. J.; Decin, L.; Cox, N. L. J.; Meliani, Z.

    2015-01-01

    Many massive stars travel through the interstellar medium at supersonic speeds. As a result they form bow shocks at the interface between the stellar wind. We use numerical hydrodynamics to reproduce such bow shocks numerically, creating models that can be compared to observations. In this paper we discuss the influence of two physical phenomena, interstellar magnetic fields and the presence of interstellar dust grains on the observable shape of the bow shocks of massive stars. We find that the interstellar magnetic field, though too weak to restrict the general shape of the bow shock, reduces the size of the instabilities that would otherwise be observed in the bow shock of a red supergiant. The interstellar dust grains, due to their inertia can penetrate deep into the bow shock structure of a main sequence O-supergiant, crossing over from the ISM into the stellar wind. Therefore, the dust distribution may not always reflect the morphology of the gas. This is an important consideration for infrared observations, which are dominated by dust emission. Our models clearly show, that the bow shocks of massive stars are useful diagnostic tools that can used to investigate the properties of both the stellar wind as well as the interstellar medium.

  19. Bow Shocks from Neutron Stars: Scaling Laws and Hubble Space Telescope Observations of the Guitar Nebula

    NASA Astrophysics Data System (ADS)

    Chatterjee, S.; Cordes, J. M.

    2002-08-01

    The interaction of high-velocity neutron stars with the interstellar medium produces bow shock nebulae, in which the relativistic neutron star wind is confined by ram pressure. We present multiwavelength observations of the Guitar Nebula, including narrowband Hα imaging with Hubble Space Telescope (HST) WFPC2, which resolves the head of the bow shock. The HST observations are used to fit for the inclination of the pulsar velocity vector to the line of sight and to determine the combination of spin-down energy loss, velocity, and ambient density that sets the scale of the bow shock. We find that the velocity vector is most likely in the plane of the sky. We use the Guitar Nebula and other observed neutron star bow shocks to test scaling laws for their size and Hα emission, discuss their prevalence, and present criteria for their detectability in targeted searches. The set of Hα bow shocks shows remarkable consistency, in spite of the expected variation in ambient densities and orientations. Together, they support the assumption that a pulsar's spin-down energy losses are carried away by a relativistic wind that is indistinguishable from being isotropic. Comparison of Hα bow shocks with X-ray and nonthermal radio-synchrotron bow shocks produced by neutron stars indicates that the overall shape and scaling is consistent with the same physics. It also appears that nonthermal radio emission and Hα emission are mutually exclusive in the known objects and perhaps in all objects.

  20. Systematic search for high-energy gamma-ray emission from bow shocks of runaway stars

    SciTech Connect

    Schulz, A.; Ackermann, M.; Buehler, R.; Mayer, M.; Klepser, S.

    2014-05-01

    Context. It has been suggested that the bow shocks of runaway stars are sources of high-energy gamma rays (E > 100 MeV). Theoretical models predicting high-energy gamma-ray emission from these sources were followed by the first detection of non-thermal radio emission from the bow shock of BD+43°3654 and non-thermal X-ray emission from the bow shock of AE Aurigae. Aims. We perform the first systematic search for MeV and GeV emission from 27 bow shocks of runaway stars using data collected by the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope (Fermi). Methods. We analysed 57 months of Fermi-LAT data at the positions of 27 bow shocks of runaway stars extracted from the Extensive stellar BOw Shock Survey catalogue (E-BOSS). A likelihood analysis was performed to search for gamma-ray emission that is not compatible with diffuse background or emission from neighbouring sources and that could be associated with the bow shocks. Results. None of the bow shock candidates is detected significantly in the Fermi-LAT energy range. We therefore present upper limits on the high-energy emission in the energy range from 100MeV to 300 GeV for 27 bow shocks of runaway stars in four energy bands. For the three cases where models of the high-energy emission are published we compare our upper limits to the modelled spectra. Our limits exclude the model predictions for ζ Ophiuchi by a factor ≈ 5.

  1. Systematic search for high-energy gamma-ray emission from bow shocks of runaway stars

    DOE PAGES

    Schulz, A.; Ackermann, M.; Buehler, R.; ...

    2014-05-01

    Context. It has been suggested that the bow shocks of runaway stars are sources of high-energy gamma rays (E > 100 MeV). Theoretical models predicting high-energy gamma-ray emission from these sources were followed by the first detection of non-thermal radio emission from the bow shock of BD+43°3654 and non-thermal X-ray emission from the bow shock of AE Aurigae. Aims. We perform the first systematic search for MeV and GeV emission from 27 bow shocks of runaway stars using data collected by the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope (Fermi). Methods. We analysed 57 months of Fermi-LATmore » data at the positions of 27 bow shocks of runaway stars extracted from the Extensive stellar BOw Shock Survey catalogue (E-BOSS). A likelihood analysis was performed to search for gamma-ray emission that is not compatible with diffuse background or emission from neighbouring sources and that could be associated with the bow shocks. Results. None of the bow shock candidates is detected significantly in the Fermi-LAT energy range. We therefore present upper limits on the high-energy emission in the energy range from 100MeV to 300 GeV for 27 bow shocks of runaway stars in four energy bands. For the three cases where models of the high-energy emission are published we compare our upper limits to the modelled spectra. Our limits exclude the model predictions for ζ Ophiuchi by a factor ≈ 5.« less

  2. Bowing of marble panels: On-site damage analysis from the oeconomicum building at Goettingen (Germany)

    NASA Astrophysics Data System (ADS)

    Koch, A.; Siegesmund, S.

    2003-04-01

    The use of natural stone panels or cladding material for building facades has led to some durability problems, especially with marble slabs. To examine the effects of intrinsic and extrinsic parameters on bowing a very detailed study was performed on the Oeconomicum Building at the University of Goettingen. In total 1556 panels from the whole building were measured with respect to the bowing using a bow-meter. The variation of bowing ranges from concave (up to 23 mm/m) to convex (up to -11 mm/m). The variation is not controlled by the position with respect to the geographical coordinates, height above ground, shadows, temperature etc.. On the north facade the different rock structures visible on the panel surfaces are a result of the marble slabs being cut in different directions. The different degree in bowing is associated with the structure of the marble since all other influencing factors are relatively constant (position, temperature, moisture content, building physics). Experimental data on the expansion behaviour under dry and/or wet conditions reveal a different degree in bowing with respect to the rock fabric and may help to explain the observed differences in bowing. The effect of the rock fabric especially of the lattice preferred orientation in this case clearly controls the deterioration of the marble and the degree of bowing. The bowing is also characterized by an increase in the porosity, decreasing values of ultrasonic wave velocities and flexural strength. The loss of cohesion in the strongly deteriorated panels is clearly visible in the microstructure by the open grain boundaries which are interconnected to intergranular microcracks.

  3. The occurrence of convective systems with a bow echo in warm season in Poland

    NASA Astrophysics Data System (ADS)

    Celiński-Mysław, Daniel; Palarz, Angelika

    2017-09-01

    The characteristics of occurrence of convective systems with a bow echo in Poland in the warm season between 2007 and 2014 were presented. Using the identification criteria proposed by Fujita (1978), Burke and Schultz (2004), Klimowski et al. (2000, 2004), and supplemented by Gatzen (2013), 91 bow echo cases were identified in the analysed period. Depending on the year, the maximum number of cases usually occurred in July or August. From the multi-annual perspective, 28 and 30 cases occurred in those months. The diurnal variation of bow echo occurrences showed that it developed, or entered the Polish territory, usually between the hours of 13:00 UTC and 21:00 UTC, while it disappeared or receded beyond the country border in the hours between 15:00 UTC and 23:00 UTC. The areas most exposed to the occurrence of bow echo included the northern part of Lubuskie and Wielkopolska provinces, the southern part of West Pomerania province, Łódź province and Silesia province. In the period studied, the south-western direction of movement of convective systems with a bow echo was prevalent. This direction changed, however, depending on the region and the month of occurrence. The type and development mode of a bow echo, as well as synoptic conditions conducive to its occurrence were defined for selected cases. The results showed that BECs (bow-echo complex) and BEs (classic bow echo) were the predominant types (respectively 43 and 29 cases). Bow echoes developed most frequently from a squall line, or from a combination of a few, often weakly organized convective cells.

  4. Square and bow-tie configurations in the cyclic evasion problem

    NASA Astrophysics Data System (ADS)

    Arnold, M. D.; Golich, M.; Grim, A.; Vargas, L.; Zharnitsky, V.

    2017-05-01

    Cyclic evasion of four agents on the plane is considered. There are two stationary shapes of configurations: square and degenerate bow-tie. The bow-tie is asymptotically attracting while the square is of focus-center type. Normal form analysis shows that square is nonlinearly unstable. The stable manifold consists of parallelograms that all converge to the square configuration. Based on these observations and numerical simulations, it is conjectured that any non-parallelogram non-degenerate configuration converges to the bow-tie.

  5. Pioneer 8 plasma-wave measurements at distant bow-shock crossings.

    NASA Technical Reports Server (NTRS)

    Scarf, F. L.

    1971-01-01

    Evaluation of enhanced low-frequency plasma-wave levels detected near the Pioneer 8 multiple bow-shock crossings encountered beyond 120 earth radii (Bavassano et al., 1971) and of high-frequency plasma waves detected in the upstream region. It is suggested that the distant interaction of the solar wind and the magnetosheath produced nonthermal electrons of the type commonly found upstream from the subsolar shock. The bow-shock position is compared with fluid model predictions, and some distinctions between the standing bow shock and the propagating interplanetary shock are considered.

  6. Lower hybrid waves upstream of comets and their implications for the Comet Halley 'bow wave'

    NASA Technical Reports Server (NTRS)

    Hizanidis, K.; Cargill, P. J.; Papadopoulos, K.

    1988-01-01

    Observed and theoretical features concerning the nature of so-called cometary 'bow shocks' or 'bow waves' are discussed. Collective plasma effects associated with the presence of pickup ring ions (protons and water ions) in the vicinity of the supermagnetosonic to submagnetosonic transition region in the quasi-perpendicular limit are considered; the linear and nonlinear evolution of instabilities around the lower hybrid frequency is emphasized. It is shown that lower hybrid waves can lead to heating and produce distributions with magnitudes in reasonable agreement with Giotto data. The implications to the existence and structure of cometary bow shocks are discussed.

  7. Bowing-reactivity trends in EBR-II assuming zero-swelling ducts

    SciTech Connect

    Meneghetti, D.

    1994-03-01

    Predicted trends of duct-bowing reactivities for the Experimental Breeder Reactor II (EBR-II) are correlated with predicted row-wise duct deflections assuming use of idealized zero-void-swelling subassembly ducts. These assume no irradiation induced swellings of ducts but include estimates of the effects of irradiation-creep relaxation of thermally induced bowing stresses. The results illustrate the manners in which at-power creeps may affect subsequent duct deflections at zero power and thereby the trends of the bowing component of a subsequent power reactivity decrement.

  8. A hybrid NRPS-PKS gene cluster related to the bleomycin family of antitumor antibiotics in Alteromonas macleodii strains.

    PubMed

    Mizuno, Carolina Megumi; Kimes, Nikole E; López-Pérez, Mario; Ausó, Eva; Rodriguez-Valera, Francisco; Ghai, Rohit

    2013-01-01

    Although numerous marine bacteria are known to produce antibiotics via hybrid NRPS-PKS gene clusters, none have been previously described in an Alteromonas species. In this study, we describe in detail a novel hybrid NRPS-PKS cluster identified in the plasmid of the Alteromonasmacleodii strain AltDE1 and analyze its relatedness to other similar gene clusters in a sequence-based characterization. This is a mobile cluster, flanked by transposase-like genes, that has even been found inserted into the chromosome of some Alteromonasmacleodii strains. The cluster contains separate genes for NRPS and PKS activity. The sole PKS gene appears to carry a novel acyltransferase domain, quite divergent from those currently characterized. The predicted specificities of the adenylation domains of the NRPS genes suggest that the final compound has a backbone very similar to bleomycin related compounds. However, the lack of genes involved in sugar biosynthesis indicates that the final product is not a glycopeptide. Even in the absence of these genes, the presence of the cluster appears to confer complete or partial resistance to phleomycin, which may be attributed to a bleomycin-resistance-like protein identified within the cluster. This also suggests that the compound still shares significant structural similarity to bleomycin. Moreover, transcriptomic evidence indicates that the NRPS-PKS cluster is expressed. Such sequence-based approaches will be crucial to fully explore and analyze the diversity and potential of secondary metabolite production, especially from increasingly important sources like marine microbes.

  9. Crystal Structure of Mycobacterium tuberculosis Polyketide Synthase 11 (PKS11) Reveals Intermediates in the Synthesis of Methyl-branched Alkylpyrones*

    PubMed Central

    Gokulan, Kuppan; O'Leary, Seán E.; Russell, William K.; Russell, David H.; Lalgondar, Mallikarjun; Begley, Tadhg P.; Ioerger, Thomas R.; Sacchettini, James C.

    2013-01-01

    PKS11 is one of three type III polyketide synthases (PKSs) identified in Mycobacterium tuberculosis. Although many PKSs in M. tuberculosis have been implicated in producing complex cell wall glycolipids, the biological function of PKS11 is unknown. PKS11 has previously been proposed to synthesize alkylpyrones from fatty acid substrates. We solved the crystal structure of M. tuberculosis PKS11 and found the overall fold to be similar to other type III PKSs. PKS11 has a deep hydrophobic tunnel proximal to the active site Cys-138 to accommodate substrates. We observed electron density in this tunnel from a co-purified molecule that was identified by mass spectrometry to be palmitate. Co-crystallization with malonyl-CoA (MCoA) or methylmalonyl-CoA (MMCoA) led to partial turnover of the substrate, resulting in trapped intermediates. Reconstitution of the reaction in solution confirmed that both co-factors are required for optimal activity, and kinetic analysis shows that MMCoA is incorporated first, then MCoA, followed by lactonization to produce methyl-branched alkylpyrones. PMID:23615910

  10. Earth’s bow shock dynamics and structure scales based on MMS multi-spacecraft data

    NASA Astrophysics Data System (ADS)

    Alrefay, T. Y.

    2017-06-01

    Space plasmas studies on bow shock dynamics and structure scales continue to attract intense theoretical and experimental investigations. The Earth’s bow shock is the closest shock accessible to scientists through various satellite missions. These missions have enabled investigations on different physical phenomena associated with solar-terrestrial interaction. Access to the interplanetary medium through satellites has provided access to valuable spatial and temporal data on the Earth bow shock, and has furthered understanding on certain aspects of shock physics that were inaccessible until now. The main objective of this study is to quantify the dynamics and structure scales of the Earth’s bow shock using data obtained by the MMS multi-spacecraft during shock crossing.

  11. Energetic ions upstream of the earth's bow shock during an energetic storm particle event

    NASA Technical Reports Server (NTRS)

    Scholer, M.; Ipavich, F. M.

    1983-01-01

    Simultaneous observations of low-energy protons and alpha particles from ISEE 3 far upstream and from ISEE 1 close to the earth's bow shock during the passage of an interplanetary shock wave with its associated energetic storm particles are presented. Intensities, spectra, and anisotropies of the energetic storm particles are modified due to the interaction of these particles with the earth's bow shock. An intensity spike observed at ISEE 1 during the passage of the interplanetary shock is interpreted as being due to postacceleration of energetic storm particles at the bow shock by the first-order Fermi mechanism. The spikes observed at ISEE 1 after the passage of the interplanetary shock are most probably due to reflection of the energetic storm particles at the bow shock.

  12. Christmas bow pins: a potential inhaled foreign body made safer by industrial modifications.

    PubMed

    Siegel, L G; Mendenhall, H V; Liston, S L

    1981-01-01

    The 3M Company (Minnesota Mining and Manufacturing Company) has produced about three billion plastic Christmas bow pins over 20 years. When it was reported that inhalation of these pins had resulted in two deaths, the company sought otolaryngologic consultation to suggest design modifications which would decrease the risk of aspiration asphyxia. The circular base of the bow pin was modified into the form of a cross so that it would not completely obstruct the airway. Barium was added to render the bow pin radiopaque. When the unmodified bow pin was inserted into the larynx of ten cats, six died. The modified pin caused no deaths in nine cats. We regard this as an example of responsible cooperation between industry and medicine.

  13. Oxygen foreshock of Mars and its implication on ion acceleration in the bow shock

    NASA Astrophysics Data System (ADS)

    Yamauchi, Masatoshi; Lundin, Rickard; Frahm, Rudy; Sauvaud, Jean-Andre; Holmstrom, Mats; Barabash, Stas

    2016-04-01

    Ion acceleration inside the bow shock is one of the poorly understood phenomena that has been observed for more than 30 years as the foreshock phenomena. While the Fermi-acceleration mechanism explains the diffuse component of foreshock ions, we still do not know the detailed mechanism that produces the discrete intense ions flowing along the local magnetic field direction (with and without gyration). One of the reasons for such difficulty is that majority of the bow shock study was performed for the Earth's case where Oxygen ions cannot be used to understand the acceleration mechanisms. The planetary oxygen ions that reach the Earth's bow shock have already been significantly accelerated, and are not adequate for such a study. In this sense the Martian bow shock is an ideal place to study the acceleration mechanisms leading to foreshock ions, although the nature of the bow shock is slightly different between the Earth and Mars (Yamauchi et al., 2011). On 21 September 2008, the Mars Express (MEX) Ion Mass Analyser (IMA) detected foreshock-like discrete distributions of oxygen ions at around 1 keV in the solar wind attached to the bow shock. This was the first time that a substantial amount of planetary oxygen was observed upstream of the bow shock. The oxygen energy increased from low energy (< 300 keV) inside the magnetosheath (or it should be called an extended bow shock) to nearly 2 keV at more than 2000 km from the bow shock. Foreshock-like protons are also observed but at a shifted location from the oxygen by about 1000 km, at a slightly higher energy, and flowing in a slightly different direction than the oxygen ions. Both protons and oxygen ions are flowing anti-sunward at different angles with respect to the solar wind direction. The observation is consistent with an electric potential barrier at the bow shock that simultaneously accelerates the planetary oxygen ions outward (to form the foreshock oxygen ions) and reflects a portion of the solar wind (to

  14. MESSENGER observations of Mercury's bow shock and magnetopause

    NASA Astrophysics Data System (ADS)

    Slavin, J. A.; Acuña, M. H.; Anderson, B. J.; Benna, M.; Gloeckler, G.; Krimigis, S. M.; Raines, J. M.; Schriver, D.; Trávníček, P.; Zurbuchen, T. H.

    2008-09-01

    Abstract The MESSENGER spacecraft made the first of three flybys of Mercury on January 14, 2008 (1). New observations of solar wind interaction with Mercury were made with MESSENGER's Magnetometer (MAG) (2,3) and Energetic Particle and Plasma Spectrometer (EPPS) - composed of the Energetic Particle Spectrometer (EPS) and Fast Imaging Plasma Spectrometer (FIPS) (3,4). These MESSENGER observations show that Mercury's magnetosphere has a large-scale structure that is distinctly Earth-like, but it is immersed in a comet-like cloud of planetary ions [5]. Fig. 1 provides a schematic view of the coupled solar wind - magnetosphere - neutral atmosphere - solid planet system at Mercury. Here we present new models of bow shock and magnetopause shape and location that incorporate both the MESSENGER and earlier Mariner 10 measurements of these boundaries. A fast magnetosonic Mach number for the solar wind at Mercury's distance from the Sun of ~ 3 is derived from the shape of the bow shock. This value is consistent with earlier observations at these distances from the Sun by the Helios mission. The shape of Mercury's magnetopause and the thickness of the magnetosheath are found to be similar to that of the Earth, suggesting that the solar wind interaction is dominated by its dipolar magnetic field. MESSENGER measurements near the magnetopause do, however, indicate that internal plasma pressure does contribute to the pressure balance across this boundary. MAG and FIPS measurements are used to estimate the ratio of plasma thermal pressure to magnetic pressure at the dusk flank of the plasma sheet and dawn terminator regions, under the assumption that pressure is balanced across the inbound and outbound magnetopause crossings. To investigate the possible origins of the plasma ions in these regions, we utilize a combination of FIPS measurements and the results of 3-D hybrid [6] and magnetohydrodynamic simulations of the solar wind interaction with Mercury for the upstream conditions

  15. Extended red objects and stellar-wind bow shocks in the Carina Nebula

    NASA Astrophysics Data System (ADS)

    Sexton, Remington O.; Povich, Matthew S.; Smith, Nathan; Babler, Brian L.; Meade, Marilyn R.; Rudolph, Alexander L.

    2015-01-01

    We report the results of infrared photometry on 39 extended red objects (EROs) in the Carina Nebula, observed with the Spitzer Space Telescope. Most EROs are identified by bright, extended 8.0 μm emission, which ranges from 10 arcsec to 40 arcsec in size, but our sample also includes four EROs identified by extended 24 μm emission. Of particular interest are nine EROs associated with late O- or early B-type stars and characterized by arc-shaped morphology, suggesting dusty, stellar-wind bow shocks. These objects are preferentially oriented towards the central regions of the Carina Nebula, suggesting that these bow shocks are generally produced by the interactions of OB winds with the bulk expansion of the H II region rather than high proper motion. We identify preferred regions of mid-infrared colour space occupied by our bow shock candidates, which also contain bow shock candidates in M17 and RCW 49 but are well separated from polycyclic aromatic hydrocarbon emission or circumstellar discs. Colour cuts identify an additional 12 marginally resolved bow shock candidates, 10 of which are also associated with known late O or early B stars. H II region expansion velocities derived from bow shock candidate standoff distances are ˜10 km s-1, assuming typical H II region gas densities, comparable to expansion velocities derived from bow shocks in M17 and RCW 49. One candidate bow shock provides direct evidence of physical interaction between the massive stellar winds originating in the Trumpler 15 and Trumpler 14 clusters, supporting the conclusion that both clusters are at similar heliocentric distances.

  16. On the observability of bow shocks of Galactic runaway OB stars

    NASA Astrophysics Data System (ADS)

    Meyer, D. M.-A.; van Marle, A.-J.; Kuiper, R.; Kley, W.

    2016-06-01

    Massive stars that have been ejected from their parent cluster and supersonically sailing away through the interstellar medium (ISM) are classified as exiled. They generate circumstellar bow-shock nebulae that can be observed. We present two-dimensional, axisymmetric hydrodynamical simulations of a representative sample of stellar wind bow shocks from Galactic OB stars in an ambient medium of densities ranging from nISM = 0.01 up to 10.0 cm- 3. Independently of their location in the Galaxy, we confirm that the infrared is the most appropriated waveband to search for bow shocks from massive stars. Their spectral energy distribution is the convenient tool to analyse them since their emission does not depend on the temporary effects which could affect unstable, thin-shelled bow shocks. Our numerical models of Galactic bow shocks generated by high-mass ( ≈ 40 M⊙) runaway stars yield H α fluxes which could be observed by facilities such as the SuperCOSMOS H-Alpha Survey. The brightest bow-shock nebulae are produced in the denser regions of the ISM. We predict that bow shocks in the field observed at H α by means of Rayleigh-sensitive facilities are formed around stars of initial mass larger than about 20 M⊙. Our models of bow shocks from OB stars have the emission maximum in the wavelength range 3 ≤ λ ≤ 50 μm which can be up to several orders of magnitude brighter than the runaway stars themselves, particularly for stars of initial mass larger than 20 M⊙.

  17. The solar cycle dependence of the location and shape of the Venus bow shock

    NASA Technical Reports Server (NTRS)

    Zhang, T.-L.; Luhmann, J. G.; Russell, C. T.

    1990-01-01

    The Venus terminator bow shock position is monitored and it is shown that the shock radius increases as the solar cycle approaches a new maximum. It is also shown that the subsolar bow shock changes with the solar cycle, and that these positions are correlated with each other and with solar activity. It is hypothesized that, at solar minimum, the magnetic barrier is weak, and that some absorption of solar wind is to be expected.

  18. A Global 3D Bow Shock Model Valid for a Wide Range of Upstream Mach Numbers

    NASA Astrophysics Data System (ADS)

    Merka, Jan; Sibeck, David; Wang, Yongli

    2014-05-01

    Interaction of the supersonic solar wind with Earth's magnetosphere creates fast mode magnetosonic waves that travel back upstream, combine and steepen to form the bow shock wave. The bow shock wave has been studied for more than four decades but existing models are still often inaccurate. Previous studies established that bow shock shape and position are primarily controlled by solar wind pressure, upstream Mach numbers, interplanetary magnetic ?eld orientation and magnetopause shape and position. We have collected a total of 28,287 bow shock crossings identi?ed in observations from the Cluster 1-4, Geotail, IMP-8, Interball-1, MAGION-4, THEMIS A-E and WIND spacecraft and use this database to predict bow shock position as a function of solar wind parameters. The large dataset appeared sufficient for employing a modelling technique that does not assume a prescribed shock shape to eliminate a potential bias: The Support Vector Regression Machine (SVRM) technique for mapping multi-dimensional data into a high- dimensional feature space via nonlinear mapping through a selected kernel function and performing a linear regression in this space. After a thorough study, we have concluded that even though the employed number of shock crossings is the largest used by at least an order of magnitude, the fitted data points are still unevenly distributed in the modeled phase space and that severely limits the validity and applicability of the SVRM-produced bow shock models. Therefore, the same database of bow shock crossings is fitted using a method similar to Peredo et al. [1995] which presumes a general 3D second-order bow shock shape parameterized by the upstream dynamic pressure and Alfven Mach number values. The use of a prescribed shock shape results in a model that provides accurate predictions for Alfven Mach numbers as low as 2 and can be used with confidence up to 40 Re along the magnetotail.

  19. Congenital tibial dysplasia with lateral bowing and duplication of hallux: case presentations.

    PubMed

    Beck, Jennifer J; Altiok, Haluk

    2013-05-01

    This article reports on two children with congenital unilateral tibial dysplasia with lateral bowing with no associated sagittal plane deformity. In both cases, it is associated with ipsilateral duplication of the hallux. Long-term follow-up of the patients showed spontaneous, almost complete resolution of the bowing without progressing into fracture or pseudoarthrosis. Leg length discrepancy appeared to be the only orthopedic sequela related to this phenomenon.

  20. 3D Bow Shock Modeling with and without Apriori Prescribed Shock Shapes

    NASA Astrophysics Data System (ADS)

    Merka, J.; Wang, Y.; Sibeck, D. G.

    2013-12-01

    Interaction of the supersonic solar wind with Earth's magnetosphere creates fast mode magnetosonic waves that travel back upstream, combine and steepen to form the bow shock wave. The bow shock wave has been studied for more than four decades but existing models are still often inaccurate. Previous studies established that bow shock shape and position are primarily controlled by solar wind pressure PSW , upstream Mach numbers, interplanetary magnetic field orientation and magnetopause shape and position. Our study employs the Support Vector Regression Machine (SVRM) technique for mapping multi-dimensional data into a high- dimensional feature space via nonlinear mapping through a selected kernel function and performing a linear regression in this space. The use of SVRM means that there is no apriori prescribed shock shape. In addition to SVRM, the bootstrap technique is employed for error calculations in contrast to existing shock models that rarely provide any error estimates at all. We fit a total of 28,287 bow shock crossings identified in observations from the Cluster 1-4, Geotail, IMP-8, Interball-1, MAGION-4, THEMIS A-E and WIND spacecraft. Even thought the employed number of shock crossings is the largest used by at least an order of magnitude, the fitted data points are still unevenly distributed in the modeled phase space and that significantly limits the validity of the SVRM-produced bow shock models under certain upstream conditions. Therefore, the same database of bow shock crossings is fitted using a method similar to Peredo et al. [1995] which presumes a general 3D second-order bow shock shape parametrized by the upstream dynamic pressure and Alfven Mach number values. The use of a prescribed shock shape results in a model usable and more accurate even at the night-side magnetosphere as opposed to a SVRM-based model. We will further discuss in detail the advantages of either method and propose a bow shock model combining both approaches.

  1. The use of palm kernel shell (PKS) as substrate material in vertical-flow engineered wetlands for septage treatment in Malaysia.

    PubMed

    Jong, Valerie Siaw Wee; Tang, Fu Ee

    2015-01-01

    In this study, the treatment of septage (originating from septic tanks) was carried out in a pilot-scale, two-staged, vertical-flow engineered wetland (VFEW). Palm kernel shells (PKS) were incorporated as part of the VFEW's substrate (B-PKS), to compare its organic matter (OM) and nitrogen (N) removal efficiency against wetlands with only sand substrates (B-SD). The results revealed satisfactory OM removal with >90% reduction efficiencies at both wetlands B-PKS and B-SD. No increment of chemical oxygen demand (COD) concentration was observed in the effluent of B-PKS. Ammonia load removal efficiencies were comparable (>91% and 95% in wetland B-PKS and B-SD, respectively). However, nitrate accumulation was observed in the effluent of B-SD where PKS was absent. This was due to the limited denitrification in B-SD, as sand is free of carbon. A lower nitrate concentration was associated with higher COD concentration in the effluent at B-PKS. This study has shown that the use of PKS was effective in improving the N removal efficiency in engineered wetlands.

  2. The dipole tilt angle dependence of the bow shock for southward IMF: MHD results

    NASA Astrophysics Data System (ADS)

    Wang, M.; Lu, J. Y.; Yuan, H. Z.; Kabin, K.; Liu, Z.-Q.; Zhao, M. X.; Li, G.

    2015-02-01

    The location and shape of the Earth's bow shock depend on the properties of the upstream solar wind, as well as the size and shape of the downstream magnetopause. Many studies have suggested that the influence of the dipole tilt angle on the magnetopause is significant, especially at the high-latitude region, however, to date there is no bow shock model which depends on the dipole tilt angle. Using a physics-based global magnetohydrodynamic (MHD) model, the Space Weather Modeling Framework (SWMF), we investigate the effect of the dipole tilt angle on the location and shape of the bow shock, and our results show that (1) the subsolar standoff distance and the north-south asymmetry of bow shock increase with the increasing dipole tilt angle; (2) with the dipole tilt angle positively increasing, the flaring angle of the bow shock increases in the northern hemisphere but keeps almost unchanged in the southern hemisphere, and the rotational asymmetry slightly decreases in the northern hemisphere and rapidly decreases in the southern hemisphere; and (3) the influence of dipole tilt angle on the shape of the bow shock is north-south symmetric.

  3. Bow Shocks Around Runaway Stars.III.The High Resolution Maps

    NASA Astrophysics Data System (ADS)

    Noriega-Crespo, Alberto; van Buren, Dave; Dgani, Ruth

    1997-02-01

    In a recent survey for bow shock structures around OB runaway stars using the ISSA/IRAS archival data and excess maps at 60 \\mum, 58 candidates were found. These objects are surrounded by extended infrared emission at 60 \\mum, characteristic of warm dust heated by ultraviolet photons, a signature of wind bow shocks. High resolution IRAS (HiRes) images have been produced for these 58 objects and some of those spatially resolved are presented in this study. The images were used to distinguish between multiple confused IR sources, possible artifacts and unambiguous bow shocks, as the sources of the extended 60 \\mum emission. Six new bow shocks have been identified using this method, and three have been rejected. Twenty two of the targets, however, remain spatially unresolved even at the nominal HiRes resolution of ~ 1arcmin . For the larger and better defined bow shocks some internal substructure is discernible. The length of these features suggest that they arise as the result of a subtle dynamical instability. It can not be ruled out, however, that some of the bow shock morphology could be imprinted by the surrounding medium.

  4. A variable cross-section model of the bow shock of Venus

    NASA Technical Reports Server (NTRS)

    Khurana, Krishan K.; Kivelson, Margaret G.

    1994-01-01

    Magnetohydrodynamics (MHD) parameters like the Alfvenic and the sonic Mach numbers and the direction of the interplanetary magnetic field profoundly affect the interaction of the solar wind with nonmagnetized conducting objects like Venus. The size of the bow shock depends on the two Mach numbers, whereas asymmetries in its shape are governed by the direction of the magnetic field. This paper introduces a new class of bow shock models in which both the shape and the size are controlled by the upstream plasma and field conditions. We use insights from the MHD theory of shocks for point objects and empirical information from actual bow shock crossings to obtain a semiempirical, semitheoretical model of the Cytherean bow shock. The model was developed from a limited data set obtained from the Galileo flyby of Venus but is also in substantial agreement with Pioneer Venus Orbiter observations. It is shown that the dozen bow shock crossing observed by Galileo under steady conditions of solar wind flow and density were caused by changes in the cross section of the bow shock induced by the changing direction of the interplanetary magnetic field.

  5. Observations of bow shocks of runaway stars with H.E.S.S.

    NASA Astrophysics Data System (ADS)

    Schulz, A.; Haupt, M.; Klepser, S.; Ohm, S.

    2017-01-01

    Runaway stars form bow shocks by sweeping up interstellar matter in their direction of motion. Theoretical models predict a spectrally wide non-thermal component reaching up to gamma-ray energies at a flux level detectable with current instruments. They were motivated by a detection of non-thermal radio emission from the bow shock of BD+43°3654 and a possible detection of non-thermal X-rays from AE Aurigae. A search in the high-energy regime using data from Fermi-LAT resulted in flux upper limits for 27 candidates listed in the first E-BOSS catalogue. We perform the first systematic search for TeV emission from bow shocks of runaway stars. Using all available archival H.E.S.S. I data we search for very-high-energy gamma-ray emission at the positions of bow shock candidates listed in the second E-BOSS catalogue. This catalogue comprises 73 bow shock candidates, 32 of which have been observed with the H.E.S.S. telescopes. None of the observed bow shock candidates shows significant emission in the H.E.S.S. energy range. The resulting upper limits are used to constrain current models for non-thermal emission from these objects.

  6. Bow-shock pulsar-wind nebulae passing through density discontinuities

    NASA Astrophysics Data System (ADS)

    Yoon, Doosoo; Heinz, Sebastian

    2017-01-01

    Bow-shock pulsar-wind nebulae are a subset of pulsar-wind nebulae that form when the pulsar has high velocity due to the natal kick during the supernova explosion. The interaction between the relativistic wind from the fast-moving pulsar and the interstellar medium produces a bow-shock and a trail, which are detectable in Hα emission. Among such bow-shock pulsar-wind nebulae, the Guitar Nebula stands out for its peculiar morphology, which consists of a prominent bow-shock head and a series of bubbles further behind. We present a scenario in which multiple bubbles can be produced when the pulsar encounters a series of density discontinuities in the ISM. We tested the scenario using 2D and 3D hydrodynamic simulations. The shape of the Guitar Nebula can be reproduced if the pulsar traversed a region of declining low density. We also show that if a pulsar encounters an inclined density discontinuity, it produces an asymmetric bow-shock head, consistent with observations of the bow-shock of the millisecond pulsar J2124-3358.

  7. Primary bowing tremor: a task-specific movement disorder of string instrumentalists.

    PubMed

    Lederman, Richard J

    2012-12-01

    Fear of a tremulous or unsteady bow is widespread among string instrumentalists. Faulty technique and performance anxiety have generally been blamed. The cases of 4 high-level violinists and 1 violist, 3 women and 2 men, with uncontrollable bow tremor are presented. Age at onset was from 16 to 75 years, and symptom duration 8 months to 20 years at the time of neurological evaluation. The degree of tremor varied with type of bow stroke and even the portion of the bow contacting the string. Only 1 patient had a slight postural tremor of the opposite limb. In 3 of 5 the tremor was task-specific; the other 2 had mild and nontroubling tremor with other activities. The tremor appeared to worsen over time but then seemed to stabilize. The characteristics of this tremor appear to be distinguishable from the features of both essential tremor and focal dystonia; comparison is made with representative string players afflicted by these other disorders. Analogy of this tremor is made with primary writing tremor, a well-defined task-specific movement disorder also sharing at least some features with both essential tremor and writers' cramp, a focal dystonia. Hence, it was decided to call this primary bowing tremor. Clinical features, family history, diagnostic studies, and responsiveness to treatment of primary writing tremor are discussed to emphasize the similarity to primary bowing tremor. This appears to represent a previously unreported form of task-specific movement disorder of string instrumentalists.

  8. Flow performance of highly loaded axial fan with bowed rotor blades

    NASA Astrophysics Data System (ADS)

    Chen, L.; Liu, X. J.; Yang, A. L.; Dai, R.

    2013-12-01

    In this paper, a partial bowed rotor blade was proposed for a newly designed high loaded axial fan. The blade was positively bowed 30 degrees from hub to 30 percent spanwise position. Flows of radial blade and bowed blade fans were numerically compared for various operation conditions. Results show that the fan's performance is improved. At the designed condition with flow coefficient of 0.52, the efficiency of the bowed blade fan is increased 1.44% and the static pressure rise is increased 11%. Comparing the flow structures, it can be found that the separated flow in the bowed fan is reduced and confined within 20 percent span, which is less than the 35 percent in the radial fan. It means that the bowed blade generates negative blade force and counteracts partial centrifugal force. It is alleviates the radial movements of boundary layers in fan's hub region. Flow losses due to 3D mixing are reduced in the rotor. Inlet flow to downstream stator is also improved.

  9. Asymmetric Outer Bow Length and Cervical Headgear Force System: 3D Analysis Using Finite Element Method.

    PubMed

    Geramy, Allahyar; Hassanpour, Mehdi; Emadian Razavi, Elham Sadat

    2015-03-01

    This study sought to assess distal and lateral forces and moments of asymmetric headgears by variable outer bow lengths. Four 3D finite element method (FEM) models of a cervical headgear attached to the maxillary first molars were designed in SolidWorks 2010 software and transferred to ANSYS Workbench ver. 11 software. Models contained the first molars, their periodontal ligament (PDL), cancellous and cortical bones, a mesiodistal slice of the maxillae and the headgear. Models were the same except for the outer bow length in headgears. The headgear was symmetric in model 1. In models 2 to 4, the headgears were asymmetric in length with differences of 5mm, 10mm and 15mm, respectively. A 2.5 N force in horizontal plane was applied and the loading manner of each side of the outer bow was calculated trigonometrically using data from a volunteer. The 15mm difference in outer bow length caused the greatest difference in lateral (=0.21 N) and distal (= 1.008 N) forces and also generated moments (5.044 N.mm). As the difference in outer bow length became greater, asymmetric effects increased. Greater distal force in the longer arm side was associated with greater lateral force towards the shorter arm side and more net yawing moment. A difference range of 1mm to 15 mm of length in cervical headgear can be considered as a safe length of outer bow shortening in clinical use.

  10. Asymmetric Outer Bow Length and Cervical Headgear Force System: 3D Analysis Using Finite Element Method

    PubMed Central

    Geramy, Allahyar; Hassanpour, Mehdi; Emadian Razavi, Elham sadat

    2015-01-01

    Objectives: This study sought to assess distal and lateral forces and moments of asymmetric headgears by variable outer bow lengths. Materials and Methods: Four 3D finite element method (FEM) models of a cervical headgear attached to the maxillary first molars were designed in SolidWorks 2010 software and transferred to ANSYS Workbench ver. 11 software. Models contained the first molars, their periodontal ligament (PDL), cancellous and cortical bones, a mesiodistal slice of the maxillae and the headgear. Models were the same except for the outer bow length in headgears. The headgear was symmetric in model 1. In models 2 to 4, the headgears were asymmetric in length with differences of 5mm, 10mm and 15mm, respectively. A 2.5 N force in horizontal plane was applied and the loading manner of each side of the outer bow was calculated trigonometrically using data from a volunteer. Results: The 15mm difference in outer bow length caused the greatest difference in lateral (=0.21 N) and distal (= 1.008 N) forces and also generated moments (5.044 N.mm). Conclusion: As the difference in outer bow length became greater, asymmetric effects increased. Greater distal force in the longer arm side was associated with greater lateral force towards the shorter arm side and more net yawing moment. Clinical Relevance: A difference range of 1mm to 15 mm of length in cervical headgear can be considered as a safe length of outer bow shortening in clinical use. PMID:26622275

  11. Effect of bow-type initial imperfection on reliability of minimum-weight, stiffened structural panels

    NASA Technical Reports Server (NTRS)

    Stroud, W. Jefferson; Krishnamurthy, Thiagaraja; Sykes, Nancy P.; Elishakoff, Isaac

    1993-01-01

    Computations were performed to determine the effect of an overall bow-type imperfection on the reliability of structural panels under combined compression and shear loadings. A panel's reliability is the probability that it will perform the intended function - in this case, carry a given load without buckling or exceeding in-plane strain allowables. For a panel loaded in compression, a small initial bow can cause large bending stresses that reduce both the buckling load and the load at which strain allowables are exceeded; hence, the bow reduces the reliability of the panel. In this report, analytical studies on two stiffened panels quantified that effect. The bow is in the shape of a half-sine wave along the length of the panel. The size e of the bow at panel midlength is taken to be the single random variable. Several probability density distributions for e are examined to determine the sensitivity of the reliability to details of the bow statistics. In addition, the effects of quality control are explored with truncated distributions.

  12. X-ray observations of the Ophiuchus, PKS 0745-191 and Cygnus-A clusters of galaxies

    NASA Technical Reports Server (NTRS)

    Arnaud, K. A.; Johnstone, R. M.; Fabian, A. C.; Shafer, R. A.; Mushotzky, R. F.

    1987-01-01

    Observations are reported of the X-ray emission from three bright clusters of galaxies at low Galactic latitudes: the Ophiuchus, PKS 0745-191, and Cygnus-A clusters. Temperatures and iron abundances are determined from Exosat spectral data. Images of the Ophiuchus cluster show it to have a high central density and a cooling flow. Measurements of a high gas density around PKS 0745-191 and are confirmed, and it is shown that the X-ray emission is centered on the radio galaxy. The PKS 0745-191 cluster is the most distant object for which an abundance has been measured from X-ray spectra. The spectrum of Cygnus-A contains a highly absorbed power-law component that is identified with the nucleus of the radio source.

  13. The Periodicity Analysis of Radio Flux Variability of PKS 1510-089 with the Period04 Method

    NASA Astrophysics Data System (ADS)

    Fu, Jun-Ping; Zhang, Hao-Jing; Zhang, Xiong; Xiong, Ding-Rong; Guo, Fei

    2014-10-01

    We have collected the 37 GHz radio data of PKS 1510-089 from 1990 to 2005, and obtained its long-term light curve after making data processing. From the light curve we can find that the activity in PKS 1510-089 is very strong. In this paper, the Period04 method is used for the first time to analyze the light periodicity of PKS 1510-089. The result indicates that its radio emission at 37 GHz has the periods of (1.87±0.13) yr and (0.87±0.07) yr. This result is consistent with the results obtained by Xie et al. in 2004, 2005, 2008, and Wu et al. in 2005 with other methods of data analysis.

  14. Biomechanical research on bowed string musicians: a scoping study.

    PubMed

    Kelleher, Leila K; Campbell, Kody R; Dickey, James P

    2013-12-01

    Performing arts biomechanics is concerned with quantifying the musculoskeletal demands of artistic tasks. The growing body of related research has prompted this scoping study, solely focused on quantitative research, to summarize the state of the science, identify knowledge gaps, and identify opportunities for future research. To identify, summarize, and categorize quantitative research on the biomechanics of violin, viola, cello, and double bass players, using scoping study methodology. Established scoping study methodology was used to identify and categorize existing research. We identified 74 articles for review. Of these, 34 met our scoping study criteria and were included in this study. Twenty-one of the 34 articles that met the scoping criteria were published since 2000. Investigations using electromyography (16 studies) and kinematics (15 studies) comprise the bulk of the research. Two studies employed force transducers for data collection. Violinists were the most frequently studied musicians (22 studies) and double bass players were the least (1 study). Fewer than half of the studies used solely professional musicians as their subjects (13 studies). This scoping study confirmed that quantitative biomechanical research into bowed string musicians has been performed with increasing frequency and that there are voids in the research, particularly in investigating mechanisms of injury and protective strategies. Currently, arts biomechanics research is largely descriptive in nature. There are few studies that investigate protective strategies, although it is expected that the field will progress to incorporate this type of research.

  15. Characterizing the Bow Shock of the Large Magellanic Cloud

    NASA Astrophysics Data System (ADS)

    Setton, David; Besla, Gurtina; Hummels, Cameron

    2017-01-01

    The Circumgalactic Medium (CGM) surrounding our Milky Way plays an essential role in supplying the fuel needed to drive and sustain star formation in our Galaxy. However, the CGM is extremely diffuse (~10^28 g/cm^3), and therefore difficult to probe. Consequently, we know little about the structure, mass profile or evolution of the CGM. Using hydrodynamic simulations, we study the impact of the supersonic motions (Mach ~ 3) of the Large Magellanic Cloud (LMC), the largest satellite galaxy of the Milky Way, on the structure of the CGM. We conclude that the LMC must induce a large bow shock in the CGM and use simulations to characterize its size, shape, temperature, and density structure. Using these properties, we propose possible observational signatures that could be used to confirm the existence of the shock, and illustrate how the shock may provide a tool to probe the CGM. These results illustrate that the CGM is a dynamic system, affected not only by outflows from the host galaxy, but also by the motions of the satellites that orbit within it.

  16. Electromyographic analysis of bow string release in highly skilled archers.

    PubMed

    Martin, P E; Siler, W L; Hoffman, D

    1990-01-01

    A predominant archery coaching tenet holds that the most effective means of releasing the bow string is by relaxation of the finger flexor muscles without activation of finger extensors. To evaluate the validity of this view, EMG patterns of the flexor digitorum superficialis and extensor digitorum muscles of the draw arm were examined using surface EMG electrodes in 15 highly skilled archers as each performed six shots. Each archer displayed consistent EMG patterns from shot-to-shot and two distinct flexor-extensor patterns were exhibited by the sample. The first, characterized by eight of the archers, supported the relaxation principle. For these archers, both flexor and extensor digitorum activity decreased markedly immediately prior to or at arrow release. The second pattern, characteristic of the remaining seven archers, contradicted the coaching tenet. While the flexor digitorum pattern was essentially the same as that described for the first pattern, the extensor digitorum displayed a marked increase in activity just prior to release, indicating that string release was facilitated by an active extension of the fingers. It was concluded that highly skilled archers do not predominantly reflect a release consistent with the coaching canon and that factors other than the string release mechanism discriminate the performances of skilled archers.

  17. Magnetohydrodynamic and gasdynamic theories for planetary bow waves

    NASA Technical Reports Server (NTRS)

    Spreiter, J. R.; Stahara, S. S.

    1984-01-01

    The observed properties of bow waves and the associated plasma flows are outlined, along with those features identified that can be described by a continuum magnetohydrodynamic flow theory as opposed to a more detailed multicomponent particle and field plasma theory. The primary objectives are to provide an account of the fundamental concepts and current status of the magnetohydrodynamic and gas dynamic theories for solar wind flow past planetary bodies. This includes a critical examination of: (1) the fundamental assumptions of the theories; (2) the various simplifying approximations introduced to obtain tractable mathematical problems; (3) the limitations they impose on the results; and (4) the relationship between the results of the simpler gas dynamic-frozen field theory and the more accurate but less completely worked out magnetohydrodynamic theory. Representative results of the various theories are presented and compared. A number of deficiencies, ambiguities, and suggestions for improvements are discussed, and several significant extensions of the theory required to provide comparable results for all planets, their satellites, and comets are noted.

  18. Electron plasma waves upstream of the earth's bow shock

    NASA Technical Reports Server (NTRS)

    Lacombe, C.; Mangeney, A.; Harvey, C. C.; Scudder, J. D.

    1985-01-01

    Electrostatic waves are observed around the plasma frequency fpe in the electron foreshock, together with electrons backstreaming from the bow shock. Using data from the sounder aboard ISEE 1, it is shown that this noise, previously understood as narrow band Langmuir waves more or less widened by Doppler shift or nonlinear effects, is in fact composed of two distinct parts: one is a narrow band noise, emitted just above fpe, and observed at the upstream boundary of the electron foreshock. This component has been interpreted as Langmuir waves emitted by a beam-plasma instability. It is suggested that it is of sufficiently large amplitude and monochromatic enough to trap resonant electrons. The other is a broad band noise, more impulsive than the narrow band noise, observed well above and/or well below fpe, deeper in the electron foreshock. The broad band noise has an average spectrum with a typical bi-exponential shape; its peak frequency is not exactly equal to fpe and depends on the Deybe length. This peak frequency also depends on the velocity for which the electron distribution has maximum skew. An experimental determination of the dispersion relation of the broad band noise shows that this noise, as well as the narrow band noise, may be due to the instability of a hot beam in a plasma.

  19. Evolution of the Bow Shock in the Guitar Nebula

    NASA Astrophysics Data System (ADS)

    Cordes, James

    2001-07-01

    We propose WFPC2 observations of the Guitar Nebula, a bow shock produced by the high-velocity {V>1000 kms} pulsar B2224+65. By comparison with a previous observation in 1994, a new narrow-band H-alpha image will allow exploitation of the change in pulsar location { 1"}, in order to: {a} quantify ambient interstellar density variations on scales <=10^-3 pc that perturb the shape of the bowshock near the contact discontinuity {size 0.2"}; and {b} better model the bowshock to determine the orientation of the pulsar velocity vector. The results will be combined with a prior ROSAT image and a deep X-ray exposure {Chandra, October 2000} and ground based images from Palomar Observatory that constrain the shock heating and large scale structure of the nebula. PSR B2224+65 has the highest estimated space velocity of any pulsar: these results will also improve the pulsar distance and velocity estimates, which are important inputs for the study of pulsar kicks and supernovae asymmetry.

  20. PROTON SYNCHROTRON RADIATION FROM EXTENDED JETS OF PKS 0637–752 AND 3C 273

    SciTech Connect

    Bhattacharyya, Wrijupan; Gupta, Nayantara

    2016-02-01

    Many powerful radio quasars are associated with large-scale jets, exhibiting bright knots as shown by high-resolution images from the Hubble Space Telescope (HST) and the Chandra X-ray Observatory. The radio-optical flux component from these jets can be attributed to synchrotron radiation by accelerated relativistic electrons while the IC/CMB model, by far, has been the most popular explanation for the observed X-ray emission from these jets. Recently, the IC/CMB X-ray mechanism has been strongly disfavored for 3C 273 and PKS 0637–752 since the anomalously hard and steady gamma-ray emission predicted by such models violates the observational results from Fermi-LAT. Here we propose the proton synchrotron origin of the X-ray–gamma-ray flux from the knots of PKS 0637–752 with a reasonable budget in luminosity, by considering synchrotron radiation from an accelerated proton population. Moreover, for the source 3C 273, the optical data points near 10{sup 15} Hz could not be fitted using electron synchrotron. We propose an updated proton synchrotron model, including the optical data from HST, to explain the common origin of optical-X-ray–gamma-ray emission from the knots of quasar 3C 273 as an extension of the work done by Kundu and Gupta. We also show that TeV emission from large-scale quasar jets, in principle, can arise from proton synchrotron, which we discuss in the context of knot wk8.9 of PKS 0637–752.

  1. Colibactin Contributes to the Hypervirulence of pks+ K1 CC23 Klebsiella pneumoniae in Mouse Meningitis Infections

    PubMed Central

    Lu, Min-Chi; Chen, Ying-Tsong; Chiang, Ming-Ko; Wang, Yao-Chen; Hsiao, Pei-Yi; Huang, Yi-Jhen; Lin, Ching-Ting; Cheng, Ching-Chang; Liang, Chih-Lung; Lai, Yi-Chyi

    2017-01-01

    Klebsiella pneumoniae is the most common pathogen of community-acquired meningitis in Taiwan. However, the lack of a physiologically relevant meningitis model for K. pneumoniae has impeded research into its pathogenesis mechanism. Based on the core genome MLST analyses, the hypervirulent K1 K. pneumoniae strains, which are etiologically implicated in adult meningitis, mostly belong to a single clonal complex, CC23. Some K1 CC23 K. pneumoniae strains carry a gene cluster responsible for colibactin production. Colibactin is a small genotoxic molecule biosynthesized by an NRPS-PKS complex, which is encoded by genes located on the pks island. Compared to other hypervirulent K. pneumoniae which primarily infect the liver, the colibactin-producing (pks+) K1 CC23 strains had significant tropism toward the brain of BALB/c mice. We aimed in this study to develop a physiologically relevant meningitis model with the use of pks+ K1 CC23 K. pneumoniae. Acute meningitis was successfully induced in adult BALB/c male mice through orogastric, intranasal, and intravenous inoculation of pks+ K1 CC23 K. pneumoniae. Besides the typical symptoms of bacterial meningitis, severe DNA damages, and caspase 3-independent cell death were elicited by the colibactin-producing K1 CC23 K. pneumoniae strain. The deletion of clbA, which abolished the production of colibactin, substantially hindered K. pneumoniae hypervirulence in the key pathogenic steps toward the development of meningitis. Our findings collectively demonstrated that colibactin was necessary but not sufficient for the meningeal tropism of pks+ K1 CC23 K. pneumoniae, and the mouse model established in this study can be applied to identify other virulence factors participating in the development of this life-threatening disease. PMID:28409125

  2. Fermi LAT detection of renewed gamma-ray activity from the FSRQ PKS 2326-502

    NASA Astrophysics Data System (ADS)

    D'Ammando, F.; Torresi, E.

    2012-06-01

    The Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope has observed an increasing gamma-ray flux from a source positionally consistent with the Flat Spectrum Radio Quasar PKS 2326-502 (also known as 2FGL J2329.2-4956, Nolan et al. 2012, ApJS, 199, 31; R.A.=23:29:20.880 Dec.=-49:55:40.68, J2000.0, Costa and Loyola 1996, A&AS, 115, 75) at redshift z=0.518 (Jauncey et al. 1984, ApJ, 286, 498).

  3. First results from the Faint Object Camera - Observations of PKS 0521 - 36

    NASA Technical Reports Server (NTRS)

    Macchetto, F.; Albrecht, R.; Barbieri, C.; Blades, J. C.; Boksenberg, A.

    1991-01-01

    The Faint Object Camera on the Hubble Space Telescope was used to observe the radio galaxy PKS 0521 - 36 which hosts a prominent radio jet. Images of the jet show spatial structure comparable to VLA data and significantly better than optical ground-based observations. The jet structure is resolved at FOC resolution. In addition to the radio knot, well resolved by the FOC, an extension of the jet toward the nucleus is apparent. The rest of the jet does not show much clumpiness, implying that the synchrotron electrons must be accelerated all along the jet to account for the extent in the optical region.

  4. VSOP Imaging of the Quasar PKS 1402+044 at z = 3.2

    NASA Astrophysics Data System (ADS)

    Yang, J.; Gurvits, L. I.; Frey, S.; Lobanov, A. P.; Hong, X.-Y.

    2009-08-01

    We present results of VSOP observations of the high-redshift (z = 3.2) quasar PKS 1402+044 (J1405+0415) at 1.6 and 5 GHz, and VLA observations at 1.4, 5, 16, and 43 GHz. The source has a pronounced core-jet structure traced by VSOP down to sub-mas angular scales. The results offer a set of observational data enabling physical diagnostics of the inner parsecs of a typical radio-loud quasar.

  5. NIR flaring of the Gamma ray source PKS1550-242

    NASA Astrophysics Data System (ADS)

    Carrasco, L.; Carramiñana, A.; Recillas, E.; Porras, A.; Mayya, D. Y.; Escobedo, G.

    2010-07-01

    We call attention on our recent observation of the Gamma Ray source 1FGLJ1553.4-2425 also known as PKS1550-242 with the CANICA NIR camera on the 2.1m telescope at the Observatorio Astrofísico Guillermo Haro, located in Cananea, Mexico. On June 16th, 2010 (JD24555363.741), we found this blazar to be in outburst. It showed fluxes about 1.6 magnitudes brighter than our previous NIR photometry. On this date the source was found to have a flux corresponding to H = 14.615 ± 0.04.

  6. Another NIR flare of the Gamma ray source PKS1550-242

    NASA Astrophysics Data System (ADS)

    Carrasco, L.; Carraminana, A.; Porras, A.; Recillas, E.; Escobedo, G.

    2011-05-01

    We call attention on our recent observation of the Gamma Ray source 1FGLJ1553.4-2425 also known as PKS1550-242 with the CANICA NIR camera on the 2.1m telescope at the Observatorio Astrofisico Guillermo Haro, located in Cananea, Mexico. On April 26th, 2011 (JD24555677.877), we found this blazar to be in outburst. It showed fluxes about 4.2 magnitudes brighter than our previous NIR photometry. On this date the source was found to have a flux corresponding to H = 14.527 ± 0.05.

  7. Detection of extragalactic CF+ toward PKS 1830-211. Chemical differentiation in the absorbing gas

    NASA Astrophysics Data System (ADS)

    Muller, S.; Kawaguchi, K.; Black, J. H.; Amano, T.

    2016-05-01

    We report the first extragalactic detection of the fluoromethylidynium ion CF+ in the z = 0.89 absorber toward PKS 1830-211. We estimate an abundance of ~3 × 10-10 relative to H2 and that ~1% of fluorine is captured in CF+. The absorption line profile of CF+ is found to be markedly different from that of other species observed within the same tuning, and is notably anticorrelated with CH3OH. On the other hand, the CF+ profile resembles that of [C I]. Our results are consistent with expected fluorine chemistry and point to chemical differentiation in the column of absorbing gas.

  8. Fermi LAT detection of renewed activity from the blazar PKS 1502+106

    NASA Astrophysics Data System (ADS)

    Ciprini, Stefano

    2015-06-01

    The Large Area Telescope (LAT), one of two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux from a source positionally consistent with the flat spectrum radio quasar PKS 1502+106 (also known as OR 103, S3 1502+10 and 3FGL J1504.4+1029, Acero et al., arXiv:1501.02003), with radio coordinates, (J2000.0), R.A.: 226.10408 deg, Dec: 10.49422 deg (Johnston et al. 1995, AJ, 110, 880). This blazar has a redshift of z=1.8383 (Hewett & Wild 2010, MNRAS, 405, 2302).

  9. Anatomy of a blazar in the (sub-)millimeter: ALMA observations of PKS 0521-365

    NASA Astrophysics Data System (ADS)

    Leon, S.; Cortes, P. C.; Guerard, M.; Villard, E.; Hidayat, T.; Ocaña Flaquer, B.; Vila-Vilaro, B.

    2016-02-01

    Aims: We aim at analyzing the (sub-)millimeter emission in a nearby blazar, PKS 0521-365, to study the synchrotron and thermal emission in the different components detected at low frequency. Methods: We analyzed the archive public data of the ALMA Cycle 0 where PKS 0521-365 is used as a calibrator. A total of 13 projects with 23 dataset were analyzed in Bands 3, 6, and 7 and combined. The whole set of data was combined and wavelet-filtered to obtain a deep image toward PKS 0521-365, reaching a dynamic range of 47 000. The individual emission flux was measured on different dates over a period of 11 months in various components. Finally we analyzed the spectral energy distribution (SED) in each different component, including the radio jet and counter jet. Results: The point sources detected in the field follow a similar distribution to previous studies. The blazar flux shows large variation especially in Band 3. Different components are observed: core, radio jet, and newly detected counter jet, hot spot (HS), and a disky structure roughly perpendicular to the jet. The HS emission is formed by a point source surrounded by an extended emission. The viewing angle of the jet is about 30° with a Doppler factor of δ = 1.6. The HS is at a distance of 19 kpc from the center. The SED analysis shows a strong variation in the core spectral index, especially in Band 3. The two components in the radio jet have roughly a flat spectral index in Bands 6 and 7. Conclusions: The different weak and extended components in PKS 0521-365 are detected with the ALMA data. The analysis of both jets constrains the geometrical distance of the HS to the center. The SED presents a different shape in time and frequency for each component. Finally, a new structure is detected roughly perpendicular to the radio jet. and a thermal emission origin is currently favored. Further observations at higher spatial resolution are needed to confirm that hypothesis. FITS files for all the images are only

  10. Optical activity of the flaring gamma-ray blazar PKS 0458-02

    NASA Astrophysics Data System (ADS)

    Pursimo, Tapio; Ojha, Roopesh; Kiaeerad, Fatemeh

    2012-09-01

    We report optical photometry of the high redshift (z=2.286 Strittmatter et al. 1974, ApJ, 190, 509) flat spectrum radio quasar PKS 0458-02 obtained with the 2.56m Nordic Optical Telescope in La Palma. This superluminal FSRQ (apparent speed of 16.51c; Lister et al. 2009, AJ, 138,1874), is also known as 2FGL J0501.2-0155 (Nolan et al. 2012, ApJS, 199, 31) and was reported to be 30 times brighter than its average daily Fermi/LAT (E > 100 MeV) flux on 17 September (Atel#4396).

  11. Fermi LAT detection of renewed GeV flaring activity from PKS 0426-380

    NASA Astrophysics Data System (ADS)

    Ciprini, Stefano

    2012-12-01

    The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed gamma-ray flaring activity from a source positionally consistent with the BL Lac object PKS 0426-380 (also known as 2FGL J0428.6-3756, Nolan et al. 2012, ApJS, 199, 31, and RX J0428.6-3756) with radio coordinates R.A.: 67.16843 deg, Dec: -37.93877 deg, J2000 (Johnston et al. 1995, AJ, 110, 880) and redshift z=1.111 (Heidt et al....

  12. Detection of a strong optical and gamma-ray flare from blazar PKS 1424-41

    NASA Astrophysics Data System (ADS)

    D'Ammando, F.; Orienti, M.; Longo, F.; Jankowsky, F.; Schwemmer, S.; Wagn, S.

    2013-01-01

    The Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope has observed an increasing gamma-ray flux from a source positionally coincident with PKS 1424-41 (also known as 2FGL J1428.0-4206, Nolan et al. 2012, ApJS, 199, 31; R.A.= 14h27m56.2975s, Dec.= -42d06m19.437s, J2000, Johnston et al. 1995, AJ, 110, 880), a flat spectrum radio quasar with a redshift of 1.522 (White et al. 1988, ApJ, 327, 561).

  13. Modeling X-Ray Emission of a Straight Jet: PKS 0920-397

    DTIC Science & Technology

    2010-01-01

    and with the jet at an angle 2◦to 4◦from our line of sight. Keywords: Quasar jets; X–ray jets; jet emission mechanisms. In t. J. M od . P hy s. D...detection of the jet in the quasar PKS 0637–7513 during the very first pointed observation. While X–ray jet emission from FR I radio galaxies is normally...explained via the synchrotron mechanism, the quasar jets initially presented a puz- zle. Observations, or upper limits, to optical emission from quasar

  14. Optical, X, Gamma-ray activity of the FSRQ PKS 1313-333

    NASA Astrophysics Data System (ADS)

    Pacciani, Luigi

    2015-12-01

    We asked a Swift ToO campaign on the FSRQ PKS 1313-333 (z=1.21), triggered by prolonged High Energy activity detected with FERMI-LAT. The trigger method detected activity at E > 20GeV/(1+z) with TS ~79 from 2015-12-10 to 2015-12-30, following the prescription of Pacciani et al. 2014, ApJ, 790, 45. FERMI-LAT detected Two Gamma-ray photons of about 50 GeV within the last week.

  15. Radio re-brightening of the gamma-ray flaring blazar PKS 1510-089

    NASA Astrophysics Data System (ADS)

    Fuhrmann, L.; Angelakis, E.; Nestoras, I.; Schmidt, R.; Krichbaum, T. P.; Zensus, J. A.; Ungerechts, H.; Sievers, A.; Riquelme, D.

    2011-07-01

    Responding to the ATels #3473 and #3470 reporting the recent flaring activity of PKS 1510-089 at gamma-rays beginning of July 2011 as well as ATel #3479 reporting no optical counterpart of this activity, we here report its behavior at radio bands as observed by the F-GAMMA program. Long-term activity: Observations performed with the Effelsberg 100-m and the IRAM 30-m telescope since its pronounced flaring activity of 2009 show that the source is basically following a continuously decaying long-term trend at low to intermediate frequencies, though with smaller "sub-flares" superimposed.

  16. PKS 2123-463: A Confirmed Gamma-ray Blazar at High Redshift

    NASA Technical Reports Server (NTRS)

    D'Ammando, F.; Rau, A.; Schady, P.; Finke, J.; Orienti, M.; Greiner, J.; Kann, D. A.; Ojha, R.; Foley, A. R.; Stevens, J.; Blanchard, J. M.; Edwards, P. G.; Kadler, M.; Lovell, J. E.

    2013-01-01

    The flat spectrum radio quasar (FSRQ) PKS 2123-463 was associated in the first Fermi- Large Area Telescope (LAT) source catalogue with the gamma-ray source 1FGL J2126.1-4603, but when considering the full first two years of Fermi observations, no gamma-ray source at a position consistent with this FSRQ was detected, and thus PKS 2123-463 was not reported in the second Fermi-LAT source catalogue. On 2011 December 14 a gamma-ray source positionally consistent with PKS 2123-463 was detected in flaring activity by Fermi-LAT. This activity triggered radio-to-X-ray observations by the Swift,Gamma-ray Optical/Near-Infrared Detector (GROND), Australia Telescope Compact Array (ATCA), Ceduna and Seven Dishes Karoo Array Telescope (KAT-7) observatories. Results of the localization of the gamma-ray source over 41 months of Fermi-LAT operation are reported here in conjunction with the results of the analysis of radio, optical, ultraviolet (UV) and X-ray data collected soon after the gamma-ray flare. The strict spatial association with the lower energy counterpart together with a simultaneous increase of the activity in optical, UV, X-ray and gamma-ray bands led to a firm identification of the gamma-ray source with PKS 2123-463. A new photometric redshift has been estimated as z = 1.46 plus or minus 0.05 using GROND and Swift Ultraviolet/Optical Telescope (UVOT) observations, in rough agreement with the disputed spectroscopic redshift of z = 1.67.We fit the broad-band spectral energy distribution with a synchrotron/external Compton model. We find that a thermal disc component is necessary to explain the optical/UV emission detected by Swift/UVOT. This disc has a luminosity of approximately 1.8 x 10(exp 46) erg s(exp -1), and a fit to the disc emission assuming a Schwarzschild (i.e. non-rotating) black hole gives a mass of approximately 2 x 10(exp 9) solar mass. This is the first black hole mass estimate for this source.

  17. Fermi LAT detection of GeV flares from blazars PKS 0458-02 and B2 1144+40

    NASA Astrophysics Data System (ADS)

    Antolini, Elisa; Buson, Sara

    2014-03-01

    The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux from two sources positionally consistent with the flat spectrum radio quasars PKS 0458-02 (also known as 2FGL J0501.2-0155, Nolan et al. 2012 ApJS, 199, 31) and B2 1144+40 (also known as S4 1144+40 and 2FGL J1146.9+4000). PKS 0458-02 has the radio coordinates RA=05h01m12.8098s, Dec=-1d59m14.255s (J2000, Johnston et al.

  18. Comparison of accelerated ion populations observed upstream of the bow shocks at Venus and Mars

    NASA Astrophysics Data System (ADS)

    Yamauchi, M.; Futaana, Y.; Fedorov, A.; Frahm, R. A.; Winningham, J. D.; Dubinin, E.; Lundin, R.; Barabash, S.; Holmström, M.; Mazelle, C.; Sauvaud, J.-A.; Zhang, T. L.; Baumjohann, W.; Coates, A. J.; Fraenz, M.

    2011-03-01

    Foreshock ions are compared between Venus and Mars at energies of 0.6~20 keV using the same ion instrument, the Ion Mass Analyser, on board both Venus Express and Mars Express. Venus Express often observes accelerated protons (2~6 times the solar wind energy) that travel away from the Venus bow shock when the spacecraft location is magnetically connected to the bow shock. The observed ions have a large field-aligned velocity compared to the perpendicular velocity in the solar wind frame, and are similar to the field-aligned beams and intermediate gyrating component of the foreshock ions in the terrestrial upstream region. Mars Express does not observe similar foreshock ions as does Venus Express, indicating that the Martian foreshock does not possess the intermediate gyrating component in the upstream region on the dayside of the planet. Instead, two types of gyrating protons in the solar wind frame are observed very close to the Martian quasi-perpendicular bow shock within a proton gyroradius distance. The first type is observed only within the region which is about 400 km from the bow shock and flows tailward nearly along the bow shock with a similar velocity as the solar wind. The second type is observed up to about 700 km from the bow shock and has a bundled structure in the energy domain. A traversal on 12 July 2005, in which the energy-bunching came from bundling in the magnetic field direction, is further examined. The observed velocities of the latter population are consistent with multiple specular reflections of the solar wind at the bow shock, and the ions after the second reflection have a field-aligned velocity larger than that of the de Hoffman-Teller velocity frame, i.e., their guiding center has moved toward interplanetary space out from the bow shock. To account for the observed peculiarity of the Martian upstream region, finite gyroradius effects of the solar wind protons compared to the radius of the bow shock curvature and effects of cold ion

  19. The upper Bow Island (Blackleaf) Formation of southwestern Alberta: Geological aspects and exploration approaches

    SciTech Connect

    Putnam, P.E.; Christensen, S.L. )

    1991-06-01

    The upper parts of the Bow Island Formation (Albian) of southwestern Alberta are significant gas reservoirs. The main westernmost reservoir zone is part of a complex package of interbedded lenticular sandstones, mudstones, and localized chert pebble conglomerates. The depositional setting for these sediments comprised a wave-dominated shoreline with conglomerates found proximal to drowned river mouths. The coarse nature of the upper Bow Island is related to tectonic movements associated with Crowsnest (Vaughn) volcanism. Conglomerates form the most impressive Bow Island reservoirs because of their thickness (up to 25 m) and petrophysical properties (17% porosity, 24 d permeability). Diagenesis dominantly comprises compaction features within grain-supported conglomerates. Increasing quartz content is related to decreasing grain size and is associated with porosity occlusion by quartz overgrowths. Bow Island reservoirs in southwestern Alberta are cool (under 50C) and significantly underpressured (0.2 psi). The high permeabilities and low pressures at depths of 1,000 to 1,500 m suggest the potential for formation damage is high, and many wells in the region were targeted for deeper, high-pressure zones. In spite of the low pressures, however, many Bow Island wells are capable of excellent gas deliveries with individual well recoveries of up to 10 bcf. All significant Bow Island porosity in the deepest, undisturbed parts of southwestern Alberta is gas saturated with updip aquifers flanking the gas. Seismic definition of the thickest Bow Island targets is feasible but has been hampered, in part, by difficult surface conditions and a prior emphasis on deeper targets.

  20. A bow-shaped thermal structure traveling upstream of the zonal wind flow of Venus atmosphere

    NASA Astrophysics Data System (ADS)

    Taguchi, Makoto; Fukuhara, Tetsuya; Imamura, Takeshi; Kouyama, Toru; Nakamura, Masato; Sato, Takao M.; Ueno, Munetaka; Suzuki, Makoto; Iwagami, Naomoto; Sato, Mitsuteru; Hashimoto, George L.; Takagi, Seiko; Akatsuki Science Team

    2016-10-01

    The Longwave Infrared Camera (LIR) onboard the Japanese Venus orbiter Akatsuki acquires a snap shot of Venus in the middle infrared region, and provides a brightness temperature distribution at the cloud-top altitudes of about 65 km. Hundreds of images taken by LIR have been transferred to the ground since the successful Venus orbit insertion of Akatsuki on Dec. 7, 2015. Here we report that a bow shaped thermal structure extending from the northern high latitudes to the southern high latitudes was found in the brightness temperature map on Dec. 7, 2015, and that it lasted for four days at least surprisingly at almost same geographical position. The bow shape structure looks symmetrical with the equator, and consists of a high temperature region in east or upstream of the background strong westward wind or the super rotation of the Venus atmosphere followed by a low temperature region in west with an amplitude of 5 K. It appeared close to the evening terminator in the dayside, and seems not to have stayed in the same local time rather to have co-rotated with the slowly rotating ground where the western part of Aphrodite Continent was below the center of the bow shape. Meridionally aligned dark filaments similar to the bow shape structure in shape but in much smaller scale were also identified in the brightness temperature map on Dec. 7, and they propagated upstream of the zonal wind as well. The bow shape structure disappeared when LIR observed the same local time and longitude in the earliest opportunity on Jan. 16, 2016. Similar events, though their amplitudes were less than 1 K, were found on Apr. 15 and 26, 2016, but they appeared in different local times and longitudes. A simulation of a gravity wave generated in the lower atmosphere and propagating upward reproduces the observed bow shape structure. The bow shape structure could be a signature of transferring momentum from the ground to the upper atmosphere.

  1. Annual variations in the Martian bow shock location as observed by the Mars Express mission

    NASA Astrophysics Data System (ADS)

    Hall, B. E. S.; Lester, M.; Sánchez-Cano, B.; Nichols, J. D.; Andrews, D. J.; Edberg, N. J. T.; Opgenoorth, H. J.; Fränz, M.; Holmström, M.; Ramstad, R.; Witasse, O.; Cartacci, M.; Cicchetti, A.; Noschese, R.; Orosei, R.

    2016-11-01

    The Martian bow shock distance has previously been shown to be anticorrelated with solar wind dynamic pressure but correlated with solar extreme ultraviolet (EUV) irradiance. Since both of these solar parameters reduce with the square of the distance from the Sun, and Mars' orbit about the Sun increases by ˜0.3 AU from perihelion to aphelion, it is not clear how the bow shock location will respond to variations in these solar parameters, if at all, throughout its orbit. In order to characterize such a response, we use more than 5 Martian years of Mars Express Analyser of Space Plasma and EneRgetic Atoms (ASPERA-3) Electron Spectrometer measurements to automatically identify 11,861 bow shock crossings. We have discovered that the bow shock distance as a function of solar longitude has a minimum of 2.39RM around aphelion and proceeds to a maximum of 2.65RM around perihelion, presenting an overall variation of ˜11% throughout the Martian orbit. We have verified previous findings that the bow shock in southern hemisphere is on average located farther away from Mars than in the northern hemisphere. However, this hemispherical asymmetry is small (total distance variation of ˜2.4%), and the same annual variations occur irrespective of the hemisphere. We have identified that the bow shock location is more sensitive to variations in the solar EUV irradiance than to solar wind dynamic pressure variations. We have proposed possible interaction mechanisms between the solar EUV flux and Martian plasma environment that could explain this annual variation in bow shock location.

  2. The existence and nature of the interstellar bow shock

    SciTech Connect

    Ben-Jaffel, Lotfi; Strumik, M.; Ratkiewicz, R.; Grygorczuk, J.

    2013-12-20

    We report a new diagnosis of two different states of the local interstellar medium (LISM) near our solar system by using a sensitivity study constrained by several distinct and complementary observations of the LISM, solar wind, and inner heliosphere. Assuming the Interstellar Boundary Explorer (IBEX) He flow parameters for the LISM, we obtain a strength of ∼2.7 ± 0.2 μG and a direction pointing away from galactic coordinates (28, 52) ± 3° for the interstellar magnetic field as a result of fitting Voyager 1 and Voyager 2 in situ plasma measurements and IBEX energetic neutral atoms ribbon. When using Ulysses parameters for the LISM He flow, we recently reported the same direction but with a strength of 2.2 ± 0.1 μG. First, we notice that with Ulysses He flow, our solution is in the expected hydrogen deflection plane (HDP). In contrast, for the IBEX He flow, the solution is ∼20° away from the corresponding HDP plane. Second, the long-term monitoring of the interplanetary H I flow speed shows a value of ∼26 km s{sup –1} measured upwind from the Doppler shift in the strong Lyα sky background emission line. All elements of the diagnosis seem therefore to support Ulysses He flow parameters for the interstellar state. In that frame, we argue that reliable discrimination between superfast, subfast, or superslow states of the interstellar flow should be based on most existing in situ and remote observations used together with global modeling of the heliosphere. For commonly accepted LISM ionization rates, we show that a fast interstellar bow shock should be standing off upstream of the heliopause.

  3. Simultaneous Swift and Rapid Eye Mount telescope observations of the blazar PKS 0537-441

    NASA Astrophysics Data System (ADS)

    Li, Xiao-Pan; Luo, Yu-Hui; Zhang, Li; Yang, Cheng; Yang, Hai-Tao; Cai, Yan

    2017-02-01

    We present the results of simultaneous multiwavelength observations of the blazar PKS 0537-441 performed with the Rapid Eye Mount telescope (REM) and Swift in the period 2009-2011. During our campaign, PKS 0537-441 showed prominent activity with well-correlated light curves from near-infrared to X-rays in different time epochs. The multiwavelength light curves exhibit several significant flares, in which the 2009 November flare particularly presents a double-peak feature, while the 2010 February flare shows strong optical variability (up to a factor of ˜5). The REM data show smaller fractional variability amplitudes than the Swift data. There is a general correlation between optical and X-rays, time-lags have been determined with data correlation methods and their uncertainties with Monte Carlo runs, but they are either very uncertain or too long (of the order of 300 d) to be physically relevant. The X-ray spectra exhibit neither absorption nor emission features characteristically. A slight harder-when-brighter trend in the 2-10 keV energy band is detected. The optical/ultraviolet spectra suggest the presence of thermal emission. We find evidence that the broad-band spectrum is steeper when the degree of variability is larger.

  4. Gamma-Rays from the Quasar PKS 1441+25: Story of an Escape

    NASA Astrophysics Data System (ADS)

    Abeysekara, A. U.; Archambault, S.; Archer, A.; Aune, T.; Barnacka, A.; Benbow, W.; Bird, R.; Biteau, J.; Buckley, J. H.; Bugaev, V.; Cardenzana, J. V.; Cerruti, M.; Chen, X.; Christiansen, J. L.; Ciupik, L.; Connolly, M. P.; Coppi, P.; Cui, W.; Dickinson, H. J.; Dumm, J.; Eisch, J. D.; Errando, M.; Falcone, A.; Feng, Q.; Finley, J. P.; Fleischhack, H.; Flinders, A.; Fortin, P.; Fortson, L.; Furniss, A.; Gillanders, G. H.; Griffin, S.; Grube, J.; Gyuk, G.; Hütten, M.; Håkansson, N.; Hanna, D.; Holder, J.; Humensky, T. B.; Johnson, C. A.; Kaaret, P.; Kar, P.; Kelley-Hoskins, N.; Khassen, Y.; Kieda, D.; Krause, M.; Krennrich, F.; Kumar, S.; Lang, M. J.; Maier, G.; McArthur, S.; McCann, A.; Meagher, K.; Moriarty, P.; Mukherjee, R.; Nieto, D.; O'Faoláin de Bhróithe, A.; Ong, R. A.; Otte, A. N.; Park, N.; Perkins, J. S.; Petrashyk, A.; Pohl, M.; Popkow, A.; Pueschel, E.; Quinn, J.; Ragan, K.; Ratliff, G.; Reynolds, P. T.; Richards, G. T.; Roache, E.; Rousselle, J.; Santander, M.; Sembroski, G. H.; Shahinyan, K.; Smith, A. W.; Staszak, D.; Telezhinsky, I.; Todd, N. W.; Tucci, J. V.; Tyler, J.; Vassiliev, V. V.; Vincent, S.; Wakely, S. P.; Weiner, O. M.; Weinstein, A.; Wilhelm, A.; Williams, D. A.; Zitzer, B.; VERITAS; Smith, P. S.; SPOL; Holoien, T. W.-S.; Prieto, J. L.; Kochanek, C. S.; Stanek, K. Z.; Shappee, B.; ASAS-SN; Hovatta, T.; Max-Moerbeck, W.; Pearson, T. J.; Reeves, R. A.; Richards, J. L.; Readhead, A. C. S.; OVRO; Madejski, G. M.; NuSTAR; Djorgovski, S. G.; Drake, A. J.; Graham, M. J.; Mahabal, A.; CRTS

    2015-12-01

    Outbursts from gamma-ray quasars provide insights on the relativistic jets of active galactic nuclei and constraints on the diffuse radiation fields that fill the universe. The detection of significant emission above 100 GeV from a distant quasar would show that some of the radiated gamma-rays escape pair-production interactions with low-energy photons, be it the extragalactic background light (EBL), or the radiation near the supermassive black hole lying at the jet’s base. VERITAS detected gamma-ray emission up to ˜200 GeV from PKS 1441+25 (z = 0.939) during 2015 April, a period of high activity across all wavelengths. This observation of PKS 1441+25 suggests that the emission region is located thousands of Schwarzschild radii away from the black hole. The gamma-ray detection also sets a stringent upper limit on the near-ultraviolet to near-infrared EBL intensity, suggesting that galaxy surveys have resolved most, if not all, of the sources of the EBL at these wavelengths.

  5. Methanol absorption in PKS B1830-211 at milliarcsecond scales

    NASA Astrophysics Data System (ADS)

    Marshall, M. A.; Ellingsen, S. P.; Lovell, J. E. J.; Dickey, J. M.; Voronkov, M. A.; Breen, S. L.

    2017-04-01

    Observations of the frequencies of different rotational transitions of the methanol molecule have provided the most sensitive probe to date for changes in the proton-to-electron mass ratio, μ, over space and time. Using methanol absorption detected in the gravitational lens system PKS B1830-211, changes in μ over the last 7.5 billion years have been constrained to |Δμ/μ| ≲ 1.1 × 10-7. Molecular absorption systems at cosmological distances present the best opportunity for constraining or measuring changes in the fundamental constants of physics over time; however, we are now at the stage where potential differences in the morphology of the absorbing systems and the background source, combined with their temporal evolution, provide the major source of uncertainty in some systems. Here, we present the first milliarcsecond resolution observations of the molecular absorption system towards PKS B1830-211. We have imaged the absorption from the 12.2-GHz transition of methanol (which is redshifted to 6.45 GHz) towards the southwestern component and show that it is possibly offset from the peak of the continuum emission and partially resolved on milliarcsecond scales. Future observations of other methanol transitions with similar angular resolution offer the best prospects for reducing systematic errors in investigations of possible changes in the proton-to-electron mass ratio on cosmological scales.

  6. BL LAC OBJECT PKS B1144-379: AN EXTREME SCINTILLATOR

    SciTech Connect

    Turner, R. J.; Ellingsen, S. P.; Shabala, S. S.; Blanchard, J.; Lovell, J. E. J.; McCallum, J. N.; Cimo, G.

    2012-08-01

    Rapid variability in the radio flux density of the BL Lac object PKS B1144-379 has been observed at four frequencies, ranging from 1.5 to 15 GHz, with the Very Large Array and the University of Tasmania's Ceduna antenna. Intrinsic and line-of-sight effects were examined as possible causes of this variability, with interstellar scintillation best explaining the frequency dependence of the variability timescales and modulation indices. This scintillation is consistent with a compact source 20-40 {mu}as or 0.15-0.3 pc in size. The inferred brightness temperature for PKS B1144-379 (assuming that the observed variations are due to scintillation) is 6.2 Multiplication-Sign 10{sup 12} K at 4.9 GHz, with approximately 10% of the total flux in the scintillating component. We show that scintillation surveys aimed at identifying variability timescales of days to weeks are an effective way to identify the active galactic nuclei with the highest brightness temperatures.

  7. THE REMARKABLE {gamma}-RAY ACTIVITY IN THE GRAVITATIONALLY LENSED BLAZAR PKS 1830-211

    SciTech Connect

    Donnarumma, I.; De Rosa, A.; Vittorini, V.; Tavani, M.; Striani, E.; Pacciani, L.; Popovic, L. C.; Simic, S.; Kuulkers, E.; Vercellone, S.; Verrecchia, F.; Pittori, C.; Giommi, P.; Barbiellini, G.; Bulgarelli, A.

    2011-08-01

    We report the extraordinary {gamma}-ray activity (E > 100 MeV) of the gravitationally lensed blazar PKS 1830-211 (z = 2.507) detected by AGILE between 2010 October and November. On October 14, the source experienced a factor of {approx}12 flux increase with respect to its average value and remained brightest at this flux level ({approx}500 x 10{sup -8} photons cm{sup -2} s{sup -1}) for about four days. The one-month {gamma}-ray light curve across the flare showed a mean flux F(E > 100 MeV) = 200 x 10{sup -8} photons cm{sup -2} s{sup -1}, which resulted in a factor of four enhancement with respect to the average value. Following the {gamma}-ray flare, the source was observed in near-IR (NIR)-optical energy bands at the Cerro Tololo Inter-American Observatory and in X-Rays by Swift/X-Ray Telescope and INTEGRAL/IBIS. The main result of these multifrequency observations is that the large variability observed in {gamma}-rays does not have a significant counterpart at lower frequencies: no variation greater than a factor of {approx}1.5 appeared in the NIR and X-Ray energy bands. PKS 1830-211 is then a good '{gamma}-ray only flaring' blazar showing substantial variability only above 10-100 MeV. We discuss the theoretical implications of our findings.

  8. Investigating the Function of Play Bows in Dog and Wolf Puppies (Canis lupus familiaris, Canis lupus occidentalis)

    PubMed Central

    Espinosa, Julia; Marshall-Pescini, Sarah; Smuts, Barbara; Range, Friederike

    2016-01-01

    Animals utilize behavioral signals across a range of different contexts in order to communicate with others and produce probable behavioral outcomes. During play animals frequently adopt action patterns used in other contexts. Researchers have therefore hypothesized that play signals have evolved to clarify communicative intent. One highly stereotyped play signal is the canid play bow, but its function remains contested. In order to clarify how canid puppies use play bows, we used data on play bows in immature wolves (ages 2.7–7.8 months) and dogs (ages 2 to 5 months) to test hypotheses evaluated in a previous study of adult dogs. We found that young dogs used play bows similarly to adult dogs; play bows most often occurred after a brief pause in play followed by complementary highly active play states. However, while the relative number of play bows and total observation time was similar between dog and wolf puppies, wolves did not follow this behavioral pattern, as play bows were unsuccessful in eliciting further play activity by the partner. While some similarities for the function of play bows in dog and wolf puppies were documented, it appears that play bows may function differently in wolf puppies in regards to re-initiating play. PMID:28033358

  9. Bow shock nebulae of hot massive stars in a magnetized medium

    NASA Astrophysics Data System (ADS)

    Meyer, D. M.-A.; Mignone, A.; Kuiper, R.; Raga, A. C.; Kley, W.

    2017-01-01

    A significant fraction of OB-type, main-sequence massive stars are classified as runaway and move supersonically through the interstellar medium (ISM). Their strong stellar winds interact with their surroundings, where the typical strength of the local ISM magnetic field is about 3.5-7 μG, which can result in the formation of bow shock nebulae. We investigate the effects of such magnetic fields, aligned with the motion of the flow, on the formation and emission properties of these circumstellar structures. Our axisymmetric, magneto-hydrodynamical simulations with optically thin radiative cooling, heating and anisotropic thermal conduction show that the presence of the background ISM magnetic field affects the projected optical emission of our bow shocks at Hα and [O III] λ 5007 which become fainter by about 1-2 orders of magnitude, respectively. Radiative transfer calculations against dust opacity indicate that the magnetic field slightly diminishes their projected infrared emission and that our bow shocks emit brightly at 60 μm. This may explain why the bow shocks generated by ionizing runaway massive stars are often difficult to identify. Finally, we discuss our results in the context of the bow shock of ζ Ophiuchi and we support the interpretation of its imperfect morphology as an evidence of the presence of an ISM magnetic field not aligned with the motion of its driving star.

  10. Investigation into the behavior of symmetrically and asymmetrically activated face-bows.

    PubMed

    Nobel, P M; Waters, N E

    1992-04-01

    The distal and lateral forces and also the couples (in a transverse plane) delivered by the inner terminals of a face-bow have been derived analytically according to the complementary (strain) energy method for various face-bow configurations on the assumption that the terminals are rigidly held by the molar tubes and that the external forces acting are in the plane of the inner bow. The results of the theory have been checked experimentally with a specially designed apparatus in which two mild steel transducer pegs that carry three pairs of strain gauges were used to measure the force system delivered by the inner bow under a range of loading, both symmetrical and asymmetrical. Good agreement with the theory was obtained, confirming the validity of the theoretical analysis. It is concluded that force systems are dependent on bow geometry and that with increasing asymmetry of the external loading transference of the distal load to the power-arm side is accompanied by a shift of lateral force and couple to the opposite side.

  11. In situ bow change of Al-alloy MEMS micromirrors during 248-nm laser irradiation

    NASA Astrophysics Data System (ADS)

    Mai, Alexander; Bunce, Christopher; Hübner, Rene; Pahner, Daniel; Dauderstädt, Ulrike

    2016-07-01

    Micromirror based spatial light modulators (SLMs) developed by the Fraunhofer Institute for Photonic Microsystems are well established in microlithography applications. Serving, e.g., as reflective, programmable photomasks in deep-UV mask writers, they enable highly flexible pattern generation. During operation, the micromirror bow significantly impacts contrast and the resolvable feature size of generated patterns. In some situations, MEMS micromirrors tend to change their bow during laser irradiation. A test regime including a characterization unit for the in situ analysis of MEMS micromirror topology has been developed to measure the bow change under various irradiation conditions. Experiments in which SLMs were irradiated by a 1-kHz, 248-nm pulse laser revealed that mirror bowing can occur in both directions (concave and convex). The bowing direction is dependent upon the applied irradiation parameters such as pulse-energy density, pulse number, and the deposited energy. Sustained irradiation at energy densities exceeding a certain limit can potentially become a limiting factor for the resolvable feature sizes of the patterns generated and, therefore, for the usable SLM lifespan.

  12. The Milky Way Project: A Citizen Science Catalog of Infrared Bow Shock Nebulae

    NASA Astrophysics Data System (ADS)

    Dixon, Don; Jayasinghe, Tharindu; Povich, Matthew S.

    2017-01-01

    We present preliminary results from the first citizen-science search for infrared stellar-wind bow shock candidates. This search uses the Milky Way project, hosted by the Zooniverse, an online platform with over 1 million volunteer citizen scientists. Milky Way Project volunteers examine 77,000 randomly-distributed Spitzer image cutouts at varying zoom levels. Volunteers mark the infrared arc of potential bow shock candidates as well as the star likely driving the nebula. We produce lists of candidates from bow shocks flagged by multiple volunteers, which after merging and final visual review form the basis for our catalog. Comparing our new catalog to a recently-published catalog of 709 infrared bow shock candidates identified by a small team of (primarily undergraduate) researchers will allow us to assess the effectiveness of citizen science for this type of search and should yield a more complete catalog. Planned studies using these large catalogs will improve constraints on the mass-loss rates for the massive stars that create these bow shock nebulae. Mass-loss rates are highly uncertain but are a critical component of evolutionary models for massive stars. This work is supported by the National Science Foundation under grants CAREER-1454334, AST-1411851 (RUI) and AST-1412845.

  13. The dynamics of Bow-shock Pulsar Wind Nebula: Reconstruction of multi-bubbles

    NASA Astrophysics Data System (ADS)

    Yoon, Doosoo; Heinz, Sebastian

    2014-08-01

    Bow-shock pulsar wind nebulae (PWNe) exhibit a characteristic cometary shape due to the supersonic motion of the pulsar interacting with the interstellar medium (ISM). One of the spectacular bow-shock is the Guitar Nebula, which is produced by the fast pulsar PSR B2224+65 (vpsr > 1000 km s-1 ), and consists of a bright head, a faint neck, a two larger bubbles. We present that the peculiar mophology arises from variations in the interstellar medium density. We perform 3-D hydrodynamic simulation to understand the evolution of the pulsar as its moves through the density discontinuity. We found that when the pulsar encounters the low-density medium, the pressure balance at the head of the bow shock begins to collapse, producing the second bubble. The expansion rate of the bubble is related to the properties of both the pulsar and the ambient medium. Assuming that the pulsar’s properties, including spin-down energy, are constant, we conclude that the ambient density around the second bubble should be 4.46 times larger than around the first bubble in the Guitar body. We further found that when the pulsar encounters the inclined density dicontinuity, it can produce the asymmetric shape of the bow shock observed in a subset of bow-shock PWNe including J2124-3358.

  14. Bow-tie antennas on a dielectric half-space - Theory and experiment

    NASA Technical Reports Server (NTRS)

    Compton, Richard C.; Mcphedran, Ross C.; Popovic, Zorana; Rebeiz, Gabriel M.; Tong, Peter P.

    1987-01-01

    A new formulation is discussed for the rigous calculation of the radiation pattern of a bow-tie antenna of finite length and infinitesimal thickness, placed on a lossless dielectric substrate. The analysis is based on a representation of the current density on the metal surface of the antenna as a sum of an imposed (quasistatic) term and a set of current modes with unknown amplitudes. Free-space fields that are expressed in terms of continuous spectra of symmetrized plane waves are matched to the current modes using the method of moments. The resulting set of equations are solved for the unknown current amplitudes. The calculations show that for increasing bow length the antenna impedance spirals rapidly to a value predicted by transmission line theory. The theory also shows that the E-plane pattern of a two-wavelength, 60-deg bow-tie antenna is dominated by low-loss current modes propagating at the dielectric wavenumber. As the bow tie narrows, the loss of the modes increases, and the dominant wavenumber tends to the quasi-static value. Pattern measurements made at 94 GHz are shown to agree well with theoretical predictions. Measurements for a long-wire antenna, a linear array of bow-tie elements, and a log-periodic antenna are also presented.

  15. BOW SHOCK FRAGMENTATION DRIVEN BY A THERMAL INSTABILITY IN LABORATORY ASTROPHYSICS EXPERIMENTS

    SciTech Connect

    Suzuki-Vidal, F.; Lebedev, S. V.; Pickworth, L. A.; Swadling, G. F.; Skidmore, J.; Hall, G. N.; Bennett, M.; Bland, S. N.; Burdiak, G.; De Grouchy, P.; Music, J.; Suttle, L.; Ciardi, A.; Rodriguez, R.; Gil, J. M.; Espinosa, G.; Hartigan, P.; Hansen, E.; Frank, A.

    2015-12-20

    The role of radiative cooling during the evolution of a bow shock was studied in laboratory-astrophysics experiments that are scalable to bow shocks present in jets from young stellar objects. The laboratory bow shock is formed during the collision of two counterstreaming, supersonic plasma jets produced by an opposing pair of radial foil Z-pinches driven by the current pulse from the MAGPIE pulsed-power generator. The jets have different flow velocities in the laboratory frame, and the experiments are driven over many times the characteristic cooling timescale. The initially smooth bow shock rapidly develops small-scale nonuniformities over temporal and spatial scales that are consistent with a thermal instability triggered by strong radiative cooling in the shock. The growth of these perturbations eventually results in a global fragmentation of the bow shock front. The formation of a thermal instability is supported by analysis of the plasma cooling function calculated for the experimental conditions with the radiative packages ABAKO/RAPCAL.

  16. Unilateral Outer Bow Expanded Cervical Headgear Force System: 3D Analysis Using Finite Element Method.

    PubMed

    Geramy, Allahyar; Mortezai, Omid; Esmaily, Masomeh; Darvishpour, Hojat

    2015-04-01

    Headgears are among the effective orthodontic appliances to achieve treatment goals. Unilateral molar distal movement is sometimes needed during an orthodontic treatment, which can be achieved by an asymmetric headgear. Different unilateral headgears have been introduced. The main goal of this study was to analyze the force system of unilateral expanded outer bow asymmetric headgears by the finite element method (FEM). Six 3D finite element models of a mesiodistal slice of the maxilla containing upper first molars, their periodontal ligaments (PDLs), cancellous bone, cortical bone, and a cervical headgear with expanded outer bow attached to maxillary first molars were designed in SolidWorks 2010 and meshed in ANSYS Workbench ver. 12.1. The models were the same except for the degree of outer bow expansion. The outer bow ends were loaded with 2 N force. The distal driving force and the net moment were evaluated. A decrease in the distalizing force in the normal side molar from 1.69 N to 1.37 N was shown by increasing the degree of unilateral expansion. At the same time, the force increased from 2.19 N to 2.49 N in the expanded side molar. A net moment increasing from 2.26 N.mm to 4.64 N.mm was also shown. Unilateral outer bow expansion can produce different distalizing forces in molars, which increase by increasing the expansion.

  17. Unilateral Outer Bow Expanded Cervical Headgear Force System: 3D Analysis Using Finite Element Method

    PubMed Central

    Mortezai, Omid; Esmaily, Masomeh; Darvishpour, Hojat

    2015-01-01

    Objectives: Headgears are among the effective orthodontic appliances to achieve treatment goals. Unilateral molar distal movement is sometimes needed during an orthodontic treatment, which can be achieved by an asymmetric headgear. Different unilateral headgears have been introduced. The main goal of this study was to analyze the force system of unilateral expanded outer bow asymmetric headgears by the finite element method (FEM). Materials and Methods: Six 3D finite element models of a mesiodistal slice of the maxilla containing upper first molars, their periodontal ligaments (PDLs), cancellous bone, cortical bone, and a cervical headgear with expanded outer bow attached to maxillary first molars were designed in SolidWorks 2010 and meshed in ANSYS Workbench ver. 12.1. The models were the same except for the degree of outer bow expansion. The outer bow ends were loaded with 2 N force. The distal driving force and the net moment were evaluated. Results: A decrease in the distalizing force in the normal side molar from 1.69 N to 1.37 N was shown by increasing the degree of unilateral expansion. At the same time, the force increased from 2.19 N to 2.49 N in the expanded side molar. A net moment increasing from 2.26 N.mm to 4.64 N.mm was also shown. Conclusion: Unilateral outer bow expansion can produce different distalizing forces in molars, which increase by increasing the expansion. PMID:26622282

  18. BOWS (bioinformatics open web services) to centralize bioinformatics tools in web services.

    PubMed

    Velloso, Henrique; Vialle, Ricardo A; Ortega, J Miguel

    2015-06-02

    Bioinformaticians face a range of difficulties to get locally-installed tools running and producing results; they would greatly benefit from a system that could centralize most of the tools, using an easy interface for input and output. Web services, due to their universal nature and widely known interface, constitute a very good option to achieve this goal. Bioinformatics open web services (BOWS) is a system based on generic web services produced to allow programmatic access to applications running on high-performance computing (HPC) clusters. BOWS intermediates the access to registered tools by providing front-end and back-end web services. Programmers can install applications in HPC clusters in any programming language and use the back-end service to check for new jobs and their parameters, and then to send the results to BOWS. Programs running in simple computers consume the BOWS front-end service to submit new processes and read results. BOWS compiles Java clients, which encapsulate the front-end web service requisitions, and automatically creates a web page that disposes the registered applications and clients. Bioinformatics open web services registered applications can be accessed from virtually any programming language through web services, or using standard java clients. The back-end can run in HPC clusters, allowing bioinformaticians to remotely run high-processing demand applications directly from their machines.

  19. Discovering Massive Runaway Stars with Infrared Bow Shock Nebulae: First Results

    NASA Astrophysics Data System (ADS)

    Andrews, Julian E.; Povich, Matthew S.; Kobulnicky, Henry A.; Chick, William T.; Dale, Daniel A.; Munari, Stephan; Olivier, Grace M.; Schurhammer, Danielle; Sorber, Rebecca L.; Wernke, Heather N.

    2016-01-01

    We have searched the plane of the Milky Way for candidate 22 μm and 24 μm infrared bow shock nebulae using the Wide-Field Infrared Survey Explorer (WISE) All-Sky Data Release and Spitzer GLIMPSE mosaic images. Infrared bow shocks driven by massive, OB stars can provide new constraints on stellar mass-loss rates and reveal new runaway late O- and early B-type stars. Candidate infrared bow shocks identified in this search were chosen using the criteria of a mostly symmetric arc-like morphology with the arc being bright in only 22 or 24 μm along with an apparent driving star associated with the bow shock in line with its axis of symmetry. Preliminary visible spectroscopic observations of candidate bow shock driving stars obtained using the Longslit Spectrograph at the Wyoming Infrared Observatory (WIRO) reveal that these visual inspections yield a 95% success rate of finding late O- or early B-type stars.This work is supported by the National Science Foundation under grants AST-1063146 (REU), AST-1411851 (RUI), and AST-1412845.

  20. Solar cycle variations in the neutral exosphere inferred from the location of the Venus bow shock

    NASA Technical Reports Server (NTRS)

    Russell, C. T.; Chou, E.; Luhmann, J. G.; Brace, L. H.

    1990-01-01

    Solar UV and EUV varies significantly during the solar cycle. Pioneer Venus can measure this variation both directly and indirectly. A direct measure of the EUV is obtained from the photoelectron current of the Langmuir probe when the spacecraft is in the solar wind. The indirect measure is by monitoring the location of the Venus bow shock. The UV and EUV both heat the upper atmosphere and ionize it. When solar activity is high, the upper atmosphere should be ionized more rapidly. This effect adds a greater number of planetary ions to the magnetosheath plasma as it flows by Venus. It is this increase in mass flow that causes the Venus bow shock to move away from its solar minimum location. Pioneer Venus has now monitored the location of the bow shock for an entire solar cycle. The bow shock location is well correlated with the variation in EUV flux as measured by the Langmuir probe. The bow shock is farther from Venus than expected from the sunspot number or 10.7 cm solar radio flux, indicating that solar UV radiation may be even stronger at the present time than would be predicted from the relationships determined during the previous solar cycle.

  1. A ketoreductase domain in the PksJ protein of the bacillaene assembly line carries out both α- and β-ketone reduction during chain growth

    PubMed Central

    Calderone, Christopher T.; Bumpus, Stefanie B.; Kelleher, Neil L.; Walsh, Christopher T.; Magarvey, Nathan A.

    2008-01-01

    The polyketide signaling metabolites bacillaene and dihydrobacillaene are biosynthesized in Bacillus subtilis on an enzymatic assembly line with both nonribosomal peptide synthetase (NRPS) and polyketide synthase (PKS) modules acting along with catalytic domains servicing the assembly line in trans. These signaling metabolites possess the unusual starter unit α-hydroxyisocaproate (α-HIC). We show here that it arises from initial activation of α-ketoisocaproate (α-KIC) by the first adenylation domain of PksJ (a hybrid PKS/NRPS) and installation on the pantetheinyl arm of the adjacent thiolation (T) domain. The α-KIC unit is elongated to α-KIC-Gly by the second NRPS module in PksJ as demonstrated by mass spectrometric analysis. The third module of PksJ uses PKS logic and contains an embedded ketoreductase (KR) domain along with two adjacent T domains. We show that this KR domain reduces canonical 3-ketobutyryl chains but also the α-keto group of α-KIC-containing intermediates on the PksJ T-domain doublet. This KR activity accounts for the α-HIC moiety found in the dihydrobacillaene/bacillaene pair and represents an example of an assembly-line dual-function α- and β-KR acting on disparate positions of a growing chain intermediate. PMID:18723688

  2. PKS 2155-304 in July 2006: H.E.S.S. results and simultaneous multi-wavelength observations

    SciTech Connect

    Lenain, Jean-Philippe; Boisson, Catherine; Sol, Helne; Zech, Andreas; Benbow, Wystan; Buehler, Rolf; Costamante, Luigi; Raue, Martin; Giebels, Berrie; Superina, Giulia; Punch, Michael; Volpe, Francesca

    2008-12-24

    The high-frequency-peaked BL Lac PKS 2155-304 is one of the brightest and best-studied VHE {gamma}-ray sources in the southern hemisphere. The High Energy Stereoscopic System (H.E.S.S.) has monitored PKS 2155-304 in 2006 and a multi-wavelength campaign involving X-ray, optical and radio observatories was triggered by the detection of an active state in July 2006, followed by the detection of two extraordinary flares on July, 28th and 30th, with peak fluxes {approx}100 times the usual values. We present results from the spectral and flux variability analysis of the VHE and simultaneous X-ray observations with Chandra during the second flare, as well as the detailed evolution of the VHE flux of PKS 2155-304 observed by H.E.S.S. in 2006. A study of flux correlations in the different frequency ranges during the second flare and the adjacent nights is discussed. We also present an interpretation of the active state of PKS 2155-304 in the framework of synchrotron self-Compton emission.

  3. RXTE, VLBA, Optical, and Radio Monitoring of the Quasars 3C 279, PKS 1510--089, and 3C 273

    NASA Technical Reports Server (NTRS)

    Marscher, A. P.; Jorstad, S. G.; Aller, M. F.; McHardy, I. M.; Balonek, T. J.

    2001-01-01

    We are continuing our combined RXTE X-ray, VLBA imaging (at 43 GHz), optical (several observatories), and radio (University of Michigan Radio Astronomy Observatory) monitoring of the quasars 3C 279 and PKS 1510-089, and have started similar monitoring of 3C 273. X-ray flares in 3C 279 and PKS 1510-089 are associated with ejections of superluminal components. In addition, there is a close connection between the optical and X-ray variability of 3C 279. There is a strong correlation between the 14.5 GHz and X-ray variability of PKS 1510-089 in 1997 and 1998 (with the radio leading the X-ray) that becomes weaker in subsequent years. X-ray fluctuations occur on a variety of timescales in 3C 273, with a major prolonged outburst in mid-2001. The lead author will discuss the correlations in terms of inverse Compton models for the X-ray emission coupled with synchrotron models for the lower-frequency radiation. Synchrotron self-Compton models can explain the "reverse" time lag in PKS 1510-089 is well as the variable correlation between the X-ray variations and those at lower frequencies in this object and in 3C 279.

  4. Identification of a hybrid PKS-NRPS required for the biosynthesis of NG-391 in Metarhizium anisopliae var. anisopliae

    USDA-ARS?s Scientific Manuscript database

    A 19,818 kb genomic region harboring six predicted ORFs was identified in M. anisopliae ARSEF 2575. ORF4, putatively encoding a hybrid polyketide synthase-nonribosomal peptide synthetase (PKS-NRPS) was targeted using Agrobacterium-mediated gene knockout. Homologous recombinants failed to produce det...

  5. A rapid PCR assay to characterize the intact pks15/1 gene, a virulence marker in Mycobacterium tuberculosis.

    PubMed

    Zenteno-Cuevas, Roberto; Hernandez-Morales, Rodrigo Javier; Pérez-Navarro, Lucia Monserrat; Muñiz-Salazar, Raquel; Santiago-García, Juan

    2016-02-01

    Intact pks15/1 is involved in the biosynthesis of phenolic glycolipids and proposed as a marker for virulence and phylogeny in tuberculosis. Identification of intact condition is achieved mainly by DNA sequencing. For this reason the aim of this study was to develop a reproducible endpoint PCR-assay to characterize it.

  6. Swift Follow-up of the recent Gamma-ray flare of the FSRQ PKS B1035-281

    NASA Astrophysics Data System (ADS)

    Carpenter, Bryce; Ojha, Roopesh

    2016-03-01

    Following a recent gamma-ray flare of the flat spectrum radio quasar PKS B1035-281 (ATel#8740), two Swift target of opportunity observations were performed on 2016 February 26 and March 2. Swift/XRT data were taken in Photon Counting mode for a total exposure of about 4.7 ksec and 4.0 ksec, respectively.

  7. Fermi-LAT detection of hard spectrum gamma-ray activity from the FSRQ PKS 1532+01

    NASA Astrophysics Data System (ADS)

    Ciprini, S.; Cheung, C. C.

    2015-03-01

    The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux and an unusually hard gamma-ray spectrum from a source positionally consistent with the flat spectrum radio quasar (FSRQ) PKS 1532+01 (also known as 3FGL J1534.5+0128, Acero et al.

  8. ATel 7453: Fermi LAT detection of a GeV flare from the FSRQ PKS 2032+107

    NASA Astrophysics Data System (ADS)

    Orienti, M.; D'Ammando, F.; Fermi Large Area Telescope Collaboration

    2015-04-01

    The Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope, has observed gamma-ray flaring activity from a source positionally consistent with the flat spectrum radio quasar PKS 2032+107 (also known as 3FGL J2035.3+1055, Acero et al. ...

  9. A Hybrid NRPS-PKS Gene Cluster Related to the Bleomycin Family of Antitumor Antibiotics in Alteromonas macleodii Strains

    PubMed Central

    Mizuno, Carolina Megumi; Kimes, Nikole E.; López-Pérez, Mario; Ausó, Eva; Rodriguez-Valera, Francisco; Ghai, Rohit

    2013-01-01

    Although numerous marine bacteria are known to produce antibiotics via hybrid NRPS-PKS gene clusters, none have been previously described in an Alteromonas species. In this study, we describe in detail a novel hybrid NRPS-PKS cluster identified in the plasmid of the Alteromonasmacleodii strain AltDE1 and analyze its relatedness to other similar gene clusters in a sequence-based characterization. This is a mobile cluster, flanked by transposase-like genes, that has even been found inserted into the chromosome of some Alteromonasmacleodii strains. The cluster contains separate genes for NRPS and PKS activity. The sole PKS gene appears to carry a novel acyltransferase domain, quite divergent from those currently characterized. The predicted specificities of the adenylation domains of the NRPS genes suggest that the final compound has a backbone very similar to bleomycin related compounds. However, the lack of genes involved in sugar biosynthesis indicates that the final product is not a glycopeptide. Even in the absence of these genes, the presence of the cluster appears to confer complete or partial resistance to phleomycin, which may be attributed to a bleomycin-resistance-like protein identified within the cluster. This also suggests that the compound still shares significant structural similarity to bleomycin. Moreover, transcriptomic evidence indicates that the NRPS-PKS cluster is expressed. Such sequence-based approaches will be crucial to fully explore and analyze the diversity and potential of secondary metabolite production, especially from increasingly important sources like marine microbes. PMID:24069455

  10. A numerical study on bow shocks around the lightning return stroke channel

    SciTech Connect

    Chen, Qiang Chen, Bin Yi, Yun; Chen, P. F.; Mao, Yunfei; Xiong, Run

    2015-03-15

    Bow shock structures are important to various hydrodynamics and magnetohydrodynamics (MHD) phenomena in geophysics and astrophysics. The formation and propagation of bow shocks around the lightning return stroke channel are investigated based on the self-similar motion theory and simulated with a two-dimensional Eulerian finite volume resistive radiation MHD code. In this framework, as verification of theoretical models, the evolving structures of many quantities, such as the plasma density, temperature, pressure, shock velocity, and magnetic field, can be obtained, which present all the characteristics of bow shocks in the lightning return stroke processes. The evolution characteristics and the configuration of the curved return stroke channels, e.g., the non-ideal effects and the scaling laws, are discussed in detail. The results may have applications for some observed features of the return stroke channels and other phenomena in the lightning discharge plasmas.

  11. Sedentism, social change, warfare, and the bow in the ancient Pueblo Southwest.

    PubMed

    Reed, Paul F; Geib, Phil R

    2013-01-01

    In the ancient American Southwest, use of the bow developed relatively rapidly among Pueblo people by the fifth century AD. This new technology replaced the millennia-old atlatl and dart weaponry system. Roughly 150 years later in the AD 600s, Pueblo socioeconomic organization began to evolve rapidly, as many groups adopted a much more sedentary life. Multiple factors converged to allow this sedentary pattern to emerge, but the role of the bow in this process has not been fully explored. In this paper, we trace the development of the bow and discuss its role as sedentism emerged and social changes occurred in ancient Puebloan society from the fifth through seventh centuries AD.

  12. An IRAS/ISSA Survey of Bow Shocks Around Runaway Stars

    NASA Technical Reports Server (NTRS)

    Buren, David Van

    1995-01-01

    We searched for bow shock-like objects like those known around Oph and a Cam near the positions of 183 runaway stars. Based primarily on the presence and morphology of excess 60 micron emission we identify 56 new candidate bow shocks, for which we determine photometric and morphological parameters. Previously only a dozen or so were known. Well resolved structures are present around 25 stars. A comparison of the distribution of symmetry axes of the infrared nebulae with that of their proper motion vectors indicates that these two directions are very significantly aligned. The observed alignment strongly suggests that the structures we see arise from the interaction of stellar winds with the interstellar medium, justifying the identification of these far-infrared objects as stellar wind bow shocks.

  13. An IRAS/ISSA Survey of Bow Shocks Around Runaway Stars

    NASA Astrophysics Data System (ADS)

    van Buren, Dave; Noriega-Crespo, Alberto; Dgani, Ruth

    1995-12-01

    We searched the IRAS data for bow shock-like objects like those known around ζ Oph and α Cam near the positions of 188 runaway stars. Based primarily on the presence and morphology of excess 60 μm emission we identify 58 candidate bow shocks, for which we determine photometric and morphological parameters. Previously only a dozen or so were known. Well-resolved structures are present around 25 stars. A comparison of the distribution of symmetry axes of the infrared nebulae with the proper motions of the stars indicate the two directions are very significantly aligned. The observed alignment strongly suggests that the structures we see arise from the interaction of stellar winds with the interstellar medium, justifying the identification of these far-infrared objects as stellar wind bow shocks.

  14. Effects of the bow on social organization in Western North America.

    PubMed

    Bettinger, Robert L

    2013-01-01

    The bow more than doubled, likely tripled, the success of individuals bent on killing animal or human targets (Box ). The advent of this revolutionary technology generated different responses in western North America depending on subsistence and sociopolitical organization at the time of its arrival, roughly 2300 - 1300 B.P. Its effect was substantial in California and the Great Basin, particularly on group size, which in many places diminished as a consequence of the bow's reliability. The counter-intuitive result was to increase within group-relatedness enough to encourage intensification of plant resources, previously considered too costly. The bow rose to greatest direct economic importance with the arrival of the horse, and was put to most effective use by former Great Basin groups who maintained the family band system that had developed around intensive Great Basin plant procurement, adapting the same organization to a lifestyle centered on the equestrian pursuit of buffalo and warfare. Copyright © 2013 Wiley Periodicals, Inc.

  15. An IRAS/ISSA Survey of Bow Shocks Around Runaway Stars

    NASA Technical Reports Server (NTRS)

    Buren, David Van

    1995-01-01

    We searched for bow shock-like objects like those known around Oph and a Cam near the positions of 183 runaway stars. Based primarily on the presence and morphology of excess 60 micron emission we identify 56 new candidate bow shocks, for which we determine photometric and morphological parameters. Previously only a dozen or so were known. Well resolved structures are present around 25 stars. A comparison of the distribution of symmetry axes of the infrared nebulae with that of their proper motion vectors indicates that these two directions are very significantly aligned. The observed alignment strongly suggests that the structures we see arise from the interaction of stellar winds with the interstellar medium, justifying the identification of these far-infrared objects as stellar wind bow shocks.

  16. Transport of Solar Wind H+ and He++ Ions across Earth’s Bow Shock

    NASA Astrophysics Data System (ADS)

    Parks, G. K.; Lee, E.; Fu, S. Y.; Kim, H. E.; Ma, Y. Q.; Yang, Z. W.; Liu, Y.; Lin, N.; Hong, J.; Canu, P.; Dandouras, I.; Rème, H.; Goldstein, M. L.

    2016-07-01

    We have investigated the dependence of mass, energy, and charge of solar wind (SW) transport across Earth’s bow shock. An examination of 111 crossings during quiet SW in both quasi-perpendicular and quasi-parallel shock regions shows that 64 crossings had various degrees of heating and thermalization of SW. We found 22 crossings where the SW speed was <400 km s-1. The shock potential of a typical supercritical quasi-perpendicular shock estimated from deceleration of the SW and cutoff energy of electron flat top distribution is ˜50 Volts. We find that the temperatures of H+ and He++ beams that penetrate the shock can sometimes be nearly the same in the upstream and downstream regions, indicating little or no heating had occurred crossing the bow shock. None of the models predict that the SW can cross the bow shock without heating. Our observations are important constraints for new models of collisionless shocks.

  17. Observations of low-energy electrons upstream of the earth's bow shock

    NASA Technical Reports Server (NTRS)

    Reasoner, D. L.

    1974-01-01

    Observations of electron fluxes with a lunar-based electron spectrometer when the moon was upstream of the earth have shown that a subset of observed fluxes are strongly controlled by the interplanetary magnetic field direction. The fluxes occur only when the IMF lines connect back to the earth's bow shock. Observed densities and temperatures were in the ranges 2-4 x 0,001/cu cm and 1.7-2.8 x 1,000,000 K. It is shown that these electrons can account for increases in effective solar wind electron temperatures on bow-shock connected field lines which have been observed previously by other investigators. It is further shown that if a model of the bow shock with an electrostatic potential barrier is assumed, the potential can be estimated to be 500 volts.

  18. Energetic interplanetary nucleon flux anisotropies - The effect of earth's bow shock and magnetosheath on sunward flow

    NASA Technical Reports Server (NTRS)

    Christon, S. P.

    1982-01-01

    Attention is given to the combined, average effects of the bow shock and magnetosheath on the diffusive flow of interplanetary nuclei. The observations presented show that differences between 'connected' and 'unconnected' data subsets are apparent from the beginning of the analysis. Through an investigation of the mean unconnected diffusive anisotropy (those fluxes least affected by the earth's bow shock and magnetosheath) it is confirmed that the cross-field transport of MeV energy nuclei in interplanetary space is statistically significant and in the direction expected from the large-scale particle flux gradients. The direction of particle flow relative to the IMF is then used to show that nucleon flow characteristics on connected IMF differ from those on unconnected IMF. A scenario for producing this difference is then presented. It is concluded that the inclusion of the bow shock connected information biases measurements of the flux anisotropies of MeV energy H.

  19. Prenatal diagnosis of metatropic dysplasia: beware of the pseudo-bowing sign.

    PubMed

    Garel, Catherine; Dhouib, Amira; Sileo, Chiara; Cormier-Daire, Valérie; Ducou le Pointe, Hubert

    2014-03-01

    Metatropic dysplasia is a very rare form of osteochondrodysplasia with only one case of prenatal diagnosis described in the literature. It is characterized by marked shortening of the long bones with severe platyspondyly and dumbbell-shape metaphyses. We report a case of metatropic dysplasia that was diagnosed prenatally and describe the findings on US and CT. The pregnancy was terminated and the post-mortem radiographs are shown. The woman had been referred for short and bowed long bones. Severe metaphyseal enlargement was a misleading finding because it had been misinterpreted as limb bowing. Thus when abnormal curvature of the long bones is observed at prenatal US, attention should be drawn not only to the diaphyses but also to the metaphyses because severe metaphyseal enlargement might be responsible for pseudo-bowing.

  20. Improved bow shock models for Herbig-Haro objects - Application to HH 2A-prime

    NASA Technical Reports Server (NTRS)

    Raymond, John C.; Hartmann, Lee; Hartigan, Patrick

    1988-01-01

    An improved version of the bow shock theory previously applied to Herbig-Haro objects is presented. The modifications provide a more accurate calculation of the ionization state of material entering the bow shock. The revised preionization does not drastically affect the emission-line predictions for a 200 km/s bow shock model, though the effects will be more severe for slower shock velocities. The line profiles of the new models resemble the observed profiles somewhat more closely, and the relative emission-line intensities typically differ by 30 percent from those predicted by the older models. The models agree well with new IUE spectra and existing optical data for HH 2A-prime.

  1. Research on bulbous bow optimization based on the improved PSO algorithm

    NASA Astrophysics Data System (ADS)

    Zhang, Sheng-long; Zhang, Bao-ji; Tezdogan, Tahsin; Xu, Le-ping; Lai, Yu-yang

    2017-08-01

    In order to reduce the total resistance of a hull, an optimization framework for the bulbous bow optimization was presented. The total resistance in calm water was selected as the objective function, and the overset mesh technique was used for mesh generation. RANS method was used to calculate the total resistance of the hull. In order to improve the efficiency and smoothness of the geometric reconstruction, the arbitrary shape deformation (ASD) technique was introduced to change the shape of the bulbous bow. To improve the global search ability of the particle swarm optimization (PSO) algorithm, an improved particle swarm optimization (IPSO) algorithm was proposed to set up the optimization model. After a series of optimization analyses, the optimal hull form was found. It can be concluded that the simulation based design framework built in this paper is a promising method for bulbous bow optimization.

  2. High zenith angle observations of PKS 2155-304 with the MAGIC-I telescope

    NASA Astrophysics Data System (ADS)

    Aleksić, J.; Alvarez, E. A.; Antonelli, L. A.; Antoranz, P.; Asensio, M.; Backes, M.; Barres de Almeida, U.; Barrio, J. A.; Bastieri, D.; Becerra González, J.; Bednarek, W.; Berdyugin, A.; Berger, K.; Bernardini, E.; Biland, A.; Blanch, O.; Bock, R. K.; Boller, A.; Bonnoli, G.; Borla Tridon, D.; Braun, I.; Bretz, T.; Cañellas, A.; Carmona, E.; Carosi, A.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Cossio, L.; Covino, S.; Dazzi, F.; De Angelis, A.; De Caneva, G.; De Cea del Pozo, E.; De Lotto, B.; Delgado Mendez, C.; Diago Ortega, A.; Doert, M.; Domínguez, A.; Dominis Prester, D.; Dorner, D.; Doro, M.; Eisenacher, D.; Elsaesser, D.; Ferenc, D.; Fonseca, M. V.; Font, L.; Fruck, C.; García López, R. J.; Garczarczyk, M.; Garrido, D.; Giavitto, G.; Godinović, N.; Gozzini, S. R.; Hadasch, D.; Häfner, D.; Herrero, A.; Hildebrand, D.; Höhne-Mönch, D.; Hose, J.; Hrupec, D.; Jogler, T.; Kellermann, H.; Klepser, S.; Krähenbühl, T.; Krause, J.; Kushida, J.; La Barbera, A.; Lelas, D.; Leonardo, E.; Lewandowska, N.; Lindfors, E.; Lombardi, S.; López, M.; López, R.; López-Oramas, A.; Lorenz, E.; Makariev, M.; Maneva, G.; Mankuzhiyil, N.; Mannheim, K.; Maraschi, L.; Marcote, B.; Mariotti, M.; Martínez, M.; Mazin, D.; Meucci, M.; Miranda, J. M.; Mirzoyan, R.; Moldón, J.; Moralejo, A.; Munar-Adrover, P.; Niedzwiecki, A.; Nieto, D.; Nilsson, K.; Nowak, N.; Orito, R.; Paiano, S.; Paneque, D.; Paoletti, R.; Pardo, S.; Paredes, J. M.; Partini, S.; Perez-Torres, M. A.; Persic, M.; Peruzzo, L.; Pilia, M.; Pochon, J.; Prada, F.; Prada Moroni, P. G.; Prandini, E.; Puerto Gimenez, I.; Puljak, I.; Reichardt, I.; Reinthal, R.; Rhode, W.; Ribó, M.; Rico, J.; Rügamer, S.; Saggion, A.; Saito, K.; Saito, T. Y.; Salvati, M.; Satalecka, K.; Scalzotto, V.; Scapin, V.; Schultz, C.; Schweizer, T.; Shayduk, M.; Shore, S. N.; Sillanpää, A.; Sitarek, J.; Snidaric, I.; Sobczynska, D.; Spanier, F.; Spiro, S.; Stamatescu, V.; Stamerra, A.; Steinke, B.; Storz, J.; Strah, N.; Sun, S.; Surić, T.; Takalo, L.; Takami, H.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Tibolla, O.; Torres, D. F.; Treves, A.; Uellenbeck, M.; Vankov, H.; Vogler, P.; Wagner, R. M.; Weitzel, Q.; Zabalza, V.; Zandanel, F.; Zanin, R.

    2012-08-01

    Context. The high frequency peaked BL Lac PKS 2155-304 with a redshift of z = 0.116 was discovered in 1997 in the very high energy (VHE, E > 100 GeV) γ-ray range by the University of Durham Mark VI γ-ray Cherenkov telescope in Australia with a flux corresponding to 20% of the Crab Nebula flux. It was later observed and detected with high significance by the southern Cherenkov observatory H.E.S.S. establishing this source as the best studied southern TeV blazar. Detection from the northern hemisphere is difficult due to challenging observation conditions under large zenith angles. In July 2006, the H.E.S.S. collaboration reported an extraordinary outburst of VHE γ-emission. During the outburst, the VHE γ-ray emission was found to be variable on the time scales of minutes and with a mean flux of ~7 times the flux observed from the Crab Nebula. Follow-up observations with the MAGIC-I standalone Cherenkov telescope were triggered by this extraordinary outburst and PKS 2155-304 was observed between 28 July to 2 August 2006 for 15 h at large zenith angles. Aims: We studied the behavior of the source after its extraordinary flare. Furthermore, we developed an analysis method in order to analyze these data taken under large zenith angles. Methods: Here we present an enhanced analysis method for data taken at high zenith angles. We developed improved methods for event selection that led to a better background suppression. Results: The quality of the results presented here is superior to the results presented previously for this data set: detection of the source on a higher significance level and a lower analysis threshold. The averaged energy spectrum we derived has a spectral index of (-3.5 ± 0.2) above 400 GeV, which is in good agreement with the spectral shape measured by H.E.S.S. during the major flare on MJD 53 944. Furthermore, we present the spectral energy distribution modeling of PKS 2155-304. With our observations we increased the duty cycle of the source

  3. Proper motions of five OB stars with candidate dusty bow shocks in the Carina Nebula

    NASA Astrophysics Data System (ADS)

    Kiminki, Megan M.; Smith, Nathan; Reiter, Megan; Bally, John

    2017-06-01

    We constrain the proper motions of five OB stars associated with candidate stellar wind bow shocks in the Carina Nebula using Hubble Space Telescope ACS imaging over 9-10 yr baselines. These proper motions allow us to directly compare each star's motion to the orientation of its candidate bow shock. Although these stars are saturated in our imaging, we assess their motion by the shifts required to minimize residuals in their airy rings. The results limit the direction of each star's motion to sectors less than 90° wide. None of the five stars are moving away from the Carina Nebula's central clusters as runaway stars would be, confirming that a candidate bow shock is not necessarily indicative of a runaway star. Two of the five stars are moving tangentially relative to the orientation of their candidate bow shocks, both of which point at the OB cluster Trumpler 14. In these cases, the large-scale flow of the interstellar medium, powered by feedback from the cluster, appears to dominate over the motion of the star in producing the observed candidate bow shock. The remaining three stars all have some component of motion towards the central clusters, meaning that we cannot distinguish whether their candidate bow shocks are indicators of stellar motion, of the flow of ambient gas or of density gradients in their surroundings. In addition, these stars' lack of outward motion hints that the distributed massive-star population in Carina's South Pillars region formed in place, rather than migrating out from the association's central clusters.

  4. Numerical Simulation of the SVS 13 Microjet and Bow Shock Bubble

    NASA Astrophysics Data System (ADS)

    Gardner, Carl L.; Jones, Jeremiah R.; Hodapp, Klaus W.

    2016-10-01

    Numerical simulations of the SVS 13 microjet and bow shock bubble are performed using the WENO method that reproduces the main features and dynamics of data from the Keck Telescope/OSIRIS velocity-resolved integral field spectrograph: an expanding, cooler bow shock bubble, with the bubble center moving at approximately 50 km s-1 with a radial expansion velocity of 11 km s-1, surrounding the fast, hotter jet, which is propagating at 156 km s-1. Contact and bow shock waves are visible in the simulations both from the initial short jet pulse that creates the nearly spherical bow shock bubble and from the fast microjet, while a terminal Mach disk shock is visible near the tip of the continuous microjet, which reduces the velocity of the jet gas down to the flow velocity of the contact discontinuity at the leading edge of the jet. At 21.1 years after the launch of the initial bubble pulse, the jet has caught up with and penetrated almost all the way across the bow shock bubble of the slower initial pulse. At times later than about 22 years, the jet has penetrated through the bubble and thereafter begins to subsume its spherical form. Emission maps from the simulations of the jet—traced by the emission of the shock-excited 1.644 μm [Fe ii] line—and the bow shock bubble—traced in the lower excitation 2.122 μm H2 1-0 S(1) line—projected onto the plane of the sky are presented, and are in good agreement with the Keck observations.

  5. The Evolution and Structure of the Bow Echo/microburst Events.

    NASA Astrophysics Data System (ADS)

    Lee, Wen-Chau

    The evolution and structure of several bow echo/microburst events are investigated in this study. Multiple Doppler radar analysis (three dimensional wind fields, pressure and buoyancy retrievals, vorticity budget and trajectory) is performed for the primary case of July 14, 1982 during the Joint Airport Weather Study (JAWS) experiment while single Doppler radar analysis is performed in 4 other bow echo/microburst events. The downdraft is initiated by precipitation loading at 4 km Above Ground Level (AGL) 7 min before the surface microburst. The precipitation particles within the reflectivity core contribute not only to the loading effect but also to the cooling effect via evaporation, melting and sublimation. The downdraft core initially coincides with the reflectivity core but shifts toward the weak echo region at the peak microburst time. A high perturbation pressure (maximum of 0.6 mb) builds up from the surface at the microburst center upon impact with the ground. At the surface, the microburst air is warmer than its environment. A maximum cooling of 3^circ C is located at 1.6 km at the reflectivity gradient region. The reflectivity core precedes the descent of the downdraft core, while the maximum w correlates well with the maximum negative buoyancy. The storm relative trajectories indicate that the source region of the microburst air is from 3-4 km level. A conceptual model of the single-cell type bow echo evolution is constructed based on the vorticity budget analysis. A bow echo is formed by the redistribution of hydrometeors by a vorticity couplet which is generated by the interaction between the downdraft and the vertical shear vector or the tilting effect. The rear inflow jet is induced by the vorticity couplet and its intensity should depend on the strength of the vorticity couplet. This model indicates that a bow echo may be produced by a weak downdraft as long as a proper vertical shear exists. However, strong downdrafts of microburst intensity will

  6. Thin sheets of energetic electrons upstream from the earth's bow shock

    NASA Technical Reports Server (NTRS)

    Anderson, K. A.; Lin, R. P.; Martel, F.; Lin, C. S.; Parks, G. K.; Reme, H.

    1979-01-01

    ISEE spacecraft observations show that energetic (not less than 16 keV) electrons are injected into the region upstream from the earth's bow shock in a thin sheet which lies just behind the sheet of interplanetary magnetic field lines that are tangent to the shock surface. Lower energy electrons leave the shock over a much broader region. Although the energetic electron intensity varies, the sheet is nearly always present and may be a quasi-steady state feature of the bow shock. The electron velocity distribution in the thin sheet is strongly peaked and is responsible for excitation of electron plasma waves.

  7. THEMIS Observations of Unusual Bow Shock Motion, Attending a Transient Magnetospheric Event

    NASA Technical Reports Server (NTRS)

    Korotova, Galina; Sibeck, David; Omidi, N.; Angelopoulos, V.

    2013-01-01

    We present a multipoint case study of solar wind and magnetospheric observations during a transient magnetospheric compression at 2319 UT on October 15, 2008. We use high-time resolution magnetic field and plasma data from the THEMIS and GOES-11/12 spacecraft to show that this transient event corresponded to an abrupt rotation in the IMF orientation, a change in the location of the foreshock, and transient outward bow shock motion. We employ results from a global hybrid code model to reconcile the observations indicating transient inward magnetopause motion with the outward bow shock motion.

  8. Asymptotic Steady-state Solution to a Bow Shock with an Infinite Mach Number

    NASA Astrophysics Data System (ADS)

    Yalinewich, Almog; Sari, Re'em

    2016-08-01

    The problem of a cold gas flowing past a stationary obstacle is considered. We study the bow shock that forms around the obstacle and show that at large distances from the obstacle the shock front forms a parabolic solid of revolution. The profiles of the hydrodynamic variables in the interior of the shock are obtained by solution of the hydrodynamic equations in parabolic coordinates. The results are verified with a hydrodynamic simulation. The drag force on the obstacle is also calculated. Finally, we use these results to model the bow shock around an isolated neutron star.

  9. An Evaluation Of The Effects Of The Low Energy Laser On Bowed Tendons In Horses

    NASA Astrophysics Data System (ADS)

    McKibbin, L. S.

    1987-03-01

    Bowed tendons in the horse can greatly hinder it's racing career. A pulsed, 904 nm, infrared GaAs laser, peak power 2 watts, averaging .4 mW, 10 diodes per head, was used in reducing the area of the bowed tendon. This treatment proved to capacitate the horse for better race performance. Before application of the laser the wound area was shaved. A cast of playdoe was formed over the affected area. The cast was then removed and spread over a sheet of paper which consisted of a drawing of a grid in square centimeters. The squares were then counted.

  10. Simple Method for Converting Conventional Face-bow to Postural Face-bow for Recording the Relationship of Maxilla Relative to the Temporomandibular Joint

    PubMed Central

    Gooya, Ali; Zarakani, Houman; Memari, Yeganeh

    2015-01-01

    A fundamental assumption in prosthetic dentistry is that the axis-orbital plane will usually be parallel to the horizontal reference plane. Most articulator systems have incorporated this concept into their designs and use orbitale as the anterior reference point for transferring the vertical position of the maxilla to the articulator. Clinical observations of Cantonese patients suggest that in some individuals the Frankfort plane may not be horizontal, thus the orientation of the casts in the articulator is incorrect with respect to the horizontal plane. The purpose of this study was to introduce a simple method for converting the conventional face-bow to postural face-bow to reproduce the orientation of the occlusal plane relative to the true horizontal plane with the patient in Natural Head Posture (NHP). PMID:26005456

  11. Distribution of gas and galaxies around the distant quasar PKS 1614 + 051

    SciTech Connect

    Hu, E.M.; Cowie, L.L.

    1987-06-01

    The results of narrow-band and broad-band filter observations of the region surrounding the z = 3.21 quasars, PKS 1614 + 051, made under subarcsec seeing conditions with the 3.6 m CFHT telescope at Mauna Kea are reported. The nuclear region of the Lyman-alpha companion to the quasar is resolved with a FWHM of about 0.9 arcsec A magnitude fainter. Limits on detectable continuum flux from this object suggest that it is a gas cloud interacting with the quasar, and its emission is consistent with simple photoionization by the quasar. However, the presence of several galaxies around the periphery of the quasar is noted. A search of 11 additional quasars at z greater than 3 has failed to show any other such systems. It is argued that this is consistent with the statistics of extended emission line systems in low-z quasars. 11 references.

  12. MAGIC detects activity from PKS 1424+240 at very-high-energy gamma rays

    NASA Astrophysics Data System (ADS)

    Mirzoyan, Razmik

    2017-03-01

    The MAGIC telescopes have observed an increase in the very-high-energy (VHE; > 50 GeV) gamma-ray flux from PKS 1424+240, RA: 14:27:00.4 and DEC: +23:48:00, J2000.0 (Wenger, M. et al., 2000, A & AS, v.143, 9). The preliminary analysis of the MAGIC data taken on 2017/03/09, indicates an integral photon flux of (7.6 +/- 2.3) x 10^-11 [cm^-2/s] above 70 GeV. The estimated flux corresponds to 10+/-3 % of the Crab Nebula integral flux above the same energy threshold (70 GeV), and shows a hint of elevated flux in comparison with the previous detections (Archambault, S. et al., 2014, ApJL, 785,1, L16 and the references therein).

  13. The 2007 and 2008 Optical Outbursts of the Blazar PKS 1749+096

    NASA Astrophysics Data System (ADS)

    Balonek, Thomas J.; Lam, M. T.; Tam, Y. H. Ng; Scott, E. L.; Quirk, T. S.; Graber, E. L.; Gurwell, M. A.

    2009-01-01

    The BL Lac type quasar PKS 1749+096 underwent strong optical outbursts (R 13.8) during the summers of 2007 and 2008. To study the variation timescales we initiated an intensive observing program to obtain R filtered CCD images at the Colgate University Foggy Bottom Observatory (FBO). These data, along with earlier observations from FBO's quasar monitoring program, reveal that during both the 2007 and 2008 outbursts this blazar reached its brightest optical level in three decades. Comparison of millimeter wavelength radio observations with the optical light curve indicates radio variations may be correlated with the optical outbursts. We gratefully acknowledge support for student research through an REU grant to the Keck Northeast Astronomy Consortium from the National Science Foundation, the NASA / New York Space Grant, and the Schlichting Student Research Fund at Colgate University.

  14. A single zone synchrotron model for flares of PKS1510-089

    NASA Astrophysics Data System (ADS)

    Basumallick, Partha Pratim; Gupta, Nayantara

    2017-02-01

    PKS 1510-089 is one of the most variable blazars. Very high energy gamma ray emission from this source was observed by H.E.S.S. during March-April 2009 and by MAGIC from February 3 to April 3, 2012 quasi-simultaneously with multi-wavelength flares. The spectral energy distributions of these flares have been modeled earlier with the external Compton mechanism which depends on our knowledge of the densities of the seed photons in the broad line region, the dusty infrared torus or a hypothetical slow sheath surrounding the jet around the radio core. Here we show that to explain the multi-wavelength data with synchrotron emission of electrons and protons the jet power should be of the order of 1048 ergs/s.

  15. MULTIWAVELENGTH OBSERVATIONS OF THE GAMMA-RAY BLAZAR PKS 0528+134 IN QUIESCENCE

    SciTech Connect

    Palma, N. I.; Boettcher, M.; Li, Y.; De la Calle, I.; Agudo, I.; Jorstad, S. G.; Joshi, M.; Aller, M.; Aller, H.; Bach, U.; BenItez, E.; Buemi, C. S.; Leto, P.; Escande, L.; Gurwell, M. A.; Heidt, J.; Hiriart, D.; Laehteenmaeki, A.; Larionov, V. M. E-mail: marscher@bu.edu E-mail: jlgomez@iaa.es

    2011-07-01

    We present multiwavelength observations of the ultraluminous blazar-type radio loud quasar PKS 0528+134 in quiescence during the period 2009 July-December. Four Target-of-Opportunity observations with the XMM-Newton satellite in the 0.2-10 keV range were supplemented with optical observations at the MDM Observatory, radio and optical data from the GLAST-AGILE Support Program of the Whole Earth Blazar Telescope and the Very Long Baseline Array, additional X-ray data from the Rossi X-ray Timing Explorer (2-10 keV) and from Suzaku (0.5-10 keV) as well as {gamma}-ray data from the Fermi Large Area Telescope in the 100 MeV-200 GeV range. In addition, publicly available data from the SMARTS blazar monitoring program and the University of Arizona/Steward Observatory Fermi Support program were included in our analysis. We found no evidence of significant flux or spectral variability in {gamma}-rays and most radio bands. However, significant flux variability on a timescale of several hours was found in the optical regime, accompanied by a weak trend of spectral softening with increasing flux. We suggest that this might be the signature of a contribution of unbeamed emission, possibly from the accretion disk, at the blue end of the optical spectrum. The optical flux is weakly polarized with rapid variations of the degree and direction of polarization, while the polarization of the 43 GHz radio core remains steady, perpendicular to the jet direction. Optical spectropolarimetry of the object in the quiescent state suggests a trend of increasing degree of polarization with increasing wavelength, providing additional evidence for an unpolarized emission component, possibly thermal emission from the accretion disk, contributing toward the blue end of the optical spectrum. Over an extended period of several months, PKS 0528+134 shows moderate (amplitude {approx}< 50%) flux variability in the X-rays and most radio frequencies on {approx}1-2 week timescales. We constructed four

  16. Detection of Lyman continuum absorption in the BL Lacertae object PKS 0735+178

    NASA Technical Reports Server (NTRS)

    Bregman, J. N.; Glassgold, A. E.; Huggins, P. J.

    1981-01-01

    The detection of the Lyman edge in the BL Lac object PKS 0735+178 at the absorption red shift determined by optical measurements leads to a lower limit for the column density of atomic hydrogen, N(H I) not less than 4(17)/sq cm. The Lyman-alpha absorption line appears to have been detected, but only an approximate upper limit can be obtained from the data, of the order of 2(19)/sq cm. This amount of atomic hydrogen is less than that for a line of sight through the disk of a normal spiral galaxy. It is suggested that the absorbing material exists either in the halo of a galaxy or in the tenuous, extended, gaseous disk of a galaxy.

  17. A γ-ray Quasi-periodic Modulation in the Blazar PKS 0301-243?

    NASA Astrophysics Data System (ADS)

    Zhang, Peng-Fei; Yan, Da-Hai; Zhou, Jia-Neng; Fan, Yi-Zhong; Wang, Jian-Cheng; Zhang, Li

    2017-08-01

    We report a nominally high-confidence γ-ray quasi-periodic modulation in the blazar PKS 0301-243. For this target, we analyze its Fermi-LAT Pass 8 data from 2008 August to 2017 May. Two techniques, i.e., maximum likelihood optimization and exposure-weighted aperture photometry, are used to build the γ-ray light curves. Then, both the Lomb-Scargle periodogram and the weighted wavelet Z-transform are applied to the light curves to search for period signals. A quasi-periodicity with a period of 2.1 ± 0.3 yr appears at the significance level of ˜ 5σ , although it should be noted that this putative quasi-period variability is seen in a data set that is barely four times longer. We speculate that this γ-ray quasi-periodic modulation may be evidence of a binary supermassive black hole.

  18. Quasi-simultaneous five-frequency VLBA observations of PKS 0528+134

    NASA Astrophysics Data System (ADS)

    Cai, H.-B.; Shen, Z.-Q.; Chen, X.; Shang, L.-L.

    2006-11-01

    We present results of Very Long Baseline Array (VLBA) observations of PKS 0528+134 at five frequencies (2.3, 5.0, 8.4, 15.4, and 22.2 GHz). These quasi-simultaneous data enable us to study the spectral distribution of Very Long Baseline Interferometer (VLBI) components for the first time in this highly variable source, from which the central compact core is identified. Our observations indicate that there are two bendings for the jet motion at parsec scale. We provide an approximate spatial fit to the curved jet trajectory using the Steffen et al. (1995) helical model. We further investigate the proper motions of three jet components, which all show superluminal motion. At high frequencies (15.4 and 22.2 GHz) we detected a new component, which is estimated to be related to a radio burst peaking at about 2000.

  19. Simultaneous multi-wavelength campaign on PKS 2005-489 in a high state

    NASA Astrophysics Data System (ADS)

    H.E.S.S. Collaboration; Abramowski, A.; Acero, F.; Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Barnacka, A.; Barres de Almeida, U.; Bazer-Bachi, A. R.; Becherini, Y.; Becker, J.; Behera, B.; Bernlöhr, K.; Bochow, A.; Boisson, C.; Bolmont, J.; Bordas, P.; Brucker, J.; Brucker, J.; Brun, F.; Brun, P.; Bulik, T.; Büsching, I.; Casanova, S.; Cerruti, M.; Chadwick, P. M.; Charbonnier, A.; Chaves, R. C. G.; Cheesebrough, A.; Chounet, L.-M.; Clapson, A. C.; Coignet, G.; Conrad, J.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; Dickinson, H. J.; Djannati-Ataï, A.; Domainko, W.; O'C. Drury, L.; Dubois, F.; Dubus, G.; Dyks, J.; Dyrda, M.; Egberts, K.; Eger, P.; Espigat, P.; Fallon, L.; Farnier, C.; Fegan, S.; Feinstein, F.; Fernandes, M. V.; Fiasson, A.; Fontaine, G.; Förster, A.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Gast, H.; Gérard, L.; Gerbig, D.; Giebels, B.; Glicenstein, J. F.; Glück, B.; Goret, P.; Göring, D.; Hague, J. D.; Hampf, D.; Hauser, M.; Heinz, S.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Hofverberg, P.; Horns, D.; Jacholkowska, A.; de Jager, O. C.; Jahn, C.; Jamrozy, M.; Jung, I.; Kastendieck, M. A.; Katarzynski, K.; Katz, U.; Kaufmann, S.; Keogh, D.; Kerschhaggl, M.; Khangulyan, D.; Khélifi, B.; Klochkov, D.; Kluzniak, W.; Kneiske, T.; Komin, Nu.; Kosack, K.; Kossakowski, R.; Laffon, H.; Lamanna, G.; Lenain, J.-P.; Lennarz, D.; Lohse, T.; Lopatin, A.; Lu, C.-C.; Marandon, V.; Marcowith, A.; Masbou, J.; Maurin, D.; Maxted, N.; McComb, T. J. L.; Medina, M. C.; Méhault, J.; Nguyen, N.; Moderski, R.; Moulin, E.; Naumann-Godo, M.; de Naurois, M.; Nedbal, D.; Nekrassov, D.; Nicholas, B.; Niemiec, J.; Nolan, S. J.; Ohm, S.; Olive, J.-F.; de Oña Wilhelmi, E.; Opitz, B.; Ostrowski, M.; Oya, I.; Panter, M.; Paz Arribas, M.; Pedaletti, G.; Pelletier, G.; Petrucci, P.-O.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raue, M.; Rayner, S. M.; Reimer, A.; Reimer, O.; Renaud, M.; de Los Reyes, R.; Rieger, F.; Ripken, J.; Rob, L.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Ryde, F.; Sahakian, V.; Santangelo, A.; Schlickeiser, R.; Schöck, F. M.; Schulz, A.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Sikora, M.; Skilton, J. L.; Sol, H.; Spengler, G.; Stawarz, L.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Sushch, I.; Szostek, A.; Tam, P. H.; Tavernet, J.-P.; Terrier, R.; Tibolla, O.; Tluczykont, M.; Valerius, K.; van Eldik, C.; Vasileiadis, G.; Venter, C.; Vialle, J. P.; Viana, A.; Vincent, P.; Vivier, M.; Völk, H. J.; Volpe, F.; Vorobiov, S.; Vorster, M.; Wagner, S. J.; Ward, M.; White, R.; Wierzcholska, A.; Zajczyk, A.; Zdziarski, A. A.; Zech, A.; Zechlin, H.-S.; Fermi LAT Collboration; Abdo, A. A.; Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Cannon, A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cutini, S.; Dermer, C. D.; de Palma, F.; Do Couto E Silva, E.; Drell, P. S.; Dubois, R.; Dumora, D.; Escande, L.; Favuzzi, C.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S.-H.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G. M.; Makeev, A.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nishino, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Sadrozinski, H. F.-W.; Sanchez, D.; Sander, A.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Troja, E.; Uehara, T.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.

    2011-09-01

    The high-frequency peaked BL Lac object PKS 2005-489 was the target of a multi-wavelength campaign with simultaneous observations in the TeV γ-ray (H.E.S.S.), GeV γ-ray (Fermi/LAT), X-ray (RXTE, Swift), UV (Swift) and optical (ATOM, Swift) bands. This campaign was carried out during a high flux state in the synchrotron regime. The flux in the optical and X-ray bands reached the level of the historical maxima. The hard GeV spectrum observed with Fermi/LAT connects well to the very high energy (VHE, E > 100 GeV) spectrum measured with H.E.S.S.

  20. The heating of X-ray gas by radio gas in cluster PKS0745-191

    NASA Astrophysics Data System (ADS)

    Xiang, F.; Chen, Y.; Wu, M.; Lu, F. J.; Song, L. M.; Jia, S. M..

    2004-05-01

    A calculation about the energy evolution of the relativistic particles in galaxy clusters is presented. The heating of X-ray gas by radio gas in cluster PKS 0745-191 is derived through a combined analysis of Chandra data and VLA radio observations. It was found that the heating of X-ray gas by radio gas is not enough to supply the energy lose by the X-ray emission when the low energy cut-off in the power-law spectrum of the relativistic electrons is set to 0.001erg. Therefore further computing is made to study the heating of X-ray gas by radio gas with different low energy cut-off is computed and the low energy cut-off values.

  1. The L-alpha/H-alpha intensity ratio in PKS 0237-23. [quasar

    NASA Technical Reports Server (NTRS)

    Hyland, A. R.; Becklin, E. E.; Neugebauer, G.

    1978-01-01

    The ratio I(L-alpha)/I(H-alpha) has been measured to be 1.7 plus or minus 0.6 in the quasar PKS 0237-23. The measured ratio is similar to that measured in 3C 273 by Davidsen et al. and to that inferred by Baldwin from a study of a large number of quasars; it is a factor of 5 to 14 smaller than expected from recombination theory. If the L-alpha radiation is resonantly scattered and there are modest amounts of dust within the ionized region, the measured ratio may be interpreted in terms of recombination theory, with L-alpha being depleted by absorption by the dust.

  2. Detection of gamma-ray emission from the quasar PKS 0208-512

    NASA Technical Reports Server (NTRS)

    Bertsch, D. L.; Dingus, B. L.; Fichtel, C. E.; Hartman, R. C.; Hunter, S. D.; Kanbach, G.; Kniffen, D. A.; Lin, Y. C.; Mattox, J. R.; Mayer-Hasselwander, H. A.

    1993-01-01

    High-energy gamma-ray emission has been detected from the quasar PKS 0208-512 in the energy range above 30 MeV by the Energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory. This region of sky was observed in five different viewing periods, and evidence of time variability in the gamma-ray emission by more than a factor of 3 was found. At the maximum intensity between 1991 September 19 and October 3, the flux density above 100 MeV was (9.1 +/- 0.4) x 10 exp -7 gamma/sq cm per sec. The photon spectrum during this period may be expressed as a power law with an exponent of - 1.69 +/- 0.05 between 30 MeV and 4 GeV. This is the hardest quasar spectrum observed by EGRET up to the present time.

  3. Detection of gamma-ray emission from the quasar PKS 0208-512

    NASA Technical Reports Server (NTRS)

    Bertsch, D. L.; Dingus, B. L.; Fichtel, C. E.; Hartman, R. C.; Hunter, S. D.; Kanbach, G.; Kniffen, D. A.; Lin, Y. C.; Mattox, J. R.; Mayer-Hasselwander, H. A.

    1993-01-01

    High-energy gamma-ray emission has been detected from the quasar PKS 0208-512 in the energy range above 30 MeV by the Energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory. This region of sky was observed in five different viewing periods, and evidence of time variability in the gamma-ray emission by more than a factor of 3 was found. At the maximum intensity between 1991 September 19 and October 3, the flux density above 100 MeV was (9.1 +/- 0.4) x 10 exp -7 gamma/sq cm per sec. The photon spectrum during this period may be expressed as a power law with an exponent of - 1.69 +/- 0.05 between 30 MeV and 4 GeV. This is the hardest quasar spectrum observed by EGRET up to the present time.

  4. An unusually strong Einstein ring in the radio source PKS1830 - 211

    NASA Technical Reports Server (NTRS)

    Jauncey, D. L.; Reynolds, J. E.; Tzioumis, A. K.; Murphy, D. W.; Preston, R. A.; Jones, D. L.; Meier, D. L.; Hoard, D. W.; Lobdell, E. T.; Skjerve, L.

    1991-01-01

    High-resolution radio images of PKS1830 - 211 are obtained to study the possibility that the double structure is a gravitationally lensed object. The VLBI observations, taken from interferometric radiotelescope networks, reveal an elliptical ring that connects two bright spots of similar composition. Because the lens and the lensed object are closely aligned, and because of the structure of the two spots, the source is concluded to be a radio Einstein ring. The source is found to be close to the galactic plane, and the lens and the lensed object are extragalactic. The source is also found to be unusually bright, suggesting that it is aligned with a bright background source or amplified by some mechanism related to a source that is not so bright.

  5. The increasing X-Ray Activity of PKS 2155-304

    NASA Astrophysics Data System (ADS)

    Kapanadze, Bidzina

    2016-10-01

    The southern TeV-detected HBL source PKS 2155-304 (z=0.116) is prominent with its very strong TeV/X-ray flaring behaviour (see, e.g., Aharonian et al. 2009, A & A, 502, 749; Abramowski et al. 2012, A & A, 539; Kapanadze et al. 2014, MNRAS, 444; 1076), and, therefore, it represents one of the frequent Swift targets (203 observations since 2005 November 17). In the framework of our Target of Opportunity (ToO) request Number 8344, the source was pointed nine time by X-Ray Telescope onboard the Swift satellite (Swift-XRT) since 2016 August 5 with one week intervals between the successive observations.

  6. OH+ and H2O+ absorption toward PKS 1830-211

    NASA Astrophysics Data System (ADS)

    Muller, S.; Müller, H. S. P.; Black, J. H.; Beelen, A.; Combes, F.; Curran, S.; Gérin, M.; Guélin, M.; Henkel, C.; Martín, S.; Aalto, S.; Falgarone, E.; Menten, K. M.; Schilke, P.; Wiklind, T.; Zwaan, M. A.

    2016-11-01

    We report the detection of OH+ and H2O+ in the z = 0.89 absorber toward the lensed quasar PKS 1830-211. The abundance ratio of OH+ and H2O+ is used to quantify the molecular hydrogen fraction (fH2) and the cosmic-ray ionization rate of atomic hydrogen (ζH) along two lines of sight, located at 2 kpc and 4 kpc to either side of the absorber's center. The molecular fraction decreases outward, from 0.04 to 0.02, comparable to values measured in the Milky Way at similar galactocentric radii. For ζH , we find values of 2 × 10-14 s-1 and 3 × 10-15 s-1, respectively, which are slightly higher than in the Milky Way at comparable galactocentric radii, possibly due to a higher average star formation activity in the z = 0.89 absorber. The ALMA observations of OH+, H2O+, and other hydrides toward PKS 1830-211reveal the multi-phase composition of the absorbing gas. Taking the column density ratios along the southwest and northeast lines of sight as a proxy of molecular fraction, we classify the species ArH+, OH+, H2Cl+, H2O+, CH, and HF as tracing gases increasingly more molecular. Incidentally, our data allow us to improve the accuracy of H2O+ rest frequencies and thus refine the spectroscopic parameters. The reduced spectra (FITS files) are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/595/A128

  7. AGN feedback in X-ray luminous galaxy cluster: PKS 0745-191

    NASA Astrophysics Data System (ADS)

    Sonkamble, Satish Shripati; Vagshette, Nilkanth Dattatray; Patil, Madhav Khushalrao

    2015-08-01

    We present 117 ks Chandra observation of the cooling flow cluster PKS 0745-191 providing evidence of the strong interaction between the radio source associated with the center dominant galaxy PGC 021813 and the intra-cluster gas. This system is one of the strongest cool core cluster, requiring extreme mechanical feedback from its central AGN to offset cooling of the ICM. This analysis has enabled us to detect two pairs of X-ray cavities in the central ˜ 20 kpc region. In addition to the cavities, we have also evidenced relatively cooler X-ray arc and a temperature jump due to the shock front at 92'' (184 kpc) on the western side. 2D temperature maps as well as spectral analysis of X-ray photons extracted from wedge shaped reigns revealed six different cold fronts, 3 along the eastern direction, 2 on the west direction and one in the south direction of the X-ray peak. The apparent positions of cold fronts are found to match with the spiral structure apparent in the X-ray surface brightness distribution of PKS 0745-191 that is probably due to the gas sloshing. The Mach number for this shock is found to be ˜ 1.36. Systematic study of the X-ray cavities revealed a mechanical power of ˜ 2.95 X 1045 erg s-1 and is sufficient to offset the cooling due to radiative loss. We found that the radio source associated with the center dominant galaxy of this cluster is efficient enough to carve the observed cavities. The ratio of radio luminosity to mechanical cavity power is ˜ 10-3 .

  8. A Photohadronic Model of the Large-scale Jet of PKS 0637-752

    NASA Astrophysics Data System (ADS)

    Kusunose, Masaaki; Takahara, Fumio

    2017-01-01

    Strong X-ray emission from large scale jets of radio loud quasars still remains an open problem. Models based on inverse Compton scattering off cosmic microwave background photons by relativistically beamed jets have recently been ruled out, since Fermi LAT observations for 3C 273 and PKS 0637–752 give the upper limit far below the model prediction. Synchrotron emission from a separate electron population with multi-hundred TeV energies remains a possibility although its origin is not well known. We examine a photo-hadronic origin of such high energy electrons/positrons, assuming that protons are accelerated up to 1019 eV and produce electrons/positrons through a Bethe–Heitler process and photo-pion production. These secondary electrons/positrons are injected at sufficiently high energies and produce X-rays and γ-rays by synchrotron radiation without conflicting with the Fermi LAT upper limits. We find that the resultant spectrum well reproduces the X-ray observations from PKS 0637-752, if the proton power is at least {10}49 {erg} {{{s}}}-1, which is highly super-Eddington. It is noted that the X-ray emission originates primarily from leptons through a Bethe–Heitler process, while leptons from photo-pion origin lose energy directly through synchrotron emission of multi-TeV photons rather than cascading. To avoid the overproduction of the optical flux, optical emission is primarily due to synchrotron emission of secondary leptons rather than primary electrons, or a mild degree of beaming of the jet is needed if it is owing to the primary electrons. Proton synchrotron luminosity is a few orders of magnitude smaller.

  9. Investigating the emission mechanisms of the jet in the quasar PKS 1127-145

    NASA Astrophysics Data System (ADS)

    Duffy, Ryan T.; Siemiginowska, A.; Kashyap, V.; Stein, N.; Migliori, G.

    2014-01-01

    There is currently uncertainty surrounding the emission mechanism for X-ray photons in quasar jets, with both Inverse Compton Scattering from the Cosmic Microwave Background (IC/CMB) and synchrotron models considered possibilities. We use a 100 ks observation (Siemiginowska et al 2007) of the redshift z=1.18, radio-loud quasar PKS 1127-145 taken by the Chandra X-ray Observatory, with the hope of accurately measuring the offsets between radio and X-ray radiation peaks in order to establish the emission process for this jet. PKS 1127-145 is a bright quasar with a long jet which has several bright knots and complex morphology, making it a perfect source for this investigation. We use a Bayesian statistical method called Low-Count Image Restoration and Analysis (LIRA, Connors & van Dyk 2007, Esch et al 2004) to investigate the quasar jet. This fits the parameters of a multiscale model to the data by employing a Markov Chain Monte Carlo process. LIRA has shown the location of some jet X-ray components, although further simulations must be undertaken to determine whether these are statistically significant. We also study these jet X-ray components in both hard and soft X-ray bands in order to gain more information on the energy of the emitted photons. References: Connors, A., & van Dyk, D. A. 2007, Statistical Challenges in Modern Astronomy IV, 371, 101 Esch, D.N., Connors, A., Karovska, M., & van Dyk, D.A. 2004, ApJ, 610, 1213 Siemiginowska, A., Stawarz, L., Cheung, C.C., et al. 2007, ApJ, 657, 145

  10. PKS 1718-649: a broad-band study of a young radio jet

    NASA Astrophysics Data System (ADS)

    Sobolewska, Malgosia; Siemiginowska, Aneta; Migliori, Giulia; Guainazzi, Matteo; Hardcastle, Martin; Ostorero, Luisa; Stawarz, Lukasz

    2017-08-01

    Physical conditions required to launch and sustain a jet and the jet's impact on black hole surroundings are believed to be strongly linked, and lie at the core of the AGN feedback idea. The physics of the initial stages of a radio jet expansion is still poorly understood. Nevertheless, highly relativistic plasma contained within young radio lobes and shocks accompanying a powerful jet expansion are expected to generate high energy radiation. However, this initial phase is short-lived and observing young radio sources at high energies has been challenging, with only a few sources detected before the Chandra and XMM-Newton era. We compiled a sample of Compact Symmetric Objects (CSO) that have kinematic age determination to study their high energy properties. Here we discuss one of the sources from our sample, PKS 1718-649 (z=0.014), hosting the most compact (2 pc) and youngest (100 years) extragalactic radio jet known to date. We observed PKS 1718-649 for the first time in X-rays and found that it is a low luminosity X-ray source, L(2-10 keV) ~ 6 x 1041 erg s-1, and its X-ray spectrum is consistent with a mildly (intrinsically) absorbed power law (Gamma ~ 1.75, NH ~ 1021 cm-2). In addition, using the Fermi/LAT archive we established that this source is the first robustly confirmed gamma-ray CSO emitter. Merging the archival radio-to-optical data and our high energy results, we constructed a high quality broad-band spectral energy distribution of this source. We tested a theoretical scenario in which the high energy emission of the source arises due to the Inverse Compton upscattering of the low energy photons off the non-thermal electrons in the expanding radio lobes. We discuss the impact of the expanding lobes on the environment, and constraints imposed by the data on the electron distribution within the lobes.

  11. Time-dependent Modeling of Gamma-Ray Flares in Blazar PKS1510--089

    NASA Astrophysics Data System (ADS)

    Saito, S.; Stawarz, Ł.; Tanaka, Y. T.; Takahashi, T.; Sikora, M.; Moderski, R.

    2015-08-01

    Here we present a new approach for constraining luminous blazars, incorporating fully time-dependent and self-consistent modeling of bright γ-ray flares of PKS 1510-089, resolved with Fermi-LAT, in the framework of the internal shock scenario. The results of our modeling imply the location of the γ-ray flaring zone to be outside of the broad-line region, namely around ≃ 0.3 pc from the core for a free-expanding jet with the opening angle {{Γ }} {θ }{jet}≃ 1 (where Γ is the jet bulk Lorentz factor), up to ≃ 3 pc for a collimated outflow with {{Γ }} {θ }{jet}≃ 0.1. Moreover, under the {{Γ }} {θ }{jet}≃ 1 condition, our modeling indicates the maximum efficiency of the jet production during the flares, with the total jet energy flux strongly dominated by protons and exceeding the available accretion power in the source. This is in contrast to the quiescence states of the blazar, characterized by lower jet kinetic power and an approximate energy equipartition between different plasma constituents. We demostrate how strictly simultaneous observations of flaring PKS 1510-089 at optical, X-ray, and GeV photon energies, on hourly timescales, augmented by extensive simulations as presented in this paper, may help to impose further precise constraints on the magnetization and opening angle of the emitting region. In addition, our detailed modeling implies that a non-uniformity of the Doppler factor across the jet, caused by the radial expansion of the outflow, may lead to a pronounced time distortion in the observed γ-ray light curves, resulting, in particular, in asymmetric flux profiles with substantially extended decay phases.

  12. Discovery of VHE γ-rays from the BL Lacertae object PKS 0548-322

    NASA Astrophysics Data System (ADS)

    Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Barres de Almeida, U.; Bazer-Bachi, A. R.; Becherini, Y.; Behera, B.; Benbow, W.; Bernlöhr, K.; Bochow, A.; Boisson, C.; Bolmont, J.; Borrel, V.; Brucker, J.; Brun, F.; Brun, P.; Bühler, R.; Bulik, T.; Büsching, I.; Boutelier, T.; Chadwick, P. M.; Charbonnier, A.; Chaves, R. C. G.; Cheesebrough, A.; Chounet, L.-M.; Clapson, A. C.; Coignet, G.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; Dickinson, H. J.; Djannati-Ataï, A.; Domainko, W.; O'C. Drury, L.; Dubois, F.; Dubus, G.; Dyks, J.; Dyrda, M.; Egberts, K.; Emmanoulopoulos, D.; Espigat, P.; Farnier, C.; Feinstein, F.; Fiasson, A.; Förster, A.; Fontaine, G.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Gérard, L.; Gerbig, D.; Giebels, B.; Glicenstein, J. F.; Glück, B.; Goret, P.; Göring, D.; Hauser, D.; Hauser, M.; Heinz, S.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Holleran, M.; Hoppe, S.; Horns, D.; Jacholkowska, A.; de Jager, O. C.; Jahn, C.; Jung, I.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Kendziorra, E.; Kerschhaggl, M.; Khangulyan, D.; Khélifi, B.; Keogh, D.; Kluźniak, W.; Kneiske, T.; Komin, Nu.; Kosack, K.; Lamanna, G.; Lenain, J.-P.; Lohse, T.; Marandon, V.; Martin, J. M.; Martineau-Huynh, O.; Marcowith, A.; Masbou, J.; Maurin, D.; McComb, T. J. L.; Medina, M. C.; Moderski, R.; Moulin, E.; Naumann-Godo, M.; de Naurois, M.; Nedbal, D.; Nekrassov, D.; Nicholas, B.; Niemiec, J.; Nolan, S. J.; Ohm, S.; Olive, J.-F.; de Oña Wilhelmi, E.; Orford, K. J.; Ostrowski, M.; Panter, M.; Paz Arribas, M.; Pedaletti, G.; Pelletier, G.; Petrucci, P.-O.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raubenheimer, B. C.; Raue, M.; Rayner, S. M.; Renaud, M.; Rieger, F.; Ripken, J.; Rob, L.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Sahakian, V.; Santangelo, A.; Schlickeiser, R.; Schöck, F. M.; Schröder, R.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Sikora, M.; Skilton, J. L.; Sol, H.; Spangler, D.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Superina, G.; Szostek, A.; Tam, P. H.; Tavernet, J.-P.; Terrier, R.; Tibolla, O.; Tluczykont, M.; van Eldik, C.; Vasileiadis, G.; Venter, C.; Venter, L.; Vialle, J. P.; Vincent, P.; Vivier, M.; Völk, H. J.; Volpe, F.; Wagner, S. J.; Ward, M.; Zdziarski, A. A.; Zech, A.

    2010-10-01

    Aims: PKS 0548-322 (z = 0.069) is a “high-frequency-peaked” BL Lac object and a candidate very high energy (VHE, E > 100 GeV) γ-ray emitter, due to its high X-ray and radio flux. Observations at the VHE band provide insights into the origin of very energetic particles present in this source and the radiation processes at work. Methods: We report observations made between October 2004 and January 2008 with the HESS array, a four imaging atmospheric-Cherenkov telescopes. Contemporaneous UV and X-ray observations with the Swift satellite in November 2006 are also reported. Results: PKS 0548-322 is detected for the first time in the VHE band with HESS We measure an excess of 216 γ-rays corresponding to a significance of 5.6 standard deviations. The photon spectrum of the source is described by a power-law, with a photon index of Γ = 2.86 ± 0.34stat ± 0.10sys. The integral flux above 200 GeV is ~1.3% of the flux of the Crab Nebula, and is consistent with being constant in time. Contemporaneous Swift/XRT observations reveal an X-ray flux between 2 and 10 keV of F2-10 keV = (2.3±0.2)×10-11 erg cm-2 s-1, an intermediate intensity state with respect to previous observations. The spectral energy distribution can be reproduced using a simple one-zone synchrotron self Compton model, with parameters similar those observed for other sources of this type.

  13. Simultaneous Swift and REM Monitoring of the Blazar PKS 0537-441 in 2005

    NASA Astrophysics Data System (ADS)

    Pian, E.; Romano, P.; Treves, A.; Ghisellini, G.; Covino, S.; Cucchiara, A.; Dolcini, A.; Tagliaferri, G.; Markwardt, C.; Campana, S.; Chincarini, G.; Gehrels, N.; Giommi, P.; Maraschi, L.; Vergani, S. D.; Zerbi, F. M.; Molinari, E.; Testa, V.; Tosti, G.; Vitali, F.; Antonelli, L. A.; Conconi, P.; Malaspina, G.; Nicastro, L.; Palazzi, E.; Meurs, E. J. A.; Norci, L.

    2007-07-01

    The blazar PKS 0537-441 has been observed with all instruments of the Swift satellite between the end of 2004 and 2005 November. The BAT monitored it recurrently for a total of 2.7 Ms, and the XRT and UVOT pointed it on seven occasions for a total of 67 k. The automatic optical and near-infrared telescope REM has monitored simultaneously the source at all times. In 2005 January-February, PKS 0537-441 was detected at its brightest in optical and X-rays: more than a factor of 2 brighter in X-rays and about a factor of 60 brighter in the optical than observed in 2004 December. The 2005 July observation recorded a fainter X-ray state, albeit still brighter than the historical average. The simultaneous optical state is comparable to the one recorded in early 2005 January, before the outburst. In 2005 November, the source subsided both in X-rays and optical to a quiescent state. The optical and X-ray variations are well correlated, with no measurable time lag larger than about 1 month. On intraday timescales there is no obvious correlation between X-ray and optical variations, but the former tend to be more pronounced, opposite to what is observed on monthly timescales. The widely different amplitude of the long-term variability in optical and X-rays is very unusual. The spectral energy distributions are interpreted in terms of the synchrotron and inverse Compton mechanisms within a jet where the plasma radiates via internal shocks and the dissipation depends on the distance of the emitting region from the central engine.

  14. PERIODIC STRUCTURE IN THE MEGAPARSEC-SCALE JET OF PKS 0637-752

    SciTech Connect

    Godfrey, L. E. H.; Ekers, R.; Lovell, J. E. J.; Burke-Spolaor, S.; Bicknell, G. V.; Jauncey, D. L.; Birkinshaw, M.; Worrall, D. M.; Schwartz, D. A.; Marshall, H. L.; Gelbord, J.; Perlman, E. S.; Georganopoulos, M.

    2012-10-20

    We present 18 GHz Australia Telescope Compact Array imaging of the megaparsec-scale quasar jet PKS 0637-752 with angular resolution {approx}0.''58. We draw attention to a spectacular train of quasi-periodic knots along the inner 11'' of the jet, with average separation {approx}1.1 arcsec (7.6 kpc projected). We consider two classes of model to explain the periodic knots: those that involve a static pattern through which the jet plasma travels (e.g., stationary shocks) and those that involve modulation of the jet engine. Interpreting the knots as re-confinement shocks implies the jet kinetic power Q{sub jet} {approx} 10{sup 46} erg s{sup -1}, but the constant knot separation along the jet is not expected in a realistic external density profile. For models involving modulation of the jet engine, we find that the required modulation period is 2 Multiplication-Sign 10{sup 3} yr < {tau} < 3 Multiplication-Sign 10{sup 5} yr. The lower end of this range is applicable if the jet remains highly relativistic on kiloparsec scales, as implied by the IC/CMB model of jet X-ray emission. We suggest that the periodic jet structure in PKS 0637-752 may be analogous to the quasi-periodic jet modulation seen in the microquasar GRS 1915+105, believed to result from limit cycle behavior in an unstable accretion disk. If variations in the accretion rate are driven by a binary black hole, the predicted orbital radius is 0.7 pc {approx}< a {approx}< 30 pc, which corresponds to a maximum angular separation of {approx}0.1-5 mas.

  15. Analysis of "Teno-uchi" maneuver in releasing Japanese-style bows based on muscle activities and forces acting on the bow.

    PubMed

    Hosoya, Satoshi; Byun, Keigo Ohyama; Okada, Morihiko

    2004-12-01

    Since a Japanese-style bow has a very complicated shape and structure, an archer has to apply the "Teno-uchi" maneuver including horizontally twisting torque, or "Nejiri", and sagittally down-pushing torque, or "Uwa-oshi", to the restoring bow in order to hit the target. The purpose of this study was to investigate the biomechanical relationship between the muscular activities of the left forearm and the operation of "Teno-uchi" maneuver. Surface EMG of left forearm muscles and the two kinds of torque acting on the bow around the time of release were recorded in 10 experienced subjects during arrow shooting. The "Biku", an involuntary resignation from release happening in the shooting, was also examined. Close analyses of the results revealed that activation of the extensor carpi ulnaris and extensor digitorum muscles together with inhibition of the flexor carpi ulnaris muscle brought about "Nejiri", while activation of the extensor carpi ulnaris as well as flexor carpi ulnaris muscles and inhibition of the extensor carpi redialis longus and extensor digitorum muscles gave rise to "Uwa-oshi", thus causing activities of trade-off nature in the extensor digitorum and flexor carpi ulnaris muscles for the "Nejiri" and "Uwa-oshi. The trade-off activities were presumably actualized through time-sharing coordination between the muscles.

  16. Acceleration at the Earth's Bow Shock: Spatial Depencence of Acceleration Efficiency

    NASA Astrophysics Data System (ADS)

    Terasawa, Toshio; Saito, Y.; Mukai, T.

    2003-07-01

    < We present GEOTAIL observations of diffuse protons (˜40 keV) in the bow shock upstream region, covering from the nominal nose upstream region to > the predawn upstream region (Xgse ˜-70 Re). Our results give conclusive evidence for the earlier suggestion on the acceleration/transport process in the predawn region, which was based on the ISEE-3 observations in 1983.

  17. Astrophysical bow shocks: an analytical solution for the hypersonic blunt body problem in the intergalactic medium

    NASA Astrophysics Data System (ADS)

    Schulreich, M. M.; Breitschwerdt, D.

    2011-07-01

    Aims: Bow shock waves are a common feature of groups and clusters of galaxies since they are generated as a result of supersonic motion of galaxies through the intergalactic medium. The goal of this work is to present an analytical solution technique for such astrophysical hypersonic blunt body problems. Methods: A method, developed by Schneider (1968, JFM, 31, 397) in the context of aeronautics, allows calculation of the galaxy's shape as long as the shape of the bow shock wave is known (so-called inverse method). In contrast to other analytical models, the solution is valid in the whole flow region (from the stagnation point up to the bow shock wings) and in particular takes into account velocity gradients along the streamlines. We compare our analytical results with two-dimensional hydrodynamical simulations carried out with an extended version of the VH-1 hydrocode which is based on the piecewise parabolic method with a Lagrangian remap. Results: It is shown that the applied method accurately predicts the galaxy's shape and the fluid variables in the post-shock flow, thus saving a tremendous amount of computing time for future interpretations of similar objects. We also find that the method can be applied to arbitrary angles between the direction of the incoming flow and the axis of symmetry of the body. We emphasize that it is general enough to be applied to other astrophysical bow shocks, such as those on stellar and galactic scales.

  18. Fuzzy Bayesian Network-Bow-Tie Analysis of Gas Leakage during Biomass Gasification

    PubMed Central

    Yan, Fang; Xu, Kaili; Yao, Xiwen; Li, Yang

    2016-01-01

    Biomass gasification technology has been rapidly developed recently. But fire and poisoning accidents caused by gas leakage restrict the development and promotion of biomass gasification. Therefore, probabilistic safety assessment (PSA) is necessary for biomass gasification system. Subsequently, Bayesian network-bow-tie (BN-bow-tie) analysis was proposed by mapping bow-tie analysis into Bayesian network (BN). Causes of gas leakage and the accidents triggered by gas leakage can be obtained by bow-tie analysis, and BN was used to confirm the critical nodes of accidents by introducing corresponding three importance measures. Meanwhile, certain occurrence probability of failure was needed in PSA. In view of the insufficient failure data of biomass gasification, the occurrence probability of failure which cannot be obtained from standard reliability data sources was confirmed by fuzzy methods based on expert judgment. An improved approach considered expert weighting to aggregate fuzzy numbers included triangular and trapezoidal numbers was proposed, and the occurrence probability of failure was obtained. Finally, safety measures were indicated based on the obtained critical nodes. The theoretical occurrence probabilities in one year of gas leakage and the accidents caused by it were reduced to 1/10.3 of the original values by these safety measures. PMID:27463975

  19. Sociopolitical effects of bow and arrow technology in prehistoric coastal California.

    PubMed

    Kennett, Douglas J; Lambert, Patricia M; Johnson, John R; Culleton, Brendan J

    2013-01-01

    Bow and arrow technology spread across California between ∼AD 250 and 1200, first appearing in the intermountain deserts of the Great Basin and later spreading to the coast. We critically evaluate the available data for the initial spread in bow and arrow technology and examine its societal effects on the well-studied Northern Channel Islands off the coast of Southern California. The introduction of this technology to these islands between AD 650 and 900 appears to predate the appearance of hereditary inequality between AD 900 and 1300. We conclude, based on the available data, that this technology did not immediately trigger intergroup warfare. We argue that the introduction of the bow and arrow contributed to sociopolitical instabilities that were on the rise within the context of increasing population levels and unstable climatic conditions, which stimulated intergroup conflict and favored the development of hereditary inequality. Population aggregation and economic intensification did occur with the introduction of the bow and arrow. This observation is consistent with the hypothesis that social coercion via intra-group "law enforcement" contributed to changes in societal scale that ultimately resulted in larger groups that were favored in inter-group conflict. We argue that the interplay between intra-group "law enforcement" and inter-group warfare were both essential for the ultimate emergence of social inequality between AD 900 and 1300. Copyright © 2013 Wiley Periodicals, Inc.

  20. Historic range of variability for upland vegetation in the Medicine Bow National Forest, Wyoming

    Treesearch

    Gregory K. Dillon; Dennis H. Knight; Carolyn B. Meyer

    2005-01-01

    An approach for synthesizing the results of ecological research pertinent to land management is the analysis of the historic range of variability (HRV) for key ecosystem variables that are affected by management activities. This report provides an HRV analysis for the upland vegetation of the Medicine Bow National Forest in southeastern Wyoming. The variables include...

  1. Photo series for quantifying forest residues in managed lands of the Medicine Bow National Forest

    Treesearch

    John B. Popp; John E. Lundquist

    2006-01-01

    This photo series presents a visual representation of a range of fuel loading conditions specifically found on the Medicine Bow National Forest. The photos are grouped by forest type and past management practices. This field guide describes the distribution of different types of woody fuels and includes some vegetation data.

  2. A three-dimensional analysis of finger and bow string movements during the release in archery.

    PubMed

    Horsak, Brian; Heller, Mario

    2011-05-01

    The aim of this paper was to examine finger and bow string movements during archery by investigating a top Austrian athlete (FITA score = 1233) under laboratory conditions. Maximum lateral bow string deflection and angular displacements for index, third, and ring fingers between the full draw position and the end of the release were quantified using a motion tracking system. Stepwise multiple regression analyses were used to determine whether bow string deflection and finger movements are predictive for scoring. Joint ranges of motion during the shot itself were large in the proximal and distal interphalangeal joints, and much smaller in the metacarpophalangeal joints. Contrary to our expectations, greater deflection leads to higher scores (R2 = .18, p < .001) and the distal interphalangeal joint of the third finger weakly predicts the deflection (R2 = .11, p < .014). More variability in the joint angles of the third finger was found in bad shots than in good shots. Findings in this study let presume that maximum lateral bow string deflection does not adversely affect the archer's performance.

  3. 10. VIEW TOWARD PORT BOW IN THE FOC'S'LE OF THE ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    10. VIEW TOWARD PORT BOW IN THE FOC'S'LE OF THE EVELINA M. GOULART. OBJECT IN THE FOREGROUND IS A FOLDING MESS TABLE LOCATED BETWEEN THE TIERS OF BUNKS. - Auxiliary Fishing Schooner "Evelina M. Goulart", Essex Shipbuilding Museum, 66 Main Street, Essex, Essex County, MA

  4. Observed Foreshock Ions which are Actually Behind the Martian Bow Shock

    NASA Astrophysics Data System (ADS)

    Frahm, Rudy A.; Yamauchi, Masatoshi; Winningham, J. David; Lundin, Rickard; Sharber, James R.; Nilsson, Hans; Coates, Andrew J.; Mukherjee, Joey

    2016-04-01

    The Mars Express (MEx) Analyzer of Space Plasmas and Energetic Atoms (ASPERA-3) experiment contains ion and electron instruments for conducting plasma measurements. On January 23, 2012, during in-bound travel of MEx in the southern hemisphere of Mars traveling from its dawn side toward periapsis at dusk, the plasma instruments measured foreshock-like ion beams extending from outside the bow shock and into the magnetosphere, continuing to a distance of about a proton gyroradius from the bow shock. These ion beams were mostly protons, were observed to have energies greater than solar wind protons, and were not gyrating, in agreement with reflections of the solar wind proton beam. Furthermore, in the foreshock region, the ion energy gradually decreased toward the magnetosheath, in agreement with an acceleration by an outward-directed electric field in the bow shock. The observations also suggest that this electric field exists even inside the magnetosheath, within the distance of a proton gyroradius from the bow shock.

  5. Fuzzy Bayesian Network-Bow-Tie Analysis of Gas Leakage during Biomass Gasification.

    PubMed

    Yan, Fang; Xu, Kaili; Yao, Xiwen; Li, Yang

    2016-01-01

    Biomass gasification technology has been rapidly developed recently. But fire and poisoning accidents caused by gas leakage restrict the development and promotion of biomass gasification. Therefore, probabilistic safety assessment (PSA) is necessary for biomass gasification system. Subsequently, Bayesian network-bow-tie (BN-bow-tie) analysis was proposed by mapping bow-tie analysis into Bayesian network (BN). Causes of gas leakage and the accidents triggered by gas leakage can be obtained by bow-tie analysis, and BN was used to confirm the critical nodes of accidents by introducing corresponding three importance measures. Meanwhile, certain occurrence probability of failure was needed in PSA. In view of the insufficient failure data of biomass gasification, the occurrence probability of failure which cannot be obtained from standard reliability data sources was confirmed by fuzzy methods based on expert judgment. An improved approach considered expert weighting to aggregate fuzzy numbers included triangular and trapezoidal numbers was proposed, and the occurrence probability of failure was obtained. Finally, safety measures were indicated based on the obtained critical nodes. The theoretical occurrence probabilities in one year of gas leakage and the accidents caused by it were reduced to 1/10.3 of the original values by these safety measures.

  6. Venusian bow shock as seen by the ASPERA-4 ion instrument on Venus Express

    NASA Astrophysics Data System (ADS)

    Whittaker, I.; Guymer, G.; Grande, M.; Pintér, B.; Barabash, S.; Federov, A.; Mazelle, C.; Sauvaud, J. A.; Lundin, R.; Russell, C. T.; Futaana, Y.; Fränz, M.; Zhang, T. L.; Andersson, H.; Grigoriev, A.; Holmström, M.; Yamauchi, M.; Asamura, K.; Baumjohann, W.; Lammer, H.; Coates, A. J.; Kataria, D. O.; Linder, D. R.; Curtis, C. C.; Hsieh, K. C.; Koskinen, H. E. J.; Kallio, E.; Riihelä, P.; Schmidt, W.; Kozyra, J.; McKenna-Lawlor, S.; Thocaven, J. J.; Orsini, S.; Cerulli-Irelli, R.; Mura, A.; Milillo, M.; Maggi, M.; Roelof, E.; Brandt, P.; Frahm, R. A.; Sharber, J. R.; Wurz, P.; Bochsler, P.

    2010-09-01

    The Analyzer of Space Plasmas and Energetic Atoms (ASPERA-4) instrument on Venus Express is used to determine bow shock position at Venus using ion data alone, using data recorded during a solar minimum from the Ion Mass Analyzer (IMA) which is part of the ASPERA-4 package. Previous models constructed from solar minimum data using Venus Express, Pioneer Venus Orbiter (PVO) and Venera 9 and 10 are also compared to the current fit. An important feature of this new fit is a statistical accuracy introduced in the form of a probability weighting function for the data points, based on the time spent in particular locations. The bow shock curve is then compared to two-dimensional ion maps. These verify the accuracy of this and previous solar minimum fit curves based on PVO and Venus Express magnetic data. Comparing all bow shock models to the 2D ion maps shows that a combination of models produces the best fit. Since all the fitted curves show differences in position they are investigated relative to the solar conditions pertaining at the times when the individual data sets were measured. The sub solar point and terminator distance were thus found to vary linearly with sunspot number and hence with solar activity. This relationship, which was already known to exist between solar maximum and solar minimum, is now shown to exist between different solar minima and even within the same minimum. This indicates a need for the mechanisms for bow shock maintenance and variance to be more closely modeled.

  7. Prototype adaptive bow-tie filter based on spatial exposure time modulation

    NASA Astrophysics Data System (ADS)

    Badal, Andreu

    2016-03-01

    In recent years, there has been an increased interest in the development of dynamic bow-tie filters that are able to provide patient-specific x-ray beam shaping. We introduce the first physical prototype of a new adaptive bow-tie filter design based on the concept of "spatial exposure time modulation." While most existing bow-tie filters operate by attenuating the radiation beam differently in different locations using partially attenuating objects, the presented filter shapes the radiation field using two movable completely radio-opaque collimators. The aperture and speed of the collimators is modulated in synchrony with the x-ray exposure to selectively block the radiation emitted to different parts of the object. This mode of operation does not allow the reproduction of every possible attenuation profile, but it can reproduce the profile of any object with an attenuation profile monotonically decreasing from the center to the periphery, such as an object with an elliptical cross section. Therefore, the new adaptive filter provides the same advantages as the currently existing static bow-tie filters, which are typically designed to work for a pre-determined cylindrical object at a fixed distance from the source, and provides the additional capability to adapt its performance at image acquisition time to better compensate for the actual diameter and location of the imaged object. A detailed description of the prototype filter, the implemented control methods, and a preliminary experimental validation of its performance are presented.

  8. Lunar Surface Potential Changes Possible Associated with Traversals of the Bow Shock

    NASA Technical Reports Server (NTRS)

    Collier, M. R.; Stubbs, T. J.; Hills, H. K.

    2008-01-01

    We report an analysis of seven Apollo 14 Apollo Lunar Surface Experiments Package (ALSEP) Suprathermal Ion Detector Experiment (SIDE) "resonance" events from January 1972 through January 1973. The events appear to be associated with traversals of the Moon through the terrestrial bow shock.

  9. Hybrid functional calculations on the band gap bowing parameters of In x Ga1-x N

    NASA Astrophysics Data System (ADS)

    Mei, Lin; Yixu, Xu; Jianhua, Zhang; Shunqing, Wu; Zizhong, Zhu

    2016-04-01

    The electronic band structures and band gap bowing parameters of In x Ga1-x N are studied by the first-principles method based on the density functional theory. Calculations by employing both the Heyd-Scuseria-Ernzerh of hybrid functional (HSE06) and the Perdew-Burke-Ernzerhof (PBE) one are performed. We found that the theoretical band gap bowing parameter is dependent significantly on the calculation method, especially on the exchange-correlation functional employed in the DFT calculations. The band gap of In x Ga1-x N alloy decreases considerably when the In constituent x increases. It is the interactions of s-s and p-p orbitals between anions and cations that play significant roles in formatting the band gaps bowing. In general, the HSE06 hybrid functional could provide a good alternative to the PBE functional in calculating the band gap bowing parameters. Project supported by the National Natural Science Foundation of China (Nos. 11204257, 21233004) and the China Postdoctoral Science Foundation (No. 2012M511447).

  10. "Heaven Starts at Your Parents' Feet": Adolescent Bowing to Parents and Associated Spiritual Attitudes

    ERIC Educational Resources Information Center

    Thanissaro, Phra Nicholas

    2010-01-01

    In a quantitative survey of religious attitudes and practices in a multi-religious sample of 369 school pupils aged between 13 and 15 in London, the practice of bowing to parents was found widespread in 22% of adolescents spanning several religious affiliations and ethnicities--especially Buddhists, Hindus and those of Indian, African and…

  11. Modeling and numerical investigation of the inlet circumferential fluctuations of swept and bowed blades

    NASA Astrophysics Data System (ADS)

    Tang, Mingzhi; Jin, Donghai; Gui, Xingmin

    2017-02-01

    The circumferential fluctuation (CF) source terms induced by the inviscid blade force can affect the inlet distribution of flow parameters and radial equilibrium of swept and bowed blades. However, these phenomena cannot be adequately described by throughflow methods based on the axisymmetric assumption. A transport model for the CF stresses is proposed and correlated to the distribution of circulation to reflect the effect of the inviscid blade force. To investigate the effect of the inlet CFs on swept and bowed blades, the model is integrated into a throughflow model and applied to a series of cascades with different sweep and bow angles. For swept cascades, the CF source terms change the distributions of incidence angles, as well as the radial equilibrium at the inlet of the blade passage. And the influence is enhanced as the absolute value of the sweep angle increases. For bowed cascades, the distributions of incidence angles are also altered. For both cases, the model can offer a good prediction of the inlet CF source terms, and prove to exert a better prediction of blade design key parameters such as flow angles.

  12. "Heaven Starts at Your Parents' Feet": Adolescent Bowing to Parents and Associated Spiritual Attitudes

    ERIC Educational Resources Information Center

    Thanissaro, Phra Nicholas

    2010-01-01

    In a quantitative survey of religious attitudes and practices in a multi-religious sample of 369 school pupils aged between 13 and 15 in London, the practice of bowing to parents was found widespread in 22% of adolescents spanning several religious affiliations and ethnicities--especially Buddhists, Hindus and those of Indian, African and…

  13. Transient bowing of core assemblies in advanced liquid metal fast reactors

    SciTech Connect

    Kamal, S.A.; Orechwa, Y.

    1986-01-01

    Two alternative core restraint concepts are considered for a conceptual design of a 900 MWth liquid metal fast reactor core with a heterogeneous layout. The two concepts, known as limited free bowing and free flowering, are evaluated based on core bowing criteria that emphasize the enhancement of inherent reactor safety. The core reactivity change during a postulated loss of flow transient is calculated in terms of the lateral displacements and displacement-reactivity-worths of the individual assemblies. The NUBOW-3D computer code is utilized to determine the assembly deformations and interassembly forces that arise when the assemblies are subjected to temperature gradients and irradiation induced creep and swelling during the reactor operation. The assembly ducts are made of the ferritic steel HT-9 and remain in the reactor core for four-years at full power condition. Whereas both restraint systems meet the bowing criteria, a properly designed limited free bowing system appears to be more advantageous than a free flowering system from the point of view of enhancing the reactor inherent safety.

  14. 77 FR 19661 - City of Broken Bow, OK; Notice of Technical Conference

    Federal Register 2010, 2011, 2012, 2013, 2014

    2012-04-02

    ... notice that a technical conference will be held to discuss the section 4(e) conditions filed by the U.S.... This conference will be held on Wednesday, April 25, 2012, beginning at 9:30 a.m. (CDT) at the U.S. Forest Service's Hochatown Office, Route 4, Broken Bow, OK 74728. All local, state, and federal agencies...

  15. 76 FR 65717 - City of Broken Bow, OK; Notice of Availability of Final Environmental Assessment

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-10-24

    ... Energy Regulatory Commission City of Broken Bow, OK; Notice of Availability of Final Environmental Assessment In accordance with the National Environmental Policy Act of 1969 and the Federal Energy Regulatory... Forest. Staff prepared a final environmental assessment (EA), which analyzes the potential environmental...

  16. 3D Bow Shock Modeling Based on Multi-spacecraft Observations and Support Vector Regression Machine

    NASA Astrophysics Data System (ADS)

    Merka, J.; Wang, Y.; Sibeck, D. G.

    2012-12-01

    Interaction of the supersonic solar wind with Earth's magnetosphere creates fast mode magnetosonic waves that travel back upstream, combine and steepen to form the bow shock wave. The bow shock wave has been studied for more than four decades but existing models are still often inaccurate. Previous studies established that bow shock shape and position are primarily controlled by solar wind pressure PSW , upstream Mach numbers, interplanetary magnetic field orientation and magnetopause shape and position. Our study employs the Support Vector Regression Machine (SVRM) technique for mapping multi-dimensional data into a high- dimensional feature space via nonlinear mapping through a selected kernel function and performing a linear regression in this space. The use of SVRM means that there is no apriori prescribed shock shape. In addition to SVRM, the bootstrap technique is employed for error calculations in contrast to existing shock models that rarely provide any error estimates at all. We fit a total of 28,287 bow shock crossings identified in observations from the Cluster 1-4, Geotail, IMP-8, Interball-1, MAGION-4, THEMIS A-E and WIND spacecraft.

  17. 3D Bow Shock Modeling Based on Multi-Spacecraft Observations and Support Vector Regression Machine

    NASA Astrophysics Data System (ADS)

    Merka, Jan; Wang, Yongli; Sibeck, David

    2012-07-01

    Interaction of the supersonic solar wind with Earth's magnetosphere creates fast mode magnetosonic waves that travel back upstream, combine and steepen to form the bow shock wave. The bow shock wave has been studied for more than four decades but existing models are still often inaccurate. Previous studies established that bow shock shape and position are primarily controlled by solar wind pressure P_{SW}, upstream Mach numbers, interplanetary magnetic field orientation and magnetopause shape and position. Our study employs the Support Vector Regression Machine (SVRM) technique for mapping multi-dimensional data into a high- dimensional feature space via nonlinear mapping through a selected kernel function and performing a linear regression in this space. The use of SVRM means that there is no apriori prescribed shock shape. In addition to SVRM, the bootstrap technique is employed for error calculations in contrast to existing shock models that rarely provide any error estimates at all. We fit a total of 28,287 bow shock crossings identified in observations from the Cluster 1-4, Geotail, IMP-8, Interball-1, MAGION-4, THEMIS A-E and WIND spacecraft.

  18. Designing and Implementing an Assay for the Detection of Rare and Divergent NRPS and PKS Clones in European, Antarctic and Cuban Soils.

    PubMed

    Amos, Gregory C A; Borsetto, Chiara; Laskaris, Paris; Krsek, Martin; Berry, Andrew E; Newsham, Kevin K; Calvo-Bado, Leo; Pearce, David A; Vallin, Carlos; Wellington, Elizabeth M H

    2015-01-01

    The ever increasing microbial resistome means there is an urgent need for new antibiotics. Metagenomics is an underexploited tool in the field of drug discovery. In this study we aimed to produce a new updated assay for the discovery of biosynthetic gene clusters encoding bioactive secondary metabolites. PCR assays targeting the polyketide synthases (PKS) and non-ribosomal peptide synthetases (NRPS) were developed. A range of European soils were tested for their biosynthetic potential using clone libraries developed from metagenomic DNA. Results revealed a surprising number of NRPS and PKS clones with similarity to rare Actinomycetes. Many of the clones tested were phylogenetically divergent suggesting they were fragments from novel NRPS and PKS gene clusters. Soils did not appear to cluster by location but did represent NRPS and PKS clones of diverse taxonomic origin. Fosmid libraries were constructed from Cuban and Antarctic soil samples; 17 fosmids were positive for NRPS domains suggesting a hit rate of less than 1 in 10 genomes. NRPS hits had low similarities to both rare Actinobacteria and Proteobacteria; they also clustered with known antibiotic producers suggesting they may encode for pathways producing novel bioactive compounds. In conclusion we designed an assay capable of detecting divergent NRPS and PKS gene clusters from the rare biosphere; when tested on soil samples results suggest the majority of NRPS and PKS pathways and hence bioactive metabolites are yet to be discovered.

  19. Designing and Implementing an Assay for the Detection of Rare and Divergent NRPS and PKS Clones in European, Antarctic and Cuban Soils

    PubMed Central

    Laskaris, Paris; Krsek, Martin; Berry, Andrew E.; Newsham, Kevin K.; Calvo-Bado, Leo; Pearce, David A.; Vallin, Carlos; Wellington, Elizabeth M. H.

    2015-01-01

    The ever increasing microbial resistome means there is an urgent need for new antibiotics. Metagenomics is an underexploited tool in the field of drug discovery. In this study we aimed to produce a new updated assay for the discovery of biosynthetic gene clusters encoding bioactive secondary metabolites. PCR assays targeting the polyketide synthases (PKS) and non-ribosomal peptide synthetases (NRPS) were developed. A range of European soils were tested for their biosynthetic potential using clone libraries developed from metagenomic DNA. Results revealed a surprising number of NRPS and PKS clones with similarity to rare Actinomycetes. Many of the clones tested were phylogenetically divergent suggesting they were fragments from novel NRPS and PKS gene clusters. Soils did not appear to cluster by location but did represent NRPS and PKS clones of diverse taxonomic origin. Fosmid libraries were constructed from Cuban and Antarctic soil samples; 17 fosmids were positive for NRPS domains suggesting a hit rate of less than 1 in 10 genomes. NRPS hits had low similarities to both rare Actinobacteria and Proteobacteria; they also clustered with known antibiotic producers suggesting they may encode for pathways producing novel bioactive compounds. In conclusion we designed an assay capable of detecting divergent NRPS and PKS gene clusters from the rare biosphere; when tested on soil samples results suggest the majority of NRPS and PKS pathways and hence bioactive metabolites are yet to be discovered. PMID:26398766

  20. Intra-strains diversity of expression of polymorphic PKS4 gene in comparison in zearalenone production by Fusarium graminearum during in vitro cultivation.

    PubMed

    Misiewicz, Anna; Goncerzewicz, Anna; Jędrzejczak, Renata; Zdziennicki, Filip

    2016-01-01

    Filamentous fungi belonging to the Fusarium genus are responsible for large economic losses due to their high pathogenicity and toxigenicity. Fusarium sp. may produce variety of mycotoxins, one of them is zearalenone (ZEA). The presence of the PKS4 gene shows the possibility of zearalenone biosynthesis by Fusarium sp. In this study, in four Fusarium graminearum and one Fusarium poae strains the presence of PKS4 genes and ZEA concentrations were determined. The presence of the PKS4 gene was confirmed by classical polymerase chain reaction (PCR) in three of four strains of F. graminearum. One strain with no PKS4 gene detected was found while still producing ZEA. In the present study, a real-time PCR assay has been successfully performed for the relative expression of Fusarium strains based on new designed primers targeting the PKS4 gene involved in ZEA biosynthesis. Result shows that P56/4 strain of F. graminearum has the highest mRNA level, in the range of 12, what correlates to the high production of this mycotoxin. In this study, a real-time PCR assay has been successfully developed for the prediction of the production of ZEA by F. graminearum strains by PCR real-time techniques based on primers targeting the gene, PKS4, involved in ZEA biosynthesis. The special significance was pointed to occurring genes polymorphism.

  1. Tracing Sources Of Nitrate And Sulfate In The Bow River, Alberta Canada, Using Isotope Techniques

    NASA Astrophysics Data System (ADS)

    Chao, J.; Mayer, B.; Ryan, C.

    2009-05-01

    The Bow River in Alberta is a major tributary to the South Saskatchewan River in western Canada. Urban development and agricultural activities including feedlot operations within the Bow River Basin can potentially impact the river water quality by elevating nitrate and sulfate concentrations. In this project, we applied hydrological, chemical and isotopic techniques to identify sources of nitrate and sulfate in the Bow River. The study area stretches approximately 570km along the Bow River from Lake Louise in the Rocky Mountain headwaters to near its confluence with the Oldman River in the prairies. Between June 2007 and July 2008, monthly samples were taken from the Bow River for major ion chemistry and stable isotope ratio measurements of H, O, C, N and S. Flow data from Alberta Environment were used in combination with chemical data to estimate fluxes of nitrate, sulfate and other ionic solutes along the river. Isotope results show that Bow River water near Lake Louise was characterized by δ15N-NO3 values between 0 and +4‰ and δ18O-NO3 values between +7 and +11‰ falling within the range typical for nitrate produced by nitrification in forest ecosystems. Between Canmore and Calgary, δ15N- NO3 increased to values between +3 and +8‰, and δ18O-NO3 ranged between -5 and +5‰. Nitrate discharged from the Bonnybrook wastewater treatment plant in Calgary has elevated δ15N-NO3 values of +8‰ and low δ18O-NO3 values of -10‰. Nitrate flux increased over an order of magnitude in the river as a result of wastewater effluent discharge at Calgary. In the agricultural irrigation districts downstream of Calgary, δ15N-NO3 values varied between +6 and +11‰, whereas δ18O-NO3 values ranged between -11 and +1‰. The elevated δ15N-NO3 and low δ18O-NO3 values indicate that sewage derived nitrate from the wastewater treatment plant is the major cause for increased nitrate fluxes in the Bow River downstream of Calgary. At Lake Louise, δ34S-SO4 values varied

  2. Mach 5 bow shock control by a nanosecond pulse surface dielectric barrier discharge

    NASA Astrophysics Data System (ADS)

    Nishihara, M.; Takashima, K.; Rich, J. W.; Adamovich, I. V.

    2011-06-01

    Bow shock perturbations in a Mach 5 air flow, produced by low-temperature, nanosecond pulse, and surface dielectric barrier discharge (DBD), are detected by phase-locked schlieren imaging. A diffuse nanosecond pulse discharge is generated in a DBD plasma actuator on a surface of a cylinder model placed in air flow in a small scale blow-down supersonic wind tunnel. Discharge energy coupled to the actuator is 7.3-7.8 mJ/pulse. Plasma temperature inferred from nitrogen emission spectra is a few tens of degrees higher than flow stagnation temperature, T = 340 ± 30 K. Phase-locked Schlieren images are used to detect compression waves generated by individual nanosecond discharge pulses near the actuator surface. The compression wave propagates upstream toward the baseline bow shock standing in front of the cylinder model. Interaction of the compression wave and the bow shock causes its displacement in the upstream direction, increasing shock stand-off distance by up to 25%. The compression wave speed behind the bow shock and the perturbed bow shock velocity are inferred from the Schlieren images. The effect of compression waves generated by nanosecond discharge pulses on shock stand-off distance is demonstrated in a single-pulse regime (at pulse repetition rates of a few hundred Hz) and in a quasi-continuous mode (using a two-pulse sequence at a pulse repetition rate of 100 kHz). The results demonstrate feasibility of hypersonic flow control by low-temperature, repetitive nanosecond pulse discharges.

  3. BowMapCL: Burrows-Wheeler Mapping on Multiple Heterogeneous Accelerators.

    PubMed

    Nogueira, David; Tomas, Pedro; Roma, Nuno

    2016-01-01

    The computational demand of exact-search procedures has pressed the exploitation of parallel processing accelerators to reduce the execution time of many applications. However, this often imposes strict restrictions in terms of the problem size and implementation efforts, mainly due to their possibly distinct architectures. To circumvent this limitation, a new exact-search alignment tool (BowMapCL) based on the Burrows-Wheeler Transform and FM-Index is presented. Contrasting to other alternatives, BowMapCL is based on a unified implementation using OpenCL, allowing the exploitation of multiple and possibly different devices (e.g., NVIDIA, AMD/ATI, and Intel GPUs/APUs). Furthermore, to efficiently exploit such heterogeneous architectures, BowMapCL incorporates several techniques to promote its performance and scalability, including multiple buffering, work-queue task-distribution, and dynamic load-balancing, together with index partitioning, bit-encoding, and sampling. When compared with state-of-the-art tools, the attained results showed that BowMapCL (using a single GPU) is 2 × to 7.5 × faster than mainstream multi-threaded CPU BWT-based aligners, like Bowtie, BWA, and SOAP2; and up to 4 × faster than the best performing state-of-the-art GPU implementations (namely, SOAP3 and HPG-BWT). When multiple and completely distinct devices are considered, BowMapCL efficiently scales the offered throughput, ensuring a convenient load-balance of the involved processing in the several distinct devices.

  4. CPR methodology with new steady-state criterion and more accurate statistical treatment of channel bow

    SciTech Connect

    Baumgartner, S.; Bieli, R.; Bergmann, U. C.

    2012-07-01

    An overview is given of existing CPR design criteria and the methods used in BWR reload analysis to evaluate the impact of channel bow on CPR margins. Potential weaknesses in today's methodologies are discussed. Westinghouse in collaboration with KKL and Axpo - operator and owner of the Leibstadt NPP - has developed an optimized CPR methodology based on a new criterion to protect against dryout during normal operation and with a more rigorous treatment of channel bow. The new steady-state criterion is expressed in terms of an upper limit of 0.01 for the dryout failure probability per year. This is considered a meaningful and appropriate criterion that can be directly related to the probabilistic criteria set-up for the analyses of Anticipated Operation Occurrences (AOOs) and accidents. In the Monte Carlo approach a statistical modeling of channel bow and an accurate evaluation of CPR response functions allow the associated CPR penalties to be included directly in the plant SLMCPR and OLMCPR in a best-estimate manner. In this way, the treatment of channel bow is equivalent to all other uncertainties affecting CPR. Emphasis is put on quantifying the statistical distribution of channel bow throughout the core using measurement data. The optimized CPR methodology has been implemented in the Westinghouse Monte Carlo code, McSLAP. The methodology improves the quality of dryout safety assessments by supplying more valuable information and better control of conservatisms in establishing operational limits for CPR. The methodology is demonstrated with application examples from the introduction at KKL. (authors)

  5. THEMIS satellite observations of hot flow anomalies at Earth's bow shock

    NASA Astrophysics Data System (ADS)

    Chu, Christina; Zhang, Hui; Sibeck, David; Otto, Antonius; Zong, QiuGang; Omidi, Nick; McFadden, James P.; Fruehauff, Dennis; Angelopoulos, Vassilis

    2017-03-01

    Hot flow anomalies (HFAs) at Earth's bow shock were identified in Time History of Events and Macroscale Interactions During Substorms (THEMIS) satellite data from 2007 to 2009. The events were classified as young or mature and also as regular or spontaneous hot flow anomalies (SHFAs). The dataset has 17 young SHFAs, 49 mature SHFAs, 15 young HFAs, and 55 mature HFAs. They span a wide range of magnetic local times (MLTs) from approximately 7 to 16.5 MLT. The largest ratio of solar wind to HFA core density occurred near dusk and at larger distances from the bow shock. In this study, HFAs and SHFAs were observed up to 6.3 RE and 6.1 RE (Earth radii), respectively, upstream from the model bow shock. HFA-SHFA occurrence decreases with distance upstream from the bow shock. HFAs of the highest event core ion temperatures were not seen at the flanks. The ratio of HFA ion temperature increase to HFA electron temperature increase is highest around 12 MLT and slightly duskward. For SHFAs, (Tihfa/Tisw)/(Tehfa/Tesw) generally increased with distance from the bow shock. Both mature and young HFAs are more prevalent when there is an approximately radial interplanetary magnetic field. HFAs occur most preferentially for solar wind speeds from 550 to 600 km s-1. The correlation coefficient between the HFA increase in thermal energy density from solar wind values and the decrease in kinetic energy density from solar wind values is 0.62. SHFAs and HFAs do not show major differences in this study.

  6. X-RAY EMISSION LINE PROFILES FROM WIND CLUMP BOW SHOCKS IN MASSIVE STARS

    SciTech Connect

    Ignace, R.; Waldron, W. L.; Cassinelli, J. P.; Burke, A. E. E-mail: wwaldron@satx.rr.com E-mail: burke.alexander@gmail.com

    2012-05-01

    The consequences of structured flows continue to be a pressing topic in relating spectral data to physical processes occurring in massive star winds. In a preceding paper, our group reported on hydrodynamic simulations of hypersonic flow past a rigid spherical clump to explore the structure of bow shocks that can form around wind clumps. Here we report on profiles of emission lines that arise from such bow shock morphologies. To compute emission line profiles, we adopt a two-component flow structure of wind and clumps using two 'beta' velocity laws. While individual bow shocks tend to generate double-horned emission line profiles, a group of bow shocks can lead to line profiles with a range of shapes with blueshifted peak emission that depends on the degree of X-ray photoabsorption by the interclump wind medium, the number of clump structures in the flow, and the radial distribution of the clumps. Using the two beta law prescription, the theoretical emission measure and temperature distribution throughout the wind can be derived. The emission measure tends to be power law, and the temperature distribution is broad in terms of wind velocity. Although restricted to the case of adiabatic cooling, our models highlight the influence of bow shock effects for hot plasma temperature and emission measure distributions in stellar winds and their impact on X-ray line profile shapes. Previous models have focused on geometrical considerations of the clumps and their distribution in the wind. Our results represent the first time that the temperature distribution of wind clump structures are explicitly and self-consistently accounted for in modeling X-ray line profile shapes for massive stars.

  7. Mach 5 bow shock control by a nanosecond pulse surface dielectric barrier discharge

    SciTech Connect

    Nishihara, M.; Takashima, K.; Rich, J. W.; Adamovich, I. V.

    2011-06-15

    Bow shock perturbations in a Mach 5 air flow, produced by low-temperature, nanosecond pulse, and surface dielectric barrier discharge (DBD), are detected by phase-locked schlieren imaging. A diffuse nanosecond pulse discharge is generated in a DBD plasma actuator on a surface of a cylinder model placed in air flow in a small scale blow-down supersonic wind tunnel. Discharge energy coupled to the actuator is 7.3-7.8 mJ/pulse. Plasma temperature inferred from nitrogen emission spectra is a few tens of degrees higher than flow stagnation temperature, T = 340 {+-} 30 K. Phase-locked Schlieren images are used to detect compression waves generated by individual nanosecond discharge pulses near the actuator surface. The compression wave propagates upstream toward the baseline bow shock standing in front of the cylinder model. Interaction of the compression wave and the bow shock causes its displacement in the upstream direction, increasing shock stand-off distance by up to 25%. The compression wave speed behind the bow shock and the perturbed bow shock velocity are inferred from the Schlieren images. The effect of compression waves generated by nanosecond discharge pulses on shock stand-off distance is demonstrated in a single-pulse regime (at pulse repetition rates of a few hundred Hz) and in a quasi-continuous mode (using a two-pulse sequence at a pulse repetition rate of 100 kHz). The results demonstrate feasibility of hypersonic flow control by low-temperature, repetitive nanosecond pulse discharges.

  8. Multi-wavelength observations of PKS 2142-75 during active and quiescent gamma-ray states

    DOE PAGES

    Dutka, Michael S.; Ojha, Roopesh; Pottschmidt, Katja; ...

    2013-12-04

    Here, PKS 2142–75 (a.k.a. 2FGL J2147.4–7534) is a flat-spectrum radio quasar that was observed quasi-simultaneously by a suite of instruments across the electromagnetic spectrum during two flaring states in 2010 April and 2011 August as well as a quiescent state from 2011 December through 2012 January. The results of these campaigns and model spectral energy distributions (SEDs) from the active and quiescent states are presented. The SED model parameters of PKS 2142–75 indicate that the two flares of the source are created by unique physical conditions. SED studies of flat-spectrum radio quasars are beginning to indicate that there might bemore » two types of flares, those that can be described purely by changes in the electron distribution and those that require changes in other parameters, such as the magnetic field strength or the size of the emitting region.« less

  9. Twenty-Year Optical Variability and Correlated Optical - Radio Outbursts of the Blazar PKS 1749+096

    NASA Astrophysics Data System (ADS)

    Balonek, Thomas J.; Patrick, P.; Hegel, P.; Taber, T.; Gurwell, M. A.

    2010-01-01

    We present the twenty-year optical variability light curve for the BL Lac type quasar PKS 1749+096 and investigate the characteristic timescales of variations. Observations were obtained as part of the intensive blazar variability monitoring program at the Colgate University Foggy Bottom Observatory (FBO). PKS 1749+096 underwent strong optical outbursts (R 13.8) during the summers of 2007 and 2008, reaching its brightest optical level in three decades, and exhibited an inactive period during summer 2009. Comparison of SMA millimeter wavelength radio observations with the optical light curve, using DCF and ACF analysis, indicates the radio variations may be correlated with the optical outbursts. We gratefully acknowledge support for student research through an REU grant to the Keck Northeast Astronomy Consortium from the National Science Foundation, the NASA / New York Space Grant, and the Schlichting Student Research Fund at Colgate University.

  10. Multi-wavelength observations of PKS 2142-75 during active and quiescent gamma-ray states

    SciTech Connect

    Dutka, Michael S.; Ojha, Roopesh; Pottschmidt, Katja; Finke, Justin D.; Stevens, Jamie; Edwards, Philip G.; Blanchard, Jay; Lovell, James E. J.; Nesci, Roberto; Wilms, Joern; Tosti, Gino; Pursimo, Tapio; Krauss, Felicia; Müller, Cornelia; Gehrels, Neil

    2013-12-04

    Here, PKS 2142–75 (a.k.a. 2FGL J2147.4–7534) is a flat-spectrum radio quasar that was observed quasi-simultaneously by a suite of instruments across the electromagnetic spectrum during two flaring states in 2010 April and 2011 August as well as a quiescent state from 2011 December through 2012 January. The results of these campaigns and model spectral energy distributions (SEDs) from the active and quiescent states are presented. The SED model parameters of PKS 2142–75 indicate that the two flares of the source are created by unique physical conditions. SED studies of flat-spectrum radio quasars are beginning to indicate that there might be two types of flares, those that can be described purely by changes in the electron distribution and those that require changes in other parameters, such as the magnetic field strength or the size of the emitting region.

  11. Multi-wavelength observations of PKS 2142–75 during active and quiescent gamma-ray states

    SciTech Connect

    Dutka, Michael S.; Ojha, Roopesh; Finke, Justin D.; Stevens, Jamie; Edwards, Philip G.; Blanchard, Jay; Lovell, James E. J.; Nesci, Roberto; Wilms, Joern; Krauss, Felicia; Tosti, Gino; Pursimo, Tapio; Gehrels, Neil

    2013-12-20

    PKS 2142–75 (a.k.a. 2FGL J2147.4–7534) is a flat-spectrum radio quasar that was observed quasi-simultaneously by a suite of instruments across the electromagnetic spectrum during two flaring states in 2010 April and 2011 August as well as a quiescent state from 2011 December through 2012 January. The results of these campaigns and model spectral energy distributions (SEDs) from the active and quiescent states are presented. The SED model parameters of PKS 2142–75 indicate that the two flares of the source are created by unique physical conditions. SED studies of flat-spectrum radio quasars are beginning to indicate that there might be two types of flares, those that can be described purely by changes in the electron distribution and those that require changes in other parameters, such as the magnetic field strength or the size of the emitting region.

  12. The bursting behavior of the blazar PKS 1130+009 from K2 and ground based photometry

    NASA Astrophysics Data System (ADS)

    Carini, Michael T.; Brown, Rebecca; Yik, Henry

    2017-01-01

    PKS 1130+009 (EPIC 201510350) is a z=1.64 blazar, observed as part of our continuing observations of WiBRAL blazars with the K2 mission. During the K2 observations, PKS 1130+009 exhibited repeated outbursts of up to 50% in flux, with one larger, rapid outburst well in excess of 100% flux variation detected. The outbursts were semi-regular, but did not occur with any rigorous periodicity. Ground based optical R band observations were obtained with the 1.3 Robotically Controlled Telescope at KPNO to determine if this behavior is episodic and restricted to the time of the K2 observations, or if this behavior is typical of this source. The slope and nature of the source power spectral density are discussed.

  13. Experimental investigation of the effect of bow profiles on resistance of an underwater vehicle in free surface motion

    NASA Astrophysics Data System (ADS)

    Javadi, Mehran; Manshadi, Mojtaba Dehghan; Kheradmand, Saeid; Moonesun, Mohammad

    2015-03-01

    In this paper, towing tank experiments are conducted to study the behavior of flow on a model of the underwater vehicle with various shapes of bows, i.e. tango and standard bows in free surface motion tests. The total resistances for different Froude numbers are considered experimentally. The towing tank is equipped with a trolley that can operate in through 0.05-6 m/s speed with ±0.02 m/s accuracy. Furthermore, the study is done on hydrodynamic coefficients i.e. total, residual and friction resistance coefficients, and the results are compared. Finally, the study on flow of wave fields around bows is done and wave filed around two bows are compared. The Froude number interval is between 0.099 and 0.349. Blockage fraction for the model is fixed to 0.005 3. The results showed that the residual resistance of the standard bow in 0.19 to 0.3 Froude number is more than the tango bow in surface motion which causes more total resistance for the submarine. Finally, details of wave generated by the bow are depicted and the effects of flow pattern on resistance drag are discussed.

  14. Extremely high cm-band radio flux level of the gamma-ray flaring FSRQ PKS 1510-089

    NASA Astrophysics Data System (ADS)

    Orienti, M.; D'Ammando, F.; Giroletti, M.; Orlati, A.

    2011-11-01

    The 32-m single dish antenna located at Medicina has been observing the flat spectrum radio quasar PKS 1510-089 starting from July 2011 with monthly frequency. The observations were organised as a follow-up of the gamma-ray flaring event reported in July 2011 by AGILE (ATel #3470) and Fermi (ATel #3473). Recently, radio observations were performed at 4.9 GHz and 8.0 GHz on 2011 November 16.

  15. Fermi LAT detection of a GeV flare from blazar NRAO 190 (PKS 0440-00)

    NASA Astrophysics Data System (ADS)

    Buson, S.; Gasparrini, D.

    2013-06-01

    The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, observed a gamma-ray outburst from a source positionally consistent with the flat spectrum radio quasar NRAO 190 (also known as PKS 0440-00, DA 145, OF -067; RA: 04h 42m 38.661s, Dec: -00d 17m 43.42s, J2000.0) with redshift 0.844 (Hewitt & Burbidge 1987, 63, 1).

  16. Fermi LAT detection of renewed GeV activity from the high redshift blazar PKS 0458-02

    NASA Astrophysics Data System (ADS)

    Ciprini, Stefano; Fermi Large Area Telescope Collaboration

    2015-08-01

    The Large Area Telescope (LAT), one of two instruments on the Fermi Gamma-ray Space Telescope, has observed flaring gamma rays from a source positionally consistent with the flat spectrum radio quasar PKS 0458-02 (also known as S3 0458-02, DA 157, OA 141, and 3FGL J0501.2-0157), with radio coordinates, (J2000), R.A.: 75.303374 deg, Dec.: -1.987293 deg (Johnston et al.

  17. Fermi LAT detection of a GeV flare from High-redshift Blazar PKS 0537-286

    NASA Astrophysics Data System (ADS)

    Cheung, C. C.

    2017-05-01

    The Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope, has observed a gamma-ray flare from a source positionally consistent with the flat spectrum radio quasar PKS 0537-286 (RA = 84.9761725 deg, Decl.= -28.6655406 deg, J2000; Johnston et al. 1995 AJ 110, 880), at high-redshift, z=3.104 (Osmer et al. 1994 ApJ 436, 678).

  18. Swift detection of increased X-ray activity from gamma-ray flaring blazar PKS 1424-41

    NASA Astrophysics Data System (ADS)

    Ciprini, Stefano; Cutini, Sara

    2013-01-01

    Following enduring gamma-ray flaring activity of the flat spectrum radio quasar PKS 1424-41 (also known as 2FGL J1428.0-4206, Nolan et al. 2012, ApJS, 199, 31) detected by Fermi LAT during January 2013, two Swift target of opportunity observations were performed on January 24 and 27, 2013. Recent gamma-ray and X-ray flaring activity from the source was observed on January 6 and January 7 (ATel#4714 and ATel #4717).

  19. Polarization signatures of bow shocks: A diagnostic tool to constrain the properties of stellar winds and ISM

    NASA Astrophysics Data System (ADS)

    Shrestha, Manisha; Hoffman, Jennifer L.; Nielson, Hilding R.; Ignace, Richard

    2017-01-01

    When a stellar wind traveling at supersonic speed interacts with almost stationary ISM, a bow shock shape is formed. By studying a bow shock, we can obtain information about the properties of the stellar wind as well as the surrounding ISM. Bow shocks are asymmetric structures, and thus produce net polarization even if they are unresolved. Hence, polarization studies of bow shocks can provide complementary constraints on their properties.We simulate the polarization signatures of circumstellar material with bow shock geometries using a Monte Carlo radiative transfer code called SLIP. We use the analytic solution from Wilkin (1996) to define the geometry and mass surface density of the bow shock in our models. We present results from our simulations showing how changing CSM optical depth, CSM albedo, photon source, and scattering particles (electrons or different types of dust particles) affects the observed polarization in both resolved and unresolved cases. In the optically thin regime of the unresolved electron-scattering case, the polarization peaks at an inclination angle of 90°, in agreement with analytical single-scattering models. In optically thick cases, a second polarization peak appears near 130°, which we propose is due to multiple scattering. Given these results, an observed polarization value can constrain the inclination of an unresolved bow shock to two possible angles, which in turn constrain the motion of the star. In case of resolved bow shocks, our simulations produce polarization maps which we compare with observations.We also present results from our dust-scattering simulations, which show that multicolor broadband polarization observations can constrain the characteristics of the dust in a resolved or unresolved bow shock-shaped CSM configuration.

  20. Crystallization and preliminary X-ray diffraction studies of polyketide synthase-1 (PKS-1) from Cannabis sativa

    SciTech Connect

    Taguchi, Chiho; Taura, Futoshi; Tamada, Taro; Shoyama, Yoshinari; Shoyama, Yukihiro; Tanaka, Hiroyuki; Kuroki, Ryota; Morimoto, Satoshi

    2008-03-01

    Polyketide synthase-1 from C. sativa has been crystallized. The crystal diffracted to 1.55 Å resolution with sufficient quality for further structure determination. Polyketide synthase-1 (PKS-1) is a novel type III polyketide synthase that catalyzes the biosynthesis of hexanoyl triacetic acid lactone in Cannabis sativa (Mexican strain). PKS-1 was overproduced in Escherichia coli, purified and finally crystallized in two different space groups. The crystal obtained in 0.1 M HEPES buffer pH 7.5 containing 0.2 M calcium acetate and 20%(w/v) polyethylene glycol 3350 diffracted to 1.65 Å resolution and belonged to space group P1, with unit-cell parameters a = 54.3, b = 59.3, c = 62.6 Å, α = 69, β = 81, γ = 80°. Another crystal obtained in 0.1 M HEPES buffer pH 7.5 containing 0.2 M sodium chloride and 20%(w/v) polyethylene glycol 3350 diffracted to 1.55 Å resolution and belonged to space group P2{sub 1}2{sub 1}2{sub 1}, with unit-cell parameters a = 54.3, b = 110, c = 130 Å. These data will enable us to determine the crystal structure of PKS-1.

  1. Involvement of the cell-specific pigment genes pks and sult in bacterial defense response of sea urchins Strongylocentrotus intermedius.

    PubMed

    Kiselev, Konstantin V; Ageenko, Natalya V; Kurilenko, Valeria V

    2013-03-26

    Bacterial infections are one of the most important problems in mass aquaculture, causing the loss of millions of juvenile organisms. We isolated 22 bacterial strains from the cavity fluid of the sea urchin Strongylocentrotus pallidus and used phylogenetic analysis based on 16S rRNA gene sequences to separate the bacterial strains into 9 genera (Aliivibrio, Bizionia, Colwellia, Olleya, Paenibacillus, Photobacterium, Pseudoalteromonas, Shewanella, and Vibrio). Incubating Strongylocentrotus intermedius larvae with a strain from each of the 9 bacterial genera, we investigated the viability of the larvae, the amount of pigment cells, and the level of polyketide synthase (pks) and sulfotransferase (sult) gene expression. Results of the assay on sea urchin development showed that all bacterial strains, except Pseudoalteromonas and Bizionia, suppressed sea urchin development (resulting in retardation of the embryos' development with cellular disorders) and reduced cell viability. We found that pks expression in the sea urchin larvae after incubation with the bacteria of 9 tested genera was significantly increased, while the sult expression was increased only after the treatment with Pseudoalteromonas and Shewanella. Shikimic acid, which is known to activate the biosynthesis of naphthoquinone pigments, increased the tolerance of the sea urchin embryos to the bacteria. In conclusion, we show that the cell-specific pigment genes pks and sult are involved in the bacterial defense response of sea urchins.

  2. ON THE RADIO AND NEAR-INFRARED JET OF PKS 2155-304 AND ITS CLOSE ENVIRONMENT

    SciTech Connect

    Liuzzo, E.; Falomo, R.; Farinato, J.; Moretti, A.; Ragazzoni, R.; Treves, A.; Arcidiacono, C.; Diolaiti, E.; Lombini, M.; Torresi, E.; Donaldson, R.; Kolb, J.; Marchetti, E.; Tordo, S.

    2013-03-15

    PKS 2155-304 is one of the brightest BL Lac objects in the sky and a very well-studied target from radio to TeV bands. We report on high-resolution ({approx}0.''12) direct imaging of the field of PKS 2155-304 using adaptive optics near-IR (NIR) observations in the J and Ks bands obtained with the ESO Multi-Conjugate Adaptive Optics Demonstrator on the Very Large Telescope. These data are complemented with archival Very Large Array images at various frequencies to investigate the properties of the close environment of the source. We characterize the faint galaxies that form the poor group associated with the target. No radio emission is present for these galaxies, while an old radio jet at {approx}20 kpc from the nucleus of PKS 2155-304 and a jet-like structure of {approx}2 kpc ({approx}1'') in the eastern direction are revealed. No counterparts of these radio jets are found in the NIR or in archival Chandra observations.

  3. The X-ray luminous cluster underlying the z = 1.04 quasar PKS 1229-021

    NASA Astrophysics Data System (ADS)

    Russell, H. R.; Fabian, A. C.; Taylor, G. B.; Sanders, J. S.; Blundell, K. M.; Crawford, C. S.; Johnstone, R. M.; Belsole, E.

    2012-05-01

    We present a 100 ks Chandra observation studying the extended X-ray emission around the powerful z= 1.04 quasar PKS 1229-021. The diffuse cluster X-ray emission can be traced out to ˜15 arcsec (˜120 kpc) radius and there is a drop in the calculated hardness ratio inside the central 5 arcsec consistent with the presence of a cool core. Radio observations of the quasar show a strong core and a bright, one-sided jet leading to the south-west hotspot and a second hotspot visible on the counter-jet side. Although the wings of the quasar point spread function (PSF) provided a significant contribution to the total X-ray flux at all radii where the extended cluster emission was detected, we were able to accurately subtract the PSF emission using Chandra Ray Tracer and MARX simulations. The resulting steep cluster surface brightness profile for PKS 1229-021 appears similar to the profile for the FR II (Fanaroff-Riley class II) radio galaxy 3C 444, which has a similarly rapid surface brightness drop caused by a powerful shock surrounding the radio lobes. Using a model surface brightness profile based on 3C 444, we estimated the total cluster luminosity for PKS 1229-021 to be LX ~ 2 x 1044 erg/s. We discuss the difficulty of detecting cool-core clusters, which host bright X-ray sources, in high redshift surveys.

  4. Metagenomic Analysis of Upwelling-Affected Brazilian Coastal Seawater Reveals Sequence Domains of Type I PKS and Modular NRPS.

    PubMed

    Cuadrat, Rafael R C; Cury, Juliano C; Dávila, Alberto M R

    2015-11-27

    Marine environments harbor a wide range of microorganisms from the three domains of life. These microorganisms have great potential to enable discovery of new enzymes and bioactive compounds for industrial use. However, only ~1% of microorganisms from the environment can currently be identified through cultured isolates, limiting the discovery of new compounds. To overcome this limitation, a metagenomics approach has been widely adopted for biodiversity studies on samples from marine environments. In this study, we screened metagenomes in order to estimate the potential for new natural compound synthesis mediated by diversity in the Polyketide Synthase (PKS) and Nonribosomal Peptide Synthetase (NRPS) genes. The samples were collected from the Praia dos Anjos (Angel's Beach) surface water-Arraial do Cabo (Rio de Janeiro state, Brazil), an environment affected by upwelling. In order to evaluate the potential for screening natural products in Arraial do Cabo samples, we used KS (keto-synthase) and C (condensation) domains (from PKS and NRPS, respectively) to build Hidden Markov Models (HMM) models. From both samples, a total of 84 KS and 46 C novel domain sequences were obtained, showing the potential of this environment for the discovery of new genes of biotechnological interest. These domains were classified by phylogenetic analysis and this was the first study conducted to screen PKS and NRPS genes in an upwelling affected sample.

  5. THE ROLE OF PICKUP IONS ON THE STRUCTURE OF THE VENUSIAN BOW SHOCK AND ITS IMPLICATIONS FOR THE TERMINATION SHOCK

    SciTech Connect

    Lu Quanming; Shan Lican; Zhang Tielong; Wu Mingyu; Wang Shui; Zank, Gary P.; Yang Zhongwei; Du Aimin

    2013-08-20

    The recent crossing of the termination shock by Voyager 2 has demonstrated the important role of pickup ions (PUIs) in the physics of collisionless shocks. The Venus Express (VEX) spacecraft orbits Venus in a 24 hr elliptical orbit that crosses the bow shock twice a day. VEX provides a unique opportunity to investigate the role of PUIs on the structure of collisionless shocks more generally. Using VEX observations, we find that the strength of the Venusian bow shock is weaker when solar activity is strong. We demonstrate that this surprising anti-correlation is due to PUIs mediating the Venusian bow shock.

  6. VHE γ-ray emission of PKS 2155-304: spectral and temporal variability

    NASA Astrophysics Data System (ADS)

    H.E.S.S. Collaboration; Abramowski, A.; Acero, F.; Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Barres de Almeida, U.; Bazer-Bachi, A. R.; Becherini, Y. Behera, B.; Benbow, W.; Bernlöhr, K.; Bochow, A.; Boisson, C.; Bolmont, J.; Borrel, V.; Brucker, J.; Brun, F.; Brun, P.; Bühler, R.; Bulik, T.; Büsching, I.; Boutelier, T.; Chadwick, P. M.; Charbonnier, A.; Chaves, R. C. G.; Cheesebrough, A.; Chounet, L.-M.; Clapson, A. C.; Coignet, G.; Conrad, J.; Costamante, L.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; Dickinson, H. J.; Djannati-Ataï, A.; Domainko, W.; O'C. Drury, L.; Dubois, F.; Dubus, G.; Dyks, J.; Dyrda, M.; Egberts, K.; Eger, P.; Espigat, P.; Fallon, L.; Farnier, C.; Fegan, S.; Feinstein, F.; Fernandes, M. V.; Fiasson, A.; Förster, A.; Fontaine, G.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Gérard, L.; Gerbig, D.; Giebels, B.; Glicenstein, J. F.; Glück, B.; Goret, P.; Göring, D.; Hampf, D.; Hauser, M.; Heinz, S.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Hofverberg, P.; Holleran, M.; Hoppe, S.; Horns, D.; Jacholkowska, A.; de Jager, O. C.; Jahn, C.; Jung, I.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Kerschhaggl, M.; Khangulyan, D.; Khélifi, B.; Keogh, D.; Klochkov, D.; Kluźniak, W.; Kneiske, T.; Komin, Nu.; Kosack, K.; Kossakowski, R.; Lamanna, G.; Lenain, J.-P.; Lohse, T.; Lu, C.-C.; Marandon, V.; Marcowith, A.; Masbou, J.; Maurin, D.; McComb, T. J. L.; Medina, M. C.; Méhault, J.; Moderski, R.; Moulin, E.; Naumann-Godo, M.; de Naurois, M.; Nedbal, D.; Nekrassov, D.; Nguyen, N.; Nicholas, B.; Niemiec, J.; Nolan, S. J.; Ohm, S.; Olive, J.-F.; de Oña Wilhelmi, E.; Opitz, B.; Orford, K. J.; Ostrowski, M.; Panter, M.; Paz Arribas, M.; Pedaletti, G.; Pelletier, G.; Petrucci, P.-O.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raubenheimer, B. C.; Raue, M.; Rayner, S. M.; Reimer, O.; Renaud, M.; de los Reyes, R.; Rieger, F.; Ripken, J.; Rob, L.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Ryde, F.; Sahakian, V.; Santangelo, A.; Schlickeiser, R.; Schöck, F. M.; Schönwald, A.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Sushch, I.; Sikora, M.; Skilton, J. L.; Sol, H.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Superina, G.; Szostek, A.; Tam, P. H.; Tavernet, J.-P.; Terrier, R.; Tibolla, O.; Tluczykont, M.; Valerius, K.; van Eldik, C.; Vasileiadis, G.; Venter, C.; Venter, L.; Vialle, J. P.; Viana, A.; Vincent, P.; Vivier, M.; Völk, H. J.; Volpe, F.; Vorobiov, S.; Wagner, S. J.; Ward, M.; Zdziarski, A. A.; Zech, A.; Zechlin, H. S.

    2010-09-01

    Context. Observations of very high-energy γ-rays from blazars provide information about acceleration mechanisms occurring in their innermost regions. Studies of variability in these objects lead to a better understanding of the mechanisms in play. Aims: To investigate the spectral and temporal variability of VHE (>100 GeV) γ-rays of the well-known high-frequency-peaked BL Lac object PKS 2155-304 with the HESS imaging atmospheric Cherenkov telescopes over a wide range of flux states. Methods: Data collected from 2005 to 2007 were analyzed. Spectra were derived on time scales ranging from 3 years to 4 min. Light curve variability was studied through doubling timescales and structure functions and compared with red noise process simulations. Results: The source was found to be in a low state from 2005 to 2007, except for a set of exceptional flares that occurred in July 2006. The quiescent state of the source is characterized by an associated mean flux level of (4.32 ± 0.09stat ± 0.86syst) × 10-11 cm-2 s-1 above 200 GeV, or approximately 15% of the Crab Nebula, and a power-law photon index of Γ = 3.53 ± 0.06stat ± 0.10syst. During the flares of July 2006, doubling timescales of ~2 min are found. The spectral index variation is examined over two orders of magnitude in flux, yielding different behavior at low and high fluxes, which is a new phenomenon in VHE γ-ray emitting blazars. The variability amplitude characterized by the fractional rms Fvar is strongly energy-dependent and is ∝ E0.19±0.01. The light curve rms correlates with the flux. This is the signature of a multiplicative process that can be accounted for as a red noise with a Fourier index of ~2. Conclusions: This unique data set shows evidence of a low-level γ-ray emission state from PKS 2155-304 that possibly has a different origin than the outbursts. The discovery of the light curve lognormal behavior might be an indicator of the origin of aperiodic variability in blazars.

  7. Radio and X-ray observations of the gamma-ray bright quasar PKS 0528+134

    NASA Technical Reports Server (NTRS)

    Zhang, Yun Fei; Marscher, Alan P.; Aller, Hugh D.; Aller, Margo F.; Terasranta, Harri; Valtaoja, Esko

    1994-01-01

    We present a study of the z = 2.07 quasar PKS 0528+134, which has been detected as an extraordinarily luminous gamma-ray source. Its radio properties are highly variable in both total and polarized flux density. Milliarcsecond-scale maps from global very long base interferometry (VLBI) experiments, an X-ray spectrum from ROSAT Position Sensitive Proportional Counter (PSPC) observations, and light curves in total flux density and polarization are used to investigate the geometry, radiation mechanism, and physical environment of the emission region in the source. The VLBI images reveal a bent jet extending toward the northeast on parsec scales, with less intense knots of emission appearing on the opposite side of the brightest spot. The position of the core usually found in such sources is unclear. The polarization angle is stable despite strong variability in polarized flux density and indicates that the magnetic field is aligned with the jet axis as defined by our 8.4 GHz image. The ROSAT X-ray flux density of PKS 0528+134 in 1991 March is measured to be 1.6 micro Jy at 1 keV, with a very steep spectral (`energy') index sigma(sub x) approximately equal to 2.2. The X-ray observations reveal the presence of cold gas along the line of sight significantly in excess of that present in the Galaxy. A strong radio flare began within two months of the first observation of a high flux of gamma-rays from PKS 0528+134 by Hunter et al. Using the geometry and spectral chacateristics determined by our VLBI observations, a synchrotron self-Compton calculation indicates that relativistic bulk motion is required in PKS 0528+134, with an estimated Doppler beaming factor delta approximately greater than 4.3, similar to the value delta approximately greater than 7 required to explain the low optical depth of the gamma-rays to photon-photon pair production. We suggest that the core activity of PKS 0528+134 is sporadic in nature, with the nonthermal outburst starting in 1991 representing

  8. Attenuation Distance of Low Frequency Waves Upstream of the Pre-Dawn Bow Shock: GEOTAIL snd ISEE-3 Comparison

    NASA Technical Reports Server (NTRS)

    Sugiyama, T.; Terasawa, T.; Kawano, H.; Yamamoto, T.; Kokubun, S.; Frank, L.; Ackerson, K.; Tsurutani, B.

    1994-01-01

    This paper presents a statistical study of the spatial distribution of low frequency waves in the region upstream of the pre-dawn to dawn side bow shock using both GEOTAIL and ISEE-3 magnetometer data.

  9. Interstellar Broadening of Images in the Gravitational Lens Pks 1830-211

    NASA Technical Reports Server (NTRS)

    Jones, D. L.; Preston, R. A.; Murphy, D. W.; Jauncey, D. L.; Reynolds, J. E.; Tzioumis, A. K.; King, E. A.; McCulloch, P. M.; Lovell, J. E. J.; Costa, M. E.

    1996-01-01

    The remarkably strong radio gravitational lens PKS 1830-211 consists of a one arcsecond diameter Einstein ring with two bright compact (milliarcsecond) components located on opposite sides of the ring. We have obtained 22 GHz VLBA data on this source to determine the intrinsic angular sizes of the compact components. Previous VLBI observations at lower frequencies indicate that the brightness temperatures of these components are significantly lower than 10(exp 10) K (Jauncey, et al. 1991), less than is typical for compact synchrotron radio sources and less than is implied by the short timescales of flux density variations. A possible explanation is that interstellar scattering is broadening the apparent angular size of the source and thereby reducing the observed brightness temperature. Our VLBA data support this hypothesis. At 22 GHz the measured brightness temperature is at least 10(exp 11) K, and the deconvolved 2 size of the core in the southwest compact component is proportional to upsilon(sup -2) between 1.7 and 22 GHz. VLBI observations at still higher frequencies should be unaffected by interstellar scattering.

  10. The low-frequency radio emission in blazar PKS2155-304

    NASA Astrophysics Data System (ADS)

    Pandey-Pommier, M.; Sirothia, S.; Chadwick, P.; Martin, J.-M.; Colom, P.; van Driel, W.; Combes, F.; Kharb, P.; Crespeau, P.-J.; Richard, J.; Guiderdoni, B.

    2016-12-01

    We report radio imaging and monitoring observations in the frequency range 0.235 - 2.7 GHz during the flaring mode of PKS 2155-304, one of the brightest BL Lac objects. The high sensitivity GMRT observations not only reveal extended kpc-scale jet and FRI type lobe morphology in this erstwhile 'extended-core' blazar but also delineate the morphological details, thanks to its arcsec scale resolution. The radio light curve during the end phase of the outburst measured in 2008 shows high variability (8.5%) in the jet emission in the GHz range, compared to the lower core variability (3.2%) seen at the lowest frequencies. The excess of flux density with a very steep spectral index in the MHz range supports the presence of extra diffuse emission at low frequencies. The analysis of multi wavelength (radio/optical/gamma-ray) light curves at different radio frequencies confirms the variability of the core region and agrees with the scenario of high energy emission in gamma-rays due to inverse Compton emission from a collimated relativistic plasma jet followed by synchrotron emission in radio. Clearly, these results give an interesting insight of the jet emission mechanisms in blazars and highlight the importance of studying such objects with low frequency radio interferometers like LOFAR and the SKA and its precursor instruments.

  11. The Historic Optical Light Curve and 2007 Outburst of Quasar PKS 1749+096

    NASA Astrophysics Data System (ADS)

    Balonek, Thomas J.; Chromey, F. R.; Barker, T.; Levandowski, K.; Morin, A.; Shvonski, A.; Webb, C.; Scott, E.; Goldblatt, A.; Clements, S. D.; Aller, M. F.; Aller, H. D.; Gurwell, M. A.

    2007-12-01

    The BL Lac type quasar PKS 1749+096 underwent a strong optical outburst (R 13.8) during the summer of 2007. To study the intraday and longer timescale variations, and color index changes, during this outburst we initiated a collaborative observing program to obtain B, V, R and I filtered CCD images using telescopes at Colgate University Foggy Bottom Observatory (FBO), Vassar College Observatory, Grove Creek Observatory in Australia, and Wheaton College Observatory. These data, along with earlier observations from FBO and the Univ. of Florida photographic quasar monitoring program, reveal that during the 2007 outburst this blazar reached its brightest level in three decades. Comparison of centimeter and sub-millimeter wavelength radio observations with the optical light curve indicates radio variations may be correlated with the 2007 optical outburst. We gratefully acknowledge support for student research through an REU grant to the Keck Northeast Astronomy Consortium from the National Science Foundation and from the Vassar URSI (Undergraduate Research Summer Institute) program.

  12. PKS 2155-304 relativistically beamed synchrotron radiation from BL LAC object

    NASA Technical Reports Server (NTRS)

    Urry, C. M.; Mushotzky, R. F.

    1981-01-01

    The newly discovered BL Lacertae object, PKS 2155-304, was observed with the medium and high intensity energy detectors of the HEAO-1 A2 experiment. The variability by a factor of two in less than a day reported by Snyder, et al (1979) is confirmed. Two spectra, obtained a year apart, while the satellite was in scanning mode, are well fit by simple power laws with energy spectral index alpha sub 1 equals approximately 1.4. A third spectrum, of higher statistical quality, obtained while the satellite was pointed at its source, has has two components. An acceptable fit was obtained using a two power law model, with indices alpha sub 1 equals 2.0 (+1.2, -0.6) and alpha sub 2 equals -1.5 (+1.5, -2.3). An interpretation of the overall spectrum from radio through X-rays in terms of a synchrotron self-Compton model gives a good description of the data if allowance is made for relativistic beaming. Thus, from a consideration of the spectrum, combined with an estimate of the size of the source, the presence of jets is inferred without their observation.

  13. Multifrequency VLA observations of PKS 0745 - 191 - The archetypal 'cooling flow' radio source?

    NASA Technical Reports Server (NTRS)

    Baum, S. A.; O'Dea, C. P.

    1991-01-01

    Ninety-, 20-, 6- and 2-cm VLA observations of the high-radio-luminosity cooling-flow radio source PKS 0745 - 191 are presented. The radio source was found to have a core with a very steep spectrum (alpha is approximately -1.5) and diffuse emission with an even steeper spectrum (alpha is approximately -1.5 to -2.3) without clear indications of the jets, hotspots, or double lobes found in the other radio sources of comparable luminosity. It is inferred that the energy to power the radio source comes from the central engine, but the source's structure may be heavily influenced by the past history of the galaxy and the inflowing intracluster medium. It is shown that, while the radio source is energetically unimportant for the cluster as a whole, it is important on the scale of the cooling flow. The mere existence of cosmic rays and magnetic fields within a substantial fraction of the volume inside the cooling radius has important consequences for cooling-flow models.

  14. Tentative detection of warm intervening gas towards PKS 0548-322 with XMM-Newton

    NASA Astrophysics Data System (ADS)

    Barcons, X.; Paerels, F. B. S.; Carrera, F. J.; Ceballos, M. T.; Sako, M.

    2005-06-01

    We present the results of a long (~93 ks) XMM-Newton observation of the bright BL-Lac object PKS 0548-322 (z= 0.069). Our Reflection Grating Spectrometer (RGS) spectrum shows a single absorption feature at an observed wavelength λ= 23.33 +/- 0.01 Å, which we interpret as OVI Kα absorption at z= 0.058, i.e. ~3000 km s-1 from the background object. The observed equivalent width of the absorption line, ~30 mÅ, coupled with the lack of the corresponding absorption edge in the EPIC pn data, implies a column density of NOVI~ 2 × 1016 cm-2 and turbulence with a Doppler velocity parameter b > 100 km s-1. Within the limitations of our RGS spectrum, no OVII or OV Kα absorption are detected. Under the assumption of ionization equilibrium by both collisions and the extragalactic background, this is only marginally consistent if the gas temperature is ~2.5 × 105 K, with significantly lower or higher values being excluded by our limits on OV or OVII. If confirmed, this would be the first X-ray detection of a large amount of intervening warm absorbing gas through OVI absorption. The existence of such a high column density absorber, much stronger than any previously detected one in OVI, would place stringent constraints on the large-scale distribution of baryonic gas in the Universe.

  15. The z = 1.6748 C I Absorber Toward the QSO PKS 1756+237

    NASA Astrophysics Data System (ADS)

    Roth, Katherine C.; Bauer, James M.; Jim, Kevin T. C.

    We have detected C I ground-state absorption at zabs = 1.6748 toward the QSO PKS 1756+237 (zem = 1.725), making this only the fourth known C I QSO absorber. The absence of excited-state fine-structure C I lines is compatible with the redshifted Cosmic Microwave Background Radiation at an expected temperature of TCMBR (1+z) = 7.291 K (Mather et al. 1994, ApJ, 354, L37). We find a 2 σ upper-limit on the C I excitation temperature of Tex <= 7.73(+0.53, -0.46) K (Roth & Bauer 1999, ApJ, submitted). Our Keck HIRES spectra (8.3 km s-1 FWHM) obtained in May 1997 also reveal the existence of Ni II and Fe II lines with a sub-solar Ni/Fe abundance ratio, presumably indicative of dust. We have obtained deep, high resolution (0.3'' FWHM) images in H+K' with the UH 2.2m Tip-Tilt system of the QSO field in order to identify the system responsible for the zabs = 1.6748 absorption. We detect two faint candidate systems within 1.5'' and 3'' (≅ 15 and 30 kpc, Hcirc = 65) of the QSO.

  16. The Low-Power Nucleus of PKS 1246-410 in the Centaurus Cluster

    SciTech Connect

    Taylor, G.B.; Sanders, J.S.; Fabian, A.C.; Allen, S.W.; /KIPAC, Menlo Park

    2005-10-21

    We present Chandra, Very Large Array (VLA), and Very Long Baseline Array (VLBA) observations of the nucleus of NGC 4696, a giant elliptical in the Centaurus cluster of galaxies. Like M87 in the Virgo cluster, PKS 1246-410 in the Centaurus cluster is a nearby example of a radio galaxy in a dense cluster environment. In analyzing the new X-ray data we have found a compact X-ray feature coincident with the optical and radio core. While nuclear emission from the X-ray source is expected, its luminosity is low, < 10{sup 40} erg s{sup -1}. We estimate the Bondi accretion radius to be 30 pc and the accretion rate to be 0.01 M{sub {circle_dot}} y{sup -1} which under the canonical radiative efficiency of 10% would overproduce by 3.5 orders of magnitude the radiative luminosity. Much of this energy can be directed into the kinetic energy of the jet, which over time inflates the observed cavities seen in the thermal gas. The VLBA observations reveal a weak nucleus and a broad, one-sided jet extending over 25 parsecs in position angle -150 degrees. This jet is deflected on the kpc-scale to a more east-west orientation (position angle of -80 degrees).

  17. Further observations of the head-tail radio galaxy PKS 2247 + 11

    NASA Astrophysics Data System (ADS)

    Robertson, J. G.

    1981-01-01

    Observations of the head-tail radio galaxy PKS 2247+11, which is located in a poor Zwicky cluster, are presented. Maps of polarized emission at 5.0, 1.4, and 0.61 GHz are given, as well as further observations of total intensity. Rotation measures and projected magnetic field directions are derived. Thermal plasma densities are computed from the observed depolarization ratios. The radio-optical knot (Simkin and Ekers, 1979) is significantly polarized; the physical conditions inside this component are similar to those in the region of the tail near to the galaxy, consistent with the view that the knot is a component ejected almost in the direction of motion of the galaxy. The direction of the projected magnetic field in the near tail is perpendicular to the axis of the tail, in agreement with recent observations of jet sources, but in disagreement with the magneto- spheric model of tail sources. In the more distant, diffuse parts of the tail the magnetic field structure is more complex. The density and temperature of the intracluster medium are estimated: n ˜ 10-3 and T ˜ 2 10-7 K, with considerable uncertainty.

  18. Colour variation of the BL Lacertae object PKS 0537-441

    NASA Astrophysics Data System (ADS)

    Li, Xiaopan; Zhang, Li; Luo, Yuhui; Wang, Lisha; Zhou, Li

    2015-05-01

    We present the colour indices V - R of BL Lacertae object PKS 0537-441 on the basis of the photometric data monitored by the Rapid Eye Mounting (REM) telescope located at the ESO Cerro La Silla observatory (Chile). Nearly 700 quasi-simultaneous data groups were collected during the period from 2004 to 2010. Our colour analysis shows the existence of at least two variability mechanisms: one is the long-term chromatic mechanism in which the variation traces a 0.04 ± 0.01 slope in the V - R versus V plot, the other is the chromatic mechanism implying the spectral changes during the flares and on intraday time-scales. A general bluer-when-brighter trend is confirmed in both ascent and descent states during the flares and in the 2010 February flare interval, while a much stronger bluer-when-brighter chromatism is observed in both faint and bright states on intraday time-scales. The discrete correlation function analysis reveals the existence of a time-lag of 13^{+5.8}_{-1.2} d between colour indices and magnitudes during the period MJD 54404-54453, whereas no measurable time-lag during other periods is found. Our results suggest that geometric effects may be responsible for the long-term achromatic mechanism, while the intrinsic shock-in-jet mechanism may produce the chromatic variability during the flares and on intraday time-scales.

  19. Analysis of the PKS0637-752 X-Ray Jet System

    NASA Technical Reports Server (NTRS)

    Schwartz, D. A.; Marshall, H. L.; Lovell, J. E. J.; Piner, B. G.; Tingay, S. J.; Birkinshaw, M.; Chartas, G.; Elvis, M.; Feigelson, E. D.; Ghosh, K. K.; hide

    2000-01-01

    The X-ray jet emitted from the quasar PKS0637-752 is the largest and most luminous detected to date. It extends 10 arcsec west of the nucleus, and is coincident with GHz radio jet emission in this region. If the individual X-ray/optical/radio knots in this jet were detected as isolated objects, they might be classified as BL Lac objects or quasars. We present a detailed analysis of the Chandra observations of this system, including a search for an intra-cluster medium to confine the jet, and limits to X-ray emission from the eastern radio knot and past the bend of the radio jet to the northwest. The projection in the plane of the sky implies that the X-ray jet is an aligned extension of the pc-scale jet, for which VLBI/VSOP observations show super-luminal motion with an apparent velocity of 11c. In this case, the X-ray jet is of order 1 Mpc in length, and explaining the X-ray emission mechanism presents new challenges.

  20. Interstellar Broadening of Images in the Gravitational Lens Pks 1830-211

    NASA Technical Reports Server (NTRS)

    Jones, D. L.; Preston, R. A.; Murphy, D. W.; Jauncey, D. L.; Reynolds, J. E.; Tzioumis, A. K.; King, E. A.; McCulloch, P. M.; Lovell, J. E. J.; Costa, M. E.

    1996-01-01

    The remarkably strong radio gravitational lens PKS 1830-211 consists of a one arcsecond diameter Einstein ring with two bright compact (milliarcsecond) components located on opposite sides of the ring. We have obtained 22 GHz VLBA data on this source to determine the intrinsic angular sizes of the compact components. Previous VLBI observations at lower frequencies indicate that the brightness temperatures of these components are significantly lower than 10(exp 10) K (Jauncey, et al. 1991), less than is typical for compact synchrotron radio sources and less than is implied by the short timescales of flux density variations. A possible explanation is that interstellar scattering is broadening the apparent angular size of the source and thereby reducing the observed brightness temperature. Our VLBA data support this hypothesis. At 22 GHz the measured brightness temperature is at least 10(exp 11) K, and the deconvolved 2 size of the core in the southwest compact component is proportional to upsilon(sup -2) between 1.7 and 22 GHz. VLBI observations at still higher frequencies should be unaffected by interstellar scattering.