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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. 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.

  4. 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

  5. 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.

  6. 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.

  7. 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.

  8. 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.

  9. 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.

  10. 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.

  11. 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.

  12. 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.

  13. 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

  14. [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.

  15. 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.

  16. 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.

  17. 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.

  18. 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.

  19. 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.

  20. 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).

  1. 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.

  2. 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.

  3. 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.

  4. 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.

  5. 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.

  6. 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.

  7. 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.

  8. 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.

  9. 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

  10. 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

  11. 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.

  12. 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.

  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. 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)

  15. 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.

  16. 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.

  17. 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.

  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. 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.

  20. 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

  1. 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.

  2. 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

  3. 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.

  4. 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...

  5. 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...

  6. 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

  7. 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.

  8. 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.

  9. 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.

  10. 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

  11. 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.

  12. 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.

  13. 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.

  14. 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.

  15. 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).

  16. 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.

  17. 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.

  18. 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).

  19. 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.

  20. 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].

  1. 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.

  2. 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.

  3. 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.

  4. 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.

  5. 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.

  6. 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

  7. 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

  8. 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

  9. 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

  10. 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

  11. 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

  12. 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.

  13. 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

  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. 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...

  16. 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

  17. 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.

  18. 76 FR 12016 - MedBow-Routt Resource Advisory Committee

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-03-04

    ... meeting. SUMMARY: The MedBow-Routt Resource Advisory Committee will meet in Walden, Colorado. The... will be held at Parks Ranger District, 100 Main Street, Walden, Colorado. Written comments should...

  19. 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.

  20. 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.

  1. 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

  2. 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

  3. 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

  4. 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

  5. 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

  6. 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

  7. 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

  8. 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

  9. 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.

  10. 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...

  11. 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.

  12. 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.

  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. 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.

  15. 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.

  16. 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

  17. 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.

  18. 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.

  19. [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.

  20. 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.

  1. 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.

  2. 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

  3. 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.

  4. 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.

  5. 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.

  6. 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.

  7. 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...

  8. 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

  9. 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.

  10. 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.

  11. 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... bow or arrow described in subparagraph (1) or (2) of this paragraph; and (4) Any quiver suitable...

  12. 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.

  13. 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

  14. 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.

  15. 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

  16. 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

  17. 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.

  18. 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

  19. 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

  20. 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

  1. 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.

  2. 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.

  3. 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.

  4. 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

  5. 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

  6. 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

  7. 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…

  8. 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

  9. 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

  10. 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

  11. 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

  12. 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

  13. 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.

  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...

  15. 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.

  16. 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

  17. 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.

  18. 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

  19. 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

  20. 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

  1. 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

  2. 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.

  3. 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.

  4. 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.

  5. 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.

  6. 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.

  7. 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.

  8. 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.

  9. 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.

  10. 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.

  11. 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.

  12. 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.

  13. 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. ...

  14. 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).

  15. [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.

  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. 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

  18. 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. ...

  19. 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.

  20. 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.

  1. 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

  2. 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.

  3. 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.

  4. 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.

  5. 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.

  6. 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.

  7. 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

  8. 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.

  9. 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.

  10. 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.

  11. 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

  12. 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.

  13. 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.

  14. 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.

  15. 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.

  16. 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.

  17. 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.

  18. 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.

  19. 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.

  20. 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).

  1. 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).

  2. 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.

  3. 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.

  4. 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.

  5. 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.

  6. 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.

  7. 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.

  8. 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

  9. 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

  10. 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.

  11. 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.

  12. 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.

  13. 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.

  14. 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.

  15. 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.

  16. 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.

  17. 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.

  18. 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

  19. 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.

  20. 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.

  1. 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.

  2. 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.

  3. 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.

  4. 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.

  5. 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.

  6. 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.

  7. 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

  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. 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).

  10. 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

  11. 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.

  12. 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.

  13. 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.

  14. 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.

  15. 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.

  16. 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

  17. Multispacecraft observations of energetic ions upstream and downstream of the bow shock

    NASA Technical Reports Server (NTRS)

    Scholer, M.; Moebius, E.; Kistler, L. M.; Klecker, B.; Ipavich, F. M.

    1989-01-01

    Simultaneous measurements of energetic protons and alpha particles were obtained inside and outside of the magnetopause and upstream and downstream of the bow shock. In the magnetosheath, no gradient or streaming is found in the upstream direction. The present results are consistent with first-order Fermi acceleration at the bow shock and subsequent downstream convection, and exclude the possibility of a magnetospheric source for these particles.

  18. 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.

  19. Defense Modernization Plans Through the 2020s: Addressing the Bow Wave

    DTIC Science & Technology

    2016-04-30

    45 p.m. Chair: Andrew Hunter, Senior Fellow in the International Security Program, Director of Defense-Industrial Initiatives Group , Center for...and has appeared on CNBC, CNN, NPR, Al Jazeera English, and Fox News. He has been a guest lecturer for organizations and teaches a class on the...their peak years of funding requirements at roughly the same time in the 2020s, creating a modernization bow wave. Just as a large bow wave slows a ship

  20. 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.

  1. 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⊙.

  2. 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.

  3. 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.

  4. 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.

  5. 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.

  6. 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.

  7. 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.

  8. 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.

  9. 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.

  10. 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.

  11. 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.

  12. 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.

  13. 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.

  14. 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.

  15. 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.

  16. 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

  17. 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

  18. 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.

  19. 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.

  20. 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. ...

  1. 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.

  2. Identification of a hybrid PKS-NRPS required for the biosynthesis of NG-391 in Metarhizium anisopliae var. anisopliae

    Technology Transfer Automated Retrieval System (TEKTRAN)

    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...

  3. 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.

  4. 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.

  5. 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.

  6. 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.

  7. 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

  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. 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.

  10. 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

  11. 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

  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. 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.

  14. 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.

  15. 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.

  16. 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.

  17. 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.

  18. 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.

  19. 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.

  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. 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.

  2. 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).

  3. 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.

  4. 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.

  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. 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.

  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. 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.

  9. 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.

  10. 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

  11. 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.

  12. 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.

  13. 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

  14. Detection of extragalactic argonium, ArH+, toward PKS 1830-211

    NASA Astrophysics Data System (ADS)

    Müller, Holger S. P.; Muller, Sébastien; Schilke, Peter; Bergin, Edwin A.; Black, John H.; Gerin, Maryvonne; Lis, Dariusz C.; Neufeld, David A.; Suri, Sümeyye

    2015-10-01

    Context. Argonium has recently been detected as a ubiquitous molecule in our Galaxy. Model calculations indicate that its abundance peaks at molecular fractions in the range of 10-4 to 10-3 and that the observed column densities require high values of the cosmic ray ionization rate. Therefore, this molecular cation may serve as an excellent tracer of the very diffuse interstellar medium (ISM), as well as an indicator of the cosmic ray ionization rate. Aims: We attempted to detect ArH+ in extragalactic sources to evaluate its diagnostic power as a tracer of the almost purely atomic ISM in distant galaxies. Methods: We obtained ALMA observations of a foreground galaxy at z = 0.89 in the direction of the lensed blazar PKS 1830-211. Results: Two isotopologs of argonium, 36ArH+ and 38ArH+, were detected in absorption along two different lines of sight toward PKS 1830-211, known as the SW and NE images of the background blazar. The argonium absorption is clearly enhanced on the more diffuse line of sight (NE) compared to other molecular species. The isotopic ratio 36Ar/38Ar is 3.46 ± 0.16 toward the SW image, i.e., significantly lower than the solar value of 5.5. Conclusions: Our results demonstrate the suitability of argonium as a tracer of the almost purely atomic, diffuse ISM in high-redshift sources. The evolution of the isotopic ratio with redshift may help to constrain nucleosynthetic scenarios in the early Universe. Appendix A is available in electronic form at http://www.aanda.org

  15. 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.

  16. Studies with Cluster upstream and downstream of the bow shock: An experimenter's perspective

    NASA Technical Reports Server (NTRS)

    Moebius, E.

    1995-01-01

    Some open questions in the physics of bow shock formation, the evolution of the particle distributions from solar wind into the magnetosheath, and the acceleration of ions at the moment of the shock are summarized. A layout of the current situation is presented in view of recent theoretical developments and the new diagnostic tools provided by the Cluster mission. The transition of ions across the quasi-perpendicular bow shock and their downstream thermalization are discussed. The processes and spatial scales are found to be species dependent and are discussed for H(+), He(2+), and He(+). The theory of particle acceleration at quasi-parallel shocks are reviewed. It is shown how Cluster can study the time variable structures of the shock as predicted by hybrid simulation. It is emphasized that high time resolution measurement with simultaneous species separation is necessary for the study of the ion acceleration. Suggestions for the spacecraft separations at the bow shock are suggested.

  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. 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.

  19. 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.

  20. 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.

  1. 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.

  2. 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.

  3. 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.

  4. 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.

  5. 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.

  6. 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.

  7. 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

  8. 75 FR 74678 - Medicine Bow-Routt National Forests and Thunder Basin National Grassland; Colorado and Wyoming...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-12-01

    ... Forest Service Medicine Bow-Routt National Forests and Thunder Basin National Grassland; Colorado and Wyoming; Medicine Bow-Routt National Forests and Thunder Basin National Grassland Invasive Plant... National Grassland (MBRTB) will prepare an environmental impact statement (EIS) to continue control...

  9. 78 FR 65609 - Medicine Bow-Routt National Forests and Thunder Basin National Grassland; Wyoming; Thunder Basin...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2013-11-01

    ... Forest Service Medicine Bow-Routt National Forests and Thunder Basin National Grassland; Wyoming; Thunder Basin National Grassland Prairie Dog Amendment Environmental Impact Statement; Correction AGENCY: Forest... Ranger, Douglas Ranger District, Medicine Bow-Routt National Forests and Thunder Basin National...

  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. 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.

  12. 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

  13. 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.

  14. 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.

  15. 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.

  16. 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.

  17. 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).

  18. 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.

  19. 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.

  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. 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.

  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. 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

  4. 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).

  5. "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…

  6. 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.

  7. 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.

  8. 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.

  9. 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

  10. 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.

  11. 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.

  12. 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.

  13. 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.

  14. 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

  15. 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.

  16. 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.

  17. 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.

  18. 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)

  19. 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

  20. 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.

  1. 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.

  2. 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.

  3. 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).

  4. 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.

  5. 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.

  6. Multifrequency VLA observations of PKS 0745 - 191 - The archetypal 'cooling flow' radio source?

    NASA Astrophysics Data System (ADS)

    Baum, S. A.; O'Dea, C. P.

    1991-06-01

    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.

  7. 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.

  8. 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.

  9. 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.

  10. 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.

  11. 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.

  12. Ketide Synthase (KS) Domain Prediction and Analysis of Iterative Type II PKS Gene in Marine Sponge-Associated Actinobacteria Producing Biosurfactants and Antimicrobial Agents.

    PubMed

    Selvin, Joseph; Sathiyanarayanan, Ganesan; Lipton, Anuj N; Al-Dhabi, Naif Abdullah; Valan Arasu, Mariadhas; Kiran, George S

    2016-01-01

    The important biological macromolecules, such as lipopeptide and glycolipid biosurfactant producing marine actinobacteria were analyzed and their potential linkage between type II polyketide synthase (PKS) genes was explored. A unique feature of type II PKS genes is their high amino acid (AA) sequence homology and conserved gene organization. These enzymes mediate the biosynthesis of polyketide natural products with enormous structural complexity and chemical nature by combinatorial use of various domains. Therefore, deciphering the order of AA sequence encoded by PKS domains tailored the chemical structure of polyketide analogs still remains a great challenge. The present work deals with an in vitro and in silico analysis of PKS type II genes from five actinobacterial species to correlate KS domain architecture and structural features. Our present analysis reveals the unique protein domain organization of iterative type II PKS and KS domain of marine actinobacteria. The findings of this study would have implications in metabolic pathway reconstruction and design of semi-synthetic genomes to achieve rational design of novel natural products.

  13. The ultraviolet absorption spectrum of the quasar PKS 0405-12 and the local density of Lyman-alpha absorption systems

    NASA Technical Reports Server (NTRS)

    Bahcall, John N.; Jannuzi, Buell T.; Schneider, Donald P.; Hartig, George F.

    1993-01-01

    A sample of 32 absorption lines has been identified in the ultraviolet spectrum of the z = 0.57 quasar PKS 0405-12. Data cover the wavelength range 1190-3260 A. There are 10 extragalactic Ly-alpha absorption lines in the complete sample, all with observed equivalent widths greater than or equal to 0.40 A; three of the Ly-alpha lines have Ly-beta counterparts. The number of Ly-alpha lines observed in the spectrum of PKS 0405-12 is within 1 sigma of the number predicted on the basis of previous HST observations of 3C 273 and of H1821 + 643. Combining the HST observations of 3C 273, H1821 + 643, and PKS 0405-12, we estimate the local number density of Ly-alpha systems with rest equivalent widths larger than 0.32 A to be about 15 +/- 4 Ly-alpha lines per unit redshift. Ground-based images reveal a rich field of galaxies in the direction of PKS 0405-12, including many galaxies with the brightnesses and sizes expected if they belong to a cluster associated with the quasar. The quasar spectrum does not show any evidence for absorption at the redshift of the emission lines, indicating a covering factor of less than unity for the halos of galaxies in the cluster around PKS 0405 - 12.

  14. Ketide Synthase (KS) Domain Prediction and Analysis of Iterative Type II PKS Gene in Marine Sponge-Associated Actinobacteria Producing Biosurfactants and Antimicrobial Agents

    PubMed Central

    Selvin, Joseph; Sathiyanarayanan, Ganesan; Lipton, Anuj N.; Al-Dhabi, Naif Abdullah; Valan Arasu, Mariadhas; Kiran, George S.

    2016-01-01

    The important biological macromolecules, such as lipopeptide and glycolipid biosurfactant producing marine actinobacteria were analyzed and their potential linkage between type II polyketide synthase (PKS) genes was explored. A unique feature of type II PKS genes is their high amino acid (AA) sequence homology and conserved gene organization. These enzymes mediate the biosynthesis of polyketide natural products with enormous structural complexity and chemical nature by combinatorial use of various domains. Therefore, deciphering the order of AA sequence encoded by PKS domains tailored the chemical structure of polyketide analogs still remains a great challenge. The present work deals with an in vitro and in silico analysis of PKS type II genes from five actinobacterial species to correlate KS domain architecture and structural features. Our present analysis reveals the unique protein domain organization of iterative type II PKS and KS domain of marine actinobacteria. The findings of this study would have implications in metabolic pathway reconstruction and design of semi-synthetic genomes to achieve rational design of novel natural products. PMID:26903957

  15. 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.

  16. Observações simultâneas no óptico e infravermelho próximo dos BL Lacs PKS 2005-489 e PKS 2155-304 em diversas escalas de tempo

    NASA Astrophysics Data System (ADS)

    Dominici, T. P.; Abraham, Z.; Galo, A. L.

    2003-08-01

    A existência de variações rápidas de brilho em alguns blazares é um fenômeno bem comprovado, mas até agora não sabemos ao certo quais são os mecanismos físicos envolvidos. A maior dificuldade é a ausência de observações multibanda simultâneas que poderiam fornecer vínculos aos modelos. Buscando colaborar com a discussão estudamos o comportamento de dois BL Lacs, PKS 2005-489 e PKS 2155-304, em relação à variabilidade em diversas escalas de tempo, de poucos minutos até vários meses, com observações simultâneas em seis bandas espectrais (óptico e infravermelho próximo). Para tanto dois telescópios do LNA foram utilizados em conjunto nas campanhas observacionais realizadas em 2001 e 2002, cujos resultados são apresentados aqui. As duas fontes apresentaram características bastante diferentes, inclusive em relação à existência de variabilidade nos índices espectrais. Particularmente, registramos a primeira detecção de variações em escalas de tempo da ordem de poucos minutos em PKS 2005-489, com evidências da presença de um atraso entre as curvas de luz nas bandas V e R e a variação em R ocorrendo antes (o contrário do esperado no modelo de shock-in-jet). Em PKS 2155-304 detectamos pela primeira vez variabilidade em escalas de tempo de poucos minutos no infravermelho em um AGN. As observações indicam que as variações de brilho em blazares são o resultado da ação de mais de um fenômeno, especialmente em escalas de tempo muito curtas. Alguns cenários físicos são sugeridos para explicar os resultados observacionais.

  17. Upstream pressure variations associated with the bow shock and their effects on the magnetosphere

    NASA Technical Reports Server (NTRS)

    Fairfield, D. H.; Baumjohann, W.; Paschmann, G.; Luehr, H.; Sibeck, D. G.

    1990-01-01

    The AMPTE IRM solar wind data are analyzed to determine the relationship between upstream pressure fluctuations and magnetospheric perturbations. It is argued that the upstream pressure variations are not inherent in the solar wind but rather are associated with the bow shock. This conclusion follows from the fact that the upstream field strength and density associated with perturbations are highly correlated with each other, while they tend to be anticorrelated in the undisturbed solar wind, and that the upstream perturbations occur within the foreshock or at its boundary. The results imply a mode of interaction between the solar wind upstream and the magnetosphere whereby density changes produced in the foreshock subsequently convect through the bow shock and impinge on the magnetosphere. Upstream pressure perturbations should create significant effects on the magnetopause and at the foot of nearby field lines that lead to the polar cusp ionosphere.

  18. Nonthermal ions and associated magnetic field behavior at a quasi-parallel earth's bow shock

    NASA Technical Reports Server (NTRS)

    Wilkinson, W. P.; Pardaens, A. K.; Schwartz, S. J.; Burgess, D.; Luehr, H.; Kessel, R. L.; Dunlop, M.; Farrugia, C. J.

    1993-01-01

    Attention is given to ion and magnetic field measurements at the earth's bow shock from the AMPTE-UKS and -IRM spacecraft, which were examined in high time resolution during a 45-min interval when the field remained closely aligned with the model bow shock normal. Dense ion beams were detected almost exclusively in the midst of short-duration periods of turbulent magnetic field wave activity. Many examples of propagation at large elevation angles relative to the ecliptic plane, which is inconsistent with reflection in the standard model shock configuration, were discovered. The associated waves are elliptically polarized and are preferentially left-handed in the observer's frame of reference, but are less confined to the maximum variance plane than other previously studied foreshock waves. The association of the wave activity with the ion beams suggests that the former may be triggered by an ion-driven instability, and possible candidates are discussed.

  19. The Effect of Metallic TPS Panel Bowing on the Surface Heating of the X-33 Vehicle

    NASA Technical Reports Server (NTRS)

    Palmer, Grant; Kontinos, Dean; Langhoff, Stephen R. (Technical Monitor)

    1997-01-01

    The thermal protection system of the windward surface of the X-33 vehicle consists of metallic honeycomb sandwich panels. Thermal gradients experienced during the descent phase of the trajectory result in a different rate of thermal expansion between the inner and outer face sheets of the metallic panels. This causes the panels to bow outward when the temperature of the outer face sheet is larger than that of the inner face sheet and inward when the temperature of the outer face sheet is less than that of he inner face sheet. This results in a quilted-type body surface. Using computational fluid dynamic analysis, this study will determine the effect the metallic TPS panel bowing has on the surface heating.

  20. Nonlinear Development of ULF waves in the Upstream of Earth's Bow Shock

    NASA Astrophysics Data System (ADS)

    Lee, E.; Parks, G. K.; Lin, N.; Hong, J.; Kim, K. H.; Lee, D. H.

    2015-12-01

    In the upstream region of Earth's bow shock ULF waves are frequently observed. These waves are usually associated with backstreaming ions from the bow shock. In this study we investigated nonlinear development of the ULF waves using multi-point measurements from the Cluster spacecraft. Small amplitude waves observed at spacecraft 3 (C3) rapidly grew and became nonlinear as they were observed at spacecraft 1 (C1) located downstream from C3. The nonlinear growth occurred within a few gyro-period of protons. Ion beams with Tperp/Tpara>1 were observed with the small amplitude waves at C3. As the waves grew nonlinearly, the core of the ion beams was decelerated, but they were also scattered both in energy and pitch angle producing more energetic, diffuse particles. This results in more diffuse distributions for the ULF waves with larger amplitude. During the interaction the original solar wind ions were not much disturbed.

  1. Bloodstain pattern analysis in a case of suicide with a compound bow and arrow.

    PubMed

    Wilson, Christopher I; Altschul, Samuel; Mead, Anthony; Flannagan, Lisa M

    2004-03-01

    The incidence of human fatalities due to arrow injuries in the medical literature is rare. We report an incident involving a 46-year-old man who was found in his secured apartment with a fatal arrow wound of his chest and abdomen. The initial scene investigation suggested that the victim impaled himself with an arrow attached to a razor-sharp, 4-bladed broad-head hunting tip before collapsing on the floor. However, analysis of the bloodstain patterns suggested that the victim used the compound bow to propel the arrow. When investigating deaths due to bows and arrows, thorough scene investigation along with bloodstain pattern analysis is essential in determining the mechanism of injury and manner of death.

  2. Conduction of thermal energy in the neighborhood of the earth's bow shock

    NASA Technical Reports Server (NTRS)

    Hohlfeld, R. G.

    1976-01-01

    The Rankine-Hugoniot equations for MHD shocks are generalized by the addition of a term to the energy conservation equation representing a nonzero heat flow in the plasma in the neighborhood of the shock. This generalization is found to be compatible with the assumption of infinite electrical conductivity. The effects of plasma waves in this treatment are of the order of the reciprocal Alfvenic Mach number squared and hence are neglected. The effect of alpha particles in the solar wind is discussed. Seven crossings of the earth's bow shock by Explorer 35 in lunar orbit are analyzed. Sufficient data are available so that the determination of a dimensionless parameter, psi, characterizing the heat-flow difference across the bow shock is possible. The values of psi indicate energy-flux densities due to heat flow which are a nonnegligible fraction of the total energy flux. Two possible interpretations of psi are discussed.

  3. High-Energy-Density Laboratory Astrophysics Studies of Jets and Bow Shocks

    NASA Astrophysics Data System (ADS)

    Foster, J. M.; Wilde, B. H.; Rosen, P. A.; Williams, R. J. R.; Blue, B. E.; Coker, R. F.; Drake, R. P.; Frank, A.; Keiter, P. A.; Khokhlov, A. M.; Knauer, J. P.; Perry, T. S.

    2005-11-01

    We present the first results from high-energy-density laboratory astrophysics experiments that explore the interaction of supersonic jets/outflows with an ambient medium. Our experiments were conducted on the Omega laser facility, a large Inertial Confinement Fusion facility. In our experiments, a laser pulse drives a supersonic jet into foam. High-resolution X-ray radiography reveals the resulting highly structured bow shock. These are the first laboratory astrophysics experiments to capture the behavior of both the jet and the bow shock. We discuss the astrophysical relevance of the flow processes that we observe in the experiments and in the accompanying numerical models. Scaling arguments suggest that our experiments are most directly relevant to active galactic nucleus jets and planetary nebula outflows, while future work may allow our experiments to extend into regimes relevant to radiative outflows from young stellar objects. Contains material © British Crown Copyright 2005/MOD, reprinted with permission.

  4. Large amplitude ship motions and bow flare slamming pressures in regular head seas

    SciTech Connect

    Tao, Z.; Incecik, A.

    1996-12-31

    In this paper, the motion equations incorporating nonlinear terms due to large amplitude motions and bow flare slamming pressures are described in regular head seas. Numerical predictions of ship motions based on a small amplitude linear theory and large amplitude nonlinear method and experimental data are compared with each other in the frequency and time domain. The nonlinear restoring force, nonlinear damping force and nonlinear fluid momentum force are considered in predicting ship motions. The frequency dependent added mass and damping coefficient are computed at the instantaneous submerged sections of the ship. The momentum slamming theory and Wagner theory are used to predict the bow flare slamming pressure. The total impact pressure is expressed as the sum of water immersion impact pressure and wave striking impact pressure. There is a satisfactory agreement between theoretical predictions and model test measurements.

  5. The density of cometary protons upstream of Comet Halley's bow shock

    NASA Technical Reports Server (NTRS)

    Neugebauer, M.; Goldstein, B. E.; Balsiger, H.; Neubauer, F. M.; Schwenn, R.

    1989-01-01

    Cometary protons picked up by the solar wind were detected by the high energy range spectrometer of the Giotto ion mass spectrometer starting at a cometocentric distance of about 12 million km. On the average, the density of cometary protons varied approximately as the inverse square of the cometocentric distance, reaching a value of 0.11/cu cm just outside the bow shock. The data can be successfully fit to models that include substantial amounts of both slow (1 km/s) and fast (8 km/s or greater) H atoms beyond the bow shock. Large local variations in the density of picked-up protons can be explained on the basis of variations in the direction of the interplanetary magnetic field in upstream regions where pitch angle scattering was weak.

  6. The density of cometary protons upstream of comet Halley's bow shock

    SciTech Connect

    Neugebauer, M.; Goldstein, B.E. ); Balsiger, H. ); Neubauer, F.M. ); Schwenn, R. ); Shelley, E.G. )

    1989-02-01

    Cometary protons picked up by the solar wind were detected by the high energy range spectrometer of the Giotto ion mass spectrometer starting at a cometocentric distance of {approximately}12 {times} 10{sup 6} km. On the average, the density of cometary protons varied approximately as the inverse square of the cometocentric distance, reaching a value of 0.11 cm{sup {minus}3} just outside the bow shock. The data can be successfully fit to models that include substantial amounts of both slow ({approximately}1 km/s) and fast ({ge} 8 km/s) H atoms beyond the bow shock. Large local variations in the density of picked-up protons can be explained on the basis of variations in the direction of the interplanetary magnetic field in upstream regions where pitch angle scattering was weak.

  7. Theoretical study of the transonic lift of a double-wedge profile with detached bow wave

    NASA Technical Reports Server (NTRS)

    Vincenti, Walter G; Wagoner, Cleo B

    1954-01-01

    A theoretical study is described of the aerodynamic characteristics at small angle of attack of a thin, double-wedge profile in the range of supersonic flight speed in which the bow wave is detached. The analysis is carried out within the framework of the transonic (nonlinear) small-disturbance theory, and the effects of angle of attack are regarded as a small perturbation on the flow previously calculated at zero angle. The mixed flow about the front half of the profile is calculated by relaxation solution of a suitably defined boundary-value problem for transonic small-disturbance equation in the hodograph plane (i.e., the Tricomi equation). The purely supersonic flow about the rear half is found by an extension of the usual numerical method of characteristics. Analytical results are also obtained, within the framework of the same theory, for the range of speed in which the bow wave is attached and the flow is completely supersonic.

  8. First Detection of a Pulsar Bow Shock Nebula in Far-UV: PSR J0437-4715

    NASA Astrophysics Data System (ADS)

    Rangelov, Blagoy; Pavlov, George G.; Kargaltsev, Oleg; Durant, Martin; Bykov, Andrei M.; Krassilchtchikov, Alexandre

    2016-11-01

    Pulsars traveling at supersonic speeds are often accompanied by cometary bow shocks seen in Hα. We report on the first detection of a pulsar bow shock in the far-ultraviolet (FUV). We detected it in FUV images of the nearest millisecond pulsar J0437-4715 obtained with the Hubble Space Telescope. The images reveal a bow-like structure positionally coincident with part of the previously detected Hα bow shock, with an apex at 10″ ahead of the moving pulsar. Its FUV luminosity, L(1250{--}2000 \\mathringA )≈ 5 × {10}28 erg s-1, exceeds the Hα luminosity from the same area by a factor of 10. The FUV emission could be produced by the shocked interstellar medium matter or, less likely, by relativistic pulsar wind electrons confined by strong magnetic field fluctuations in the bow shock. In addition, in the FUV images we found a puzzling extended (≃3″ in size) structure overlapping with the limb of the bow shock. If related to the bow shock, it could be produced by an inhomogeneity in the ambient medium or an instability in the bow shock. We also report on a previously undetected X-ray emission extending for about 5″ ahead of the pulsar, possibly a pulsar wind nebula created by shocked pulsar wind, with a luminosity L(0.5-8 keV) ˜ 3 × 1028 erg s-1. 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 NAS 5-26555. These observations are associated with programs GO 12917 and GO 10568.

  9. Three-dimensional plasma structures with anomalous flow directions near the earth's bow shock

    SciTech Connect

    Paschmann, G.; Haerendel, G.; Sckopke, N.; Moebius, E. ); Luehr, H. ); Carlson, C.W. )

    1988-10-01

    They authors examined AMPTE IRM data obtained in the solar wind near the Earth's bow shock and found 16 well-defined cases where a region of hot subsonic plasma is embedded in the solar wind. They also find the low ({approximately}200 km/s) flow velocities, strongly deflected from the solar wind, and they substantially strengthen the local time dependence of the flow which invariably is directed dawnward for prenoon events and duskward for postnoon events. The results differ from the reported ISEE results in two respects. First, the flows they observe tend to have larger angles relative to the solar wind, and they often even have a sunward component. Second, the events they have selected cannot be described as diamagnetic cavities. This apparent discrepancy may simply result from different event selection criteria. A quantitative analysis of the regions flanking the hot core shows they consist of fast, nearly perpendicular, supercritical shocks on the outside and tangential discontinuities on the inside. Another new finding concerns the presence of enhanced fluxes of > 70-keV electrons which appear to be of magnetospheric origin. The majority of events which are not embedded in the solar wind but occur between the solar wind and the magnetosheath, at times replacing the regular bow shock. Among the mechanisms discussed as causes for these events are the formation of sunward directed plasma jets from magnetopause reconnection, or from amplification of magnetic stresses associated with rotational discontinuities in the interplanetary medium; sudden and localized enhancements of bow shock reflection; and the interaction of the bow shock with tangential discontinuities having a specific internal structure.

  10. Serendipitous discovery of an infrared bow shock near PSR J1549–4848 with Spitzer

    SciTech Connect

    Wang, Zhongxiang; Kaplan, David L.; Slane, Patrick; Morrell, Nidia; Kaspi, Victoria M.

    2013-06-01

    We report on the discovery of an infrared cometary nebula around PSR J1549–4848 in our Spitzer survey of a few middle-aged radio pulsars. Following the discovery, multi-wavelength imaging and spectroscopic observations of the nebula were carried out. We detected the nebula in Spitzer Infrared Array Camera 8.0, Multiband Imaging Photometer for Spitzer 24 and 70 μm imaging, and in Spitzer IRS 7.5-14.4 μm spectroscopic observations, and also in the Wide-field Infrared Survey Explorer all-sky survey at 12 and 22 μm. These data were analyzed in detail, and we find that the nebula can be described with a standard bow shock shape, and that its spectrum contains polycyclic aromatic hydrocarbon and H{sub 2} emission features. However, it is not certain which object drives the nebula. We analyze the field stars and conclude that none of them can be the associated object because stars with a strong wind or mass ejection that usually produce bow shocks are much brighter than the field stars. The pulsar is approximately 15'' away from the region in which the associated object is expected to be located. In order to resolve the discrepancy, we suggest that a highly collimated wind could be emitted from the pulsar and produce the bow shock. X-ray imaging to detect the interaction of the wind with the ambient medium- and high-spatial resolution radio imaging to determine the proper motion of the pulsar should be carried out, which will help verify the association of the pulsar with the bow shock nebula.

  11. OPTICAL HYDROGEN ABSORPTION CONSISTENT WITH A THIN BOW SHOCK LEADING THE HOT JUPITER HD 189733B

    SciTech Connect

    Cauley, P. Wilson; Redfield, Seth; Jensen, Adam G.; Barman, Travis; Endl, Michael; Cochran, William D.

    2015-09-01

    Bow shocks are ubiquitous astrophysical phenomena resulting from the supersonic passage of an object through a gas. Recently, pre-transit absorption in UV metal transitions of the hot Jupiter (HJ) exoplanets HD 189733b and WASP12-b have been interpreted as being caused by material compressed in a planetary bow shock. Here we present a robust detection of a time-resolved pre-transit, as well as in-transit absorption signature around the HJ exoplanet HD 189733b using high spectral resolution observations of several hydrogen Balmer lines. The line shape of the pre-transit feature and the shape of the timeseries absorption provide the strongest constraints on the morphology and physical characteristics of extended structures around an exoplanet. The in-transit measurements confirm the previous exospheric Hα detection, although the absorption depth measured here is ∼50% lower. The pre-transit absorption feature occurs 125 minutes before the predicted optical transit, a projected linear distance from the planet to the stellar disk of 7.2 R{sub p}. The absorption strength observed in the Balmer lines indicates an optically thick, but physically small, geometry. We model this signal as the early ingress of a planetary bow shock. If the bow shock is mediated by a planetary magnetosphere, the large standoff distance derived from the model suggests a large planetary magnetic field strength of B{sub eq} = 28 G. Better knowledge of exoplanet magnetic field strengths is crucial to understanding the role these fields play in planetary evolution and the potential development of life on planets in the habitable zone.

  12. Congenital bowing of the tibia due to infantile lipofibromatosis corrected with a Taylor Spatial Frame.

    PubMed

    Joseph, George; Zenios, Michalis

    2014-12-01

    Congenital lipofibromatosis is a rare slow growing benign fibrofatty neoplasm presenting in childhood. The case of a boy presenting soon after birth with diffuse lower extremity enlargement associated with a significant tibial deformity is presented. Magnetic resonance imaging and soft tissue biopsy confirmed the diagnosis of lipofibromatosis. The child started having problems with his gait after the age of two. The tibial bowing was corrected gradually using a Taylor Spatial Frame resulting in a good clinical outcome.

  13. FORMATION OF COSMIC CRYSTALS IN HIGHLY SUPERSATURATED SILICATE VAPOR PRODUCED BY PLANETESIMAL BOW SHOCKS

    SciTech Connect

    Miura, H.; Yamada, J.; Tsukamoto, K.; Nozawa, J.; Tanaka, K. K.; Yamamoto, T.; Nakamoto, T.

    2010-08-10

    Several lines of evidence suggest that fine silicate crystals observed in primitive meteorite and interplanetary dust particles (IDPs) nucleated in a supersaturated silicate vapor followed by crystalline growth. We investigated evaporation of {mu}m-sized silicate particles heated by a bow shock produced by a planetesimal orbiting in the gas in the early solar nebula and condensation of crystalline silicate from the vapor thus produced. Our numerical simulation of shock-wave heating showed that these {mu}m-sized particles evaporate almost completely when the bow shock is strong enough to cause melting of chondrule precursor dust particles. We found that the silicate vapor cools very rapidly with expansion into the ambient unshocked nebular region; for instance, the cooling rate is estimated to be as high as 2000 K s{sup -1} for a vapor heated by a bow shock associated with a planetesimal of radius 1 km. The rapid cooling of the vapor leads to nonequilibrium gas-phase condensation of dust at temperatures much lower than those expected from the equilibrium condensation. It was found that the condensation temperatures are lower by a few hundred K or more than the equilibrium temperatures. This explains the results of the recent experimental studies of condensation from a silicate vapor that condensation in such large supercooling reproduces morphologies similar to those of silicate crystals found in meteorites. Our results strongly suggest that the planetesimal bow shock is one of the plausible sites for formation of not only chondrules but also other cosmic crystals in the early solar system.

  14. Observation of Motion of Bowed Strings and Resonant Strings in Violin Performances

    NASA Astrophysics Data System (ADS)

    Matsutani, Akihiro

    2013-10-01

    The motion of a bowed string and a resonant string of a violin were simultaneously observed for the first time. The results of the direct observation of string motion in double stops and harmonics are also presented. The importance of the resonance was experimentally demonstrated from these observations. It is suggested that players should take account of the resonance and ideal Helmholtz motion in violin performances.

  15. Numerical investigation of the bowed stator effects in a transonic fan at low Reynolds number

    NASA Astrophysics Data System (ADS)

    Huang, Enliang; Zhao, Shengfeng; Gong, Jianbo; Lu, Xingen; Zhu, Junqiang

    2017-02-01

    The performance of fan stage in a small turbofan engines is significantly affected at high-altitude low Reynolds number. In order to examine the effect of low Reynolds number on the fan stage, 3D numerical simulation method was employed to analyse the performance variations and the underlying flow structure in the fan stage. For the sake of decreasing the influence of low Reynolds number, the different bowed stator airfoils were redesigned and the effect of the modified design was evaluated.

  16. Laboratory studies of stagnating plasma flows with applications to inner solar system and stellar bow shocks

    NASA Astrophysics Data System (ADS)

    Weber, T. E.; Smith, R. J.; Hsu, S. C.

    2016-10-01

    Supercritical magnetized collisionless shocks are thought to play a dominant role in the overall partition of energy throughout the universe by converting flow kinetic energy to other forms such as thermal and supra-thermal populations, magnetic field enhancement, turbulence, and energetic particles. The Magnetized Shock Experiment (MSX) at LANL creates conditions similar to those of inner solar system and stellar bow shocks by accelerating hot (100s of eV during translation) dense (1022 - 1023 m-3) Field Reversed Configuration (FRC) plasmoids to 100s of km/s; resulting in β 1, collisionless plasma flows with Msonic and MAlfvén 10. The drifting FRC can be made to impinge upon a variety of static obstacles including: a strong mirror or cusp magnetic field (mimicking magnetically excited shocks such as the Earth's bow shock), plasma pileup from a solid obstacle (similar to the bow shocks of Mercury and the Moon), and a neural gas puff (bow shocks of Venus or the comets). Characteristic shock length and time scales that are both large enough to observe yet small enough to fit within the experiment, enabling study of the complex interplay of kinetic and fluid processes that mediate cosmic shocks and can generate non-thermal distributions, produce density and magnetic field enhancements much greater than predicted by fluid theory, and accelerate particles. An overview of the experimental program will be presented, including recent results. This work is supported by the U.S. DOE, Office of Science, Office of Fusion Energy Sciences under Contract No. DE-AC52-06NA25369.

  17. Variation of the ratio of specific heats across a detached bow shock

    NASA Technical Reports Server (NTRS)

    Chao, J. K.; Wiskerchen, M. J.

    1974-01-01

    Equations are derived which allow the ratio of specific heats behind the earth's bow shock to be evaluated if several pre-shock parameters (the specific-heat ratio, the Alfvenic Mach number, the sonic Mach number, and the angle between the shock normal at the stagnation point and the magnetic field) and the density jump across the shock are known. Numerical examples show that the dependence of the post-shock ratio on the pre-shock ratio is weak.

  18. A Search for Intergalactic Ne VIII in the COS Spectrum of PKS0405-123

    NASA Astrophysics Data System (ADS)

    Narayanan, Anand; Savage, B.; Wakker, B.; Yao, Y.; Danforth, C.; Froning, C.; Green, J.; Keeney, B.; Sembach, K.; Shull, M.

    2010-01-01

    The high S/N COS spectrum of the UV bright quasar PKS0405-123 provides the sensitivity required for a search of Ne VIII in QSO metal line absorption systems at z > 0.47. The EUV lines of Ne VIII 770,780 A are ideal tracers of hot collisionally ionized gas at T (0.5 - 1) x 106 K. However, detecting these weak lines require spectra of good S/N in which the effects of detector fixed pattern noise are well understood. The z = 0.49510 O VI multiphase metal line absorption system along this sight line is ideally suited for a search for Ne VIII. Chen & Mulchaey (2009) have identified an emission line galaxy of extended morphology at a projected physical separation of 77 kpc from this absorber. The COS spectrum provides coverage of O II 834, O III 833, O IV 788, C III 977 and higher order Lyman series lines associated with this absorber at a much higher S/N than the FUSE and STIS observations for this target. The improved line measurement based on the COS spectrum, combined with the information on O VI from STIS is used to derive detailed physical conditions in the multiple gas phases of this absorber. Evidence for the presence of shock-heated gas would imply that the absorber is tracing either transition temperature gas in the galaxy's halo or an intergalactic WHIM filament connecting galaxies as part of the large scale structure. This research has been supported by the NASA Cosmic Origins Spectrograph Program through a sub-contract to the University of Wisconsin from the University of Colorado.

  19. COS Observations Of Intergalactic O VI Systems In The Spectrum Of PKS 0405-123

    NASA Astrophysics Data System (ADS)

    Savage, Blair D.; Narayanan, A.; Wakker, B.; Danforth, C.; Froning, C.; Green, J.; Keeney, B.; Sembach, K.; Shull, M.; Stocke, J.; Yao, Y.

    2010-01-01

    Signal-to-noise > 35 observations with the COS of the QSO PKS 0405-123 (z em = 0.5726) at a resolution of 15 to 20 km/s from 1150 to 1780 A are analyzed to study the physical conditions in the prominent O VI absorption systems at z = 0. 16710, 0.18292, 0.36156, 0.36332 and 0.49501. These systems have previously been studied in STIS and FUSE spectra with S/N 10 to 15. The system at z = 0.16710 is a Lyman limit system with logN(HI) = 16.45 +/-0.05 (Prochaska et al. 2004). Chen and Mulchaey (2009) have found Galaxies with impact parameters of 81, 165 and 77 kpc associated with the z = 0.16710, O.36156, and 0.49501 absorbers. No galaxies with impact parameters < 1 Mpc have been found associated with the other two absorbers. The high S/N of the observations allows the measurement of important ions not previously detected and permits a careful evaluation of the kinematical relationships among the detected ions. The observations are being used to determine the origin of the ionization of O VI in simple and complex absorption systems. The high S/N allows a search for broad Ly alpha possibly associated with O VI if it is collisonally ionized at T 3x105 K. The multi-phase system at z = 0.16710 may be tracing a high velocity cloud in the halo of the associated galaxy. The UV properties of this absorber are similar to that for the high velocity clouds in the Milky Way halo where O VI is likely produced in interface regions between hot halo gas with T >1x106 K and the cooler gas of the HVC. The observations show that COS is extremely well suited for studies at low redshift of the surroundings of galaxies and their connection to the cosmic web.

  20. Characterizing the Low-Redshift Intergalactic Medium toward PKS 1302-102

    NASA Astrophysics Data System (ADS)

    Cooksey, Kathy L.; Prochaska, Jason X.; Chen, Hsiao-Wen; Mulchaey, John S.; Weiner, Benjamin J.

    2008-03-01

    We present a detailed analysis of the intergalactic metal-line absorption systems in the archival HST STIS and FUSE ultraviolet spectra of the low-redshift quasar PKS 1302-102 (zQSO = 0.2784). We supplement the archive data with CLOUDY ionization models and a survey of galaxies in the quasar field. There are 15 strong Lyα absorbers with column densities NH I > 14. Of these, six are associated with at least C III λ977 absorption [log N(C+ +) > 13]; this implies a redshift density dNC III/dz = 36-9+13 (68% confidence limits) for the five detections with rest equivalent width Wr > 50 mÅ. Two systems show O VI λλ1031, 1037 absorption in addition to C III [log N(O+ 5) > 14]. One is a partial Lyman limit system ( log NH I = 17) with associated C III, O VI, and Si III λ1206 absorption. There are three tentative O VI systems that do not have C III detected. For one O VI doublet with both lines detected at 3 σ with Wr > 50 mÅ, dNO VI/dz = 7-4+9. We also search for O VI doublets without Lyα absorption but identify none. From CLOUDY modeling, these metal-line systems have metallicities spanning the range -4 lesssim [ M/H ] lesssim - 0.3. The two O VI systems with associated C III absorption cannot be single-phase, collisionally ionized media based on the relative abundances of the metals and kinematic arguments. From the galaxy survey, we discover that the absorption systems are in a diverse set of galactic environments. Each metal-line system has at least one galaxy within 500 km s-1 and 600 h-175 kpc with L > 0.1L*.

  1. The z = 0.8596 damped Ly-alpha absorbing galaxy toward PKS 0454+039

    NASA Technical Reports Server (NTRS)

    Steidel, Charles C.; Bowen, David V.; Blades, J. Chris; Dickenson, Mark

    1995-01-01

    We present Hubble Space Telescope (HST) and ground-based data on the Z(sub abs) = 0.8596 metal-line absorption system along the line of sight to PKS 0454+0356. The system is a moderate-redshift damped Ly-alpha system, with N(H I) = (5.7 +/- 0.3) x 10(exp 20)/sq cm as measured from the Faint Object Spectrograph (FOS) spectrum. We also present ground-based images which we use to identify the galaxy which most probably gives rise to the damped system; the most likely candidate is relatively underluminous by QSO absorber standards M(sub B) approximately -19.0 for A(sub 0) = 0.5 and H(sub 0) = 50 km/s/Mpc) and lies approximately 8.5/h kpc in projection from the QSO sight line. Ground-based measurements of Zn II, Cr II, and Fe II absorption lines from this system allow us to infer abundances of (Zn/H) = -1.1, (Cr/H) = -1.2, and (Fe/H) = -1.2 indicating overall metallicity similar to damped systems at z is greater than 2, and that the depletion of Cr and Fe onto dust grains may be even less important than in many of the high-redshift systems of comparable metallicity. Limits previously placed on the 21 cm optical depth in the z = 0.8596 system, together with our new N(H I) measurement, suggest a very high spin temperature for the H I, T(sub s) is greater than 580 K.

  2. Brightest Fermi-LAT flares of PKS 1222+216: implications on emission and acceleration processes

    SciTech Connect

    Kushwaha, Pankaj; Singh, K. P.; Sahayanathan, Sunder

    2014-11-20

    We present a high time resolution study of the two brightest γ-ray outbursts from a blazar PKS 1222+216 observed by the Fermi Large Area Telescope (LAT) in 2010. The γ-ray light curves obtained in four different energy bands, 0.1-3, 0.1-0.3, 0.3-1, and 1-3 GeV, with time bins of six hours, show asymmetric profiles with similar rise times in all the bands but a rapid decline during the April flare and a gradual one during the June flare. The light curves during the April flare show an ∼2 day long plateau in 0.1-0.3 GeV emission, erratic variations in 0.3-1 GeV emission, and a daily recurring feature in 1-3 GeV emission until the rapid rise and decline within a day. The June flare shows a monotonic rise until the peak, followed by a gradual decline powered mainly by the multi-peak 0.1-0.3 GeV emission. The peak fluxes during both the flares are similar except in the 1-3 GeV band in April, which is twice the corresponding flux during the June flare. Hardness ratios during the April flare indicate spectral hardening in the rising phase followed by softening during the decay. We attribute this behavior to the development of a shock associated with an increase in acceleration efficiency followed by its decay leading to spectral softening. The June flare suggests hardening during the rise followed by a complicated energy dependent behavior during the decay. Observed features during the June flare favor multiple emission regions while the overall flaring episode can be related to jet dynamics.

  3. Standard systems for measurement of pKs and ionic mobilities. 1. Univalent weak acids.

    PubMed

    Slampová, Andrea; Krivánková, Ludmila; Gebauer, Petr; Bocek, Petr

    2008-12-05

    Determination of pK values of weak bases and acids by CZE has already attracted big attention in current practice and proved to offer the advantage of being applicable for mixtures of analytes. The method is based on the measurement of mobility curves plotting the effective mobility vs. the pH of the background electrolyte, and following computer-assisted regression involving corrections for ionic strength and temperature. To cover the necessary range of pH for a given case, both buffering weak acids and bases are used in one set of measurements, which requires implementing computations of individual ionic strength corrections for each pH value. It is also well known that some components of frequently used background electrolytes may interact with the analytes measured, on forming associates or complexes. This obviously deteriorates the reliability of the resulting data. This contribution brings a rational approach to this problem and establishes a standard system of anionic buffers for measurements of pKs and mobilities of weak acids, where the only counter cation present (besides H(+)) is Na(+). In this way, the risk of formation of complexes or associates of analytes with counter ions is strongly reduced. Moreover, the standard system of anionic buffers is selected in such a way that it provides, for an entire set of measurements, constant and accurately known ionic strength and the operational conditions are selected so that they provide constant Joule heating. Due to these precautions only one correction for ionic strength and temperature is needed for the obtained set of experimental data. This considerably facilitates their evaluation and regression analysis as the corrections need not be implemented in the computation software. The reliability and the advantages of the proposed system are well documented by experiments, where the known problematic group of phenol derivatives was measured with high accuracy and without any notice of anomalous behaviour.

  4. THE NATURE OF A GALAXY ALONG THE SIGHT LINE TO PKS 0454+039

    SciTech Connect

    Takamiya, Marianne; Chun, Mark; Kulkarni, Varsha P.; Gharanfoli, Soheila

    2012-10-01

    We report on the properties of a faint blue galaxy (G1) along the line of sight to the QSO PKS 0454+039 from spectroscopic and imaging data. We measured emission lines of H{alpha}, [S II] {lambda}{lambda}6716, 6732, and [N II] {lambda}6584 in the spectrum of G1 obtained with the Gemini/GMOS instrument. The spectroscopic redshift of G1 is z = 0.0715 {+-} 0.0002. From the extinction-corrected H{alpha} flux, we determine a modest star formation rate of SFR = 0.07 M{sub Sun} yr{sup -1} and a specific SFR of log (sSFR) -8.4. Using three different abundance indicators, we determine a nebular abundance 12 + log (O/H) ranging from 7.6 to 8.2. Based on the velocity dispersion inferred from the emission line widths and the observed surface brightness profile, we estimate the virial mass of G1 to be M{sub vir} {approx} 6.7 Multiplication-Sign 10{sup 9} M{sub Sun} with an effective radius of 2.0 kpc. We estimate the stellar mass of G1 using spectral energy distribution fitting to be M{sub *} Almost-Equal-To 1.2 Multiplication-Sign 10{sup 7} M{sub Sun} and an r'-luminosity of L{sub r'} = 1.5x10{sup 8} L{sub Sun }. Overall, G1 is a faint, low-mass, low-metallicity Im/H II galaxy. We also report on the line flux limits of another source (G3) which is the most likely candidate for the absorber system at z = 0.8596. From the spectrum of the QSO itself, we report a previously undetected Mg II {lambda}{lambda}2796, 2803 absorption line system at z = 1.245.

  5. On the Location of the 2009 GeV Flares of Blazar PKS 1510-089

    NASA Astrophysics Data System (ADS)

    Dotson, Amanda; Georganopoulos, Markos; Meyer, Eileen T.; McCann, Kevin

    2015-08-01

    Most of the radiated power of blazars is produced at GeV energies via inverse Compton scattering at an unknown distance from the central engine. Possible seed photon sources map to different locations along the jet spanning two orders of magnitude in distance from the black hole, ranging from the broad-line region (BLR, ˜0.1 pc), to the molecular torus (MT, ˜ 1- few pc), to the very long baseline interferometry (VLBI) radio core zone at ˜10 pc. Here, we apply a diagnostic for identifying the GeV emission zone (GEZ) in blazar PKS 1510-089 using four bright gamma-ray flares detected by Fermi in 2009. As shown by Dotson et al., the flare decay time should be energy-independent for flares in the BLR, but faster at higher energies for flares in the MT. We find that in the two cases where the gamma-ray flare was not accompanied by an optical flare, the decay times show an energy-dependence suggesting a location in the MT. For the two GeV flares accompanied by optical flares, we obtained very fast decay times (≲3 hr) in both low and high energy Fermi bands. For these flares, considering the simultaneous >100 GeV detection by HESS (H.E.S.S. Collaboration et al.) and the ejection of a superluminal component from the VLBI radio core in one case, our results suggest that both flares came from the vicinity of the VLBI core. We thus suggest that the GEZ is spread over a wide range of locations beyond the BLR.

  6. Farby-Perot observations and new models of the HH 47A and HH 47D bow shocks

    NASA Technical Reports Server (NTRS)

    Morse, Jon A.; Hartigan, Patrick; Heathcote, Steve; Raymond, John C.; Cecil, Gerald

    1994-01-01

    We present new models for the HH 47A and HH 47D bow shocks based on line flux and velocity maps obtained with an imaging Fabry-Perot spectrometer. We confirm that HH 47A and HH 47D each show a bow shock/Mach disk morphology, and that velocity variability in the outflow can account for the observed structures. While it was suggested a decade ago that the inner working surface HH 47A appears to be traveling into the wake of HH 47D, we find kinematic evidence that the outer bow shock HH 47D is also not the primary ejection event in the outflow but follows in the wake of previously ejected material. By comparing the observed line ratios and line profiles to those predicted by our bow shock models, we find that both bow shocks have substantially lower shock velocities than their space motions would imply, and that the emission from each bow shock is systematically blueshifted from the rest-frame velocity of the ambient emission, indicating a comoving preshock medium. We derive kinematic ages of approximately 1150 yr for HH 47D and approximately 550 yr for HH 47A, which implies that the stellar driving source may undergo repetitive eruptions similar to FU Orionis-type outbursts every several hundred years. This timescale is similar to estimates made by Reipurth and collaborators for the separation between major outbursts in the HH 34 and HH 111 stellar jets.

  7. Numerical Simulation of Star Formation by the Bow Shock of the Centaurus A Jet

    NASA Astrophysics Data System (ADS)

    Gardner, Carl L.; Jones, Jeremiah R.; Scannapieco, Evan; Windhorst, Rogier A.

    2017-02-01

    Recent Hubble Space Telescope (HST) observations of the extragalactic radio source Centaurus A (Cen A) display a young stellar population around the southwest tip of the inner filament 8.5 kpc from the galactic center of Cen A, with ages in the range 1–3 Myr. Crockett et al. have argued that the transverse bow shock of the Cen A jet triggered this star formation as it impacted dense molecular cores of clouds in the filament. To test this hypothesis, we perform three-dimensional numerical simulations of star formation induced by the jet bow shock in the inner filament of Cen A, using a positivity-preserving, weighted, essentially non-oscillatory method to solve the equations of gas dynamics with radiative cooling. We find that star clusters form inside a bow-shocked molecular cloud when the maximum initial density of the cloud is ≥slant 40 H2 molecules cm‑3. In a typical molecular cloud of mass {10}6 {M}ȯ and diameter 200 pc, approximately 20 star clusters of mass {10}4 {M}ȯ are formed, matching the HST images.

  8. Congenital posteromedial bowing of the tibia and fibula: treatment option by multilevel osteotomy.

    PubMed

    Napiontek, Marek; Shadi, Milud

    2014-03-01

    Few papers have described patients treated surgically with single osteotomy for congenital posteromedial bowing of the tibia and fibula. Only one paper has described two-level osteotomy for deformity correction: the first for deformity correction and the second for bone lengthening. There are no publications describing the surgical correction of deformation only by the method of multilevel tibial and fibular osteotomy. Research material included four children aged between 3.1 and 5.1 years (average age: 3.7 years) who were operated upon for bowing of the tibia and fibula exceeding 35° in the coronal plane. In all cases, tibial osteotomy was carried out at three or two levels accompanied by fibular osteotomy, and with intramedullary stabilization using K-wires (three patients) or Rush pin (one patient). Follow-up ranged from 3 to 7.7 years. In all cases, axis correction and bone healing were achieved. In large congenital posteromedial bowing of the tibia and fibula, a multilevel tibial and fibular osteotomy may be a better solution than an orthosis or a long time waiting for a spontaneous correction of the deformation. Large circumferential periosteal release that accompanied the surgery influenced the stimulation of bone growth. It may induce the process of lower limbs' equalization not to require the application of intensive surgical procedures.

  9. Interplanetary shock-bow shock interaction: Comparison of a global MHD model and observation

    NASA Astrophysics Data System (ADS)

    Goncharov, O.; Šafránková, J.; Němeček, Z.

    2015-09-01

    A fast forward shock passing through the bow shock would generate a train of new discontinuities that differ with the distance from the Sun-Earth line. However, interplanetary (IP) shocks are often followed by a rotation of the interplanetary magnetic field (IMF) over a large angle and a presence of this rotation can modify the interaction process. The present paper analyzes in detail one IP shock where data measured by Wind are used as an input to a global BATS-R-US MHD model and the model prediction is compared with Geotail magnetosheath observations. The study is based on three runs of the global MHD model that use different modifications of upstream conditions. We have found that (1) about 45% of IP shocks is followed by a significant IMF rotation within 15 min after the shock ramp; (2) the IMF rotation modifies the dynamics of the magnetospheric response to the IP shock arrival; (3) a train of new discontinuities created by an interaction of the IP shock with bow shock can be identified in MHD simulations as well as in the experimental data; and (4) a new discontinuity is created by the interaction of the IMF rotation with the bow shock.

  10. Magnetosheath Filamentary Structures Formed by Ion Acceleration at the Quasi-Parallel Bow Shock

    NASA Technical Reports Server (NTRS)

    Omidi, N.; Sibeck, D.; Gutynska, O.; Trattner, K. J.

    2014-01-01

    Results from 2.5-D electromagnetic hybrid simulations show the formation of field-aligned, filamentary plasma structures in the magnetosheath. They begin at the quasi-parallel bow shock and extend far into the magnetosheath. These structures exhibit anticorrelated, spatial oscillations in plasma density and ion temperature. Closer to the bow shock, magnetic field variations associated with density and temperature oscillations may also be present. Magnetosheath filamentary structures (MFS) form primarily in the quasi-parallel sheath; however, they may extend to the quasi-perpendicular magnetosheath. They occur over a wide range of solar wind Alfvénic Mach numbers and interplanetary magnetic field directions. At lower Mach numbers with lower levels of magnetosheath turbulence, MFS remain highly coherent over large distances. At higher Mach numbers, magnetosheath turbulence decreases the level of coherence. Magnetosheath filamentary structures result from localized ion acceleration at the quasi-parallel bow shock and the injection of energetic ions into the magnetosheath. The localized nature of ion acceleration is tied to the generation of fast magnetosonic waves at and upstream of the quasi-parallel shock. The increased pressure in flux tubes containing the shock accelerated ions results in the depletion of the thermal plasma in these flux tubes and the enhancement of density in flux tubes void of energetic ions. This results in the observed anticorrelation between ion temperature and plasma density.

  11. Variations and Effects of the Venusian Bow Shock from VEX Mission

    NASA Astrophysics Data System (ADS)

    Xue, Yansong; Jin, Shuanggen

    2014-04-01

    The upper atmosphere of Venus is not shielded by planetary magnetic field from direct interaction with the solar wind. The interaction of shocked solar wind and the ionosphere results in ionopause. Magnetic barrier, the inner region of dayside magnetosheath with the dominated magnetic pressure deflects the solar wind instead of the ionopause at solar maximum. Therefore, the structure and interaction of venusian ionosphere is very complex. Although the Venus Express (VEX) arrived at Venus in April 2006 provides more knowledge on the Venusian ionosphere and plasma environment, compared to Pioneer Venus Orbiter (PVO) with about 14 years of observations, some important details are still unknown (e.g., long Venusian bow shock variations and effects). In this paper, the bow shock positions of Venus are determined and analyzed from magnetometer (MAG) and ASPERA-4 of the Venus Express mission from May 28, 2006 to August 17, 2010. Results show that the altitude of BS was mainly affected by SZA (solar zenith angle) and Venus bow shocks inbound and outbound are asymmetry.

  12. On the generation of magnetosheath high speed jets by bow shock ripples (Invited)

    NASA Astrophysics Data System (ADS)

    Hietala, H.; Plaschke, F.

    2013-12-01

    The terrestrial magnetosheath is embedded with coherent high speed jets of about 1 RE in scale, predominantly during quasi-radial interplanetary magnetic field (IMF). When these high dynamic pressure (Pdyn) jets hit the magnetopause, they cause large indentations and further magnetospheric effects. The source of these jets has remained controversial. One of the proposed mechanisms is based on ripples of the quasi-parallel bow shock. In this paper, we combine for the first time four years of subsolar magnetosheath observations from the THEMIS mission and corresponding NASA/OMNI solar wind conditions with model calculations of a rippled bow shock. Concentrating on the magnetosheath close to the shock during low IMF cone-angles, we find that (1) 97% of the observed jets can be produced by local ripples of the shock under the observed upstream conditions; (2) the coherent jets form a significant fraction of the high Pdyn tail of the magnetosheath flow distribution; (3) the magnetosheath Pdyn distribution matches the flow from a bow shock with ripples that have a dominant amplitude to wavelength ratio of about 9% (~ 0.1 RE/1 RE) and are present ~12% of the time at any given location.

  13. High-Energy-Density, Laboratory-Astrophysics Studies of Jets and Bow Shocks

    SciTech Connect

    Foster, J M; Wilde, B H; Rosen, P A; Perry, T S; Khokhlov, A M; Coker, R F; Frank, A; Keiter, P A; Blue, B E; Drake, R P; Knauer, J P; Williams, R R

    2005-01-24

    Large-scale directional outflows of supersonic plasma, also known as ''jets'', are ubiquitous phenomena in astrophysics [1]. The interaction of such jets with surrounding matter often results in spectacular bow shocks, and intense radiation from radio to gamma-ray wavelengths. The traditional approach to understanding such phenomena is through theoretical analysis and numerical simulations. However, such numerical simulations have limited resolution, often assume axial symmetry, do not include all relevant physical processes, and fail to scale correctly in Reynolds number and perhaps other key dimensionless parameters. Additionally, they are frequently not tested by comparison with laboratory experiments. Recent advances in high-energy-density physics using large inertial-confinement-fusion devices now allow controlled laboratory experiments on macroscopic volumes of plasma of direct relevance relevant to astrophysics [2]. In this Letter we report the first results of experiments designed to study the evolution of supersonic plasma jets and the bow shocks they drive into a surrounding medium. Our experiments reveal both regular and highly complex flow patterns in the bow shock, thus opening a new window--complementary to computer simulations--into understanding the nature of three-dimensional astrophysical jets.

  14. Sociopolitical complexity and the bow and arrow in the American Southwest.

    PubMed

    VanPool, Todd L; O'Brien, Michael J

    2013-01-01

    The evolution of sociopolitical complexity, including heightened relations of cooperation and competition among large nonkin groups, has long been a central focus of anthropological research. Anthropologists suggest any number of variables that affect the waxing and waning of complexity and define the precise trajectories that groups take, including population density, subsistence strategies, warfare, the distribution of resources, and trade relationships. Changes in weaponry, here the introduction of the bow and arrow, can have profound implications for population aggregation and density, subsistence and settlement strategies, and access to resources, trade, and warfare.Bingham and Souza provide a general conceptual model for the relationship between complexity and the bow and arrow, arguing that this compound weapon system, whereby smaller projectiles travel at higher speed and are capable of hitting targets more accurately and at greater distances than hand-thrown darts, fundamentally favors the formation of larger groups because it allows for cost-effective means of dealing with conflicts of interest through social coercion, thereby dramatically transforming kin-based social relations. Here we consider the impacts the introduction of the bow and arrow had on sociopolitical complexity in the North American Southwest.

  15. Magnetosheath filamentary structures formed by ion acceleration at the quasi-parallel bow shock

    NASA Astrophysics Data System (ADS)

    Omidi, N.; Sibeck, D.; Gutynska, O.; Trattner, K. J.

    2014-04-01

    Results from 2.5-D electromagnetic hybrid simulations show the formation of field-aligned, filamentary plasma structures in the magnetosheath. They begin at the quasi-parallel bow shock and extend far into the magnetosheath. These structures exhibit anticorrelated, spatial oscillations in plasma density and ion temperature. Closer to the bow shock, magnetic field variations associated with density and temperature oscillations may also be present. Magnetosheath filamentary structures (MFS) form primarily in the quasi-parallel sheath; however, they may extend to the quasi-perpendicular magnetosheath. They occur over a wide range of solar wind Alfvénic Mach numbers and interplanetary magnetic field directions. At lower Mach numbers with lower levels of magnetosheath turbulence, MFS remain highly coherent over large distances. At higher Mach numbers, magnetosheath turbulence decreases the level of coherence. Magnetosheath filamentary structures result from localized ion acceleration at the quasi-parallel bow shock and the injection of energetic ions into the magnetosheath. The localized nature of ion acceleration is tied to the generation of fast magnetosonic waves at and upstream of the quasi-parallel shock. The increased pressure in flux tubes containing the shock accelerated ions results in the depletion of the thermal plasma in these flux tubes and the enhancement of density in flux tubes void of energetic ions. This results in the observed anticorrelation between ion temperature and plasma density.

  16. Nonlinear PRD components of EBR-II compared with bowing analyses

    SciTech Connect

    Meneghetti, D.; Kucera, D.A.

    1987-01-01

    The nonlinear components of the power reactivity decrements (PRDs) for Experimental Breeder Reactor II (EBR-II) runs 85A, 93A, 99A, and 122A have been reported. These nonlinear components were deduced by subtraction of the calculated linear (and Doppler) components from the measured PRD curves. The linear (and Doppler) components of the PRDs were calculated using the EBRPOCO program together with an addition to the program (RODCO) that accounts for the effects of positionings of the control rods. Corresponding calculated bowing components of these runs have now been calculated assuming that the hex can ducts are unirradiated and thus have been assumed to have neither swelling nor bowing at the zero-power level in the analyses. Furthermore, the initial separations of the subassemblies at the contact-button levels are all assumed to be the unirradiated nominal 0.002 in. (0.051 mm). Comparison of these calculations with the bowing components deduced from the measurements enable the signs and magnitudes of the effects of the unknown initial conditions to be ascertained.

  17. Exploring Astrophysically Relevant Bow Shocks Using MIFEDS and the OMEGA Laser

    NASA Astrophysics Data System (ADS)

    Levesque, Joseph; Kuranz, Carolyn; Young, Rachel; Fiksel, Gennady; Manuel, Mario; Trantham, Matthew; Klein, Sallee; Hartigan, Patrick; Liao, Andy; Li, Chikang

    2016-10-01

    We present current experiments using the Omega Laser Facility and their magneto-inertial fusion electrical discharge system (MIFEDS) to observe the effect of magnetic pressure on bow shock dynamics in an astrophysically relevant regime. Astrophysical bow shocks are an interesting phenomenon in which a shock forms when incident supersonic flow encounters a sufficiently magnetized medium surrounding an object. The most well-known example of this phenomena is the interaction of the solar wind with the Earth's magnetic field, which creates our magnetosphere. In our experiment the magnetosphere will be emulated by a current flowing through a curved wire to create an azimuthal magnetic field. To create the analogous solar wind, lasers rear-irradiate two opposing graphite targets so the plasma outflows collide and then expand along the collision plane toward the magnetized wires. We use the UV Thomson scattering diagnostic technique to determine plasma parameters along with optical imaging and proton radiography to characterize the plasma flow and the bow shock that forms. This work is supported by the U.S. DOE, through NNSA Grants DE-NA0002956 (SSAA) and DE-NA0002719 (NLUF), by the LLE under DE-NA0001944, and by the LLNL under subcontract B614207 to DE-AC52-07NA27344.

  18. The Bow City structure, southern Alberta, Canada: The deep roots of a complex impact structure?

    NASA Astrophysics Data System (ADS)

    Glombick, Paul; Schmitt, Douglas R.; Xie, Wei; Bown, Todd; Hathway, Ben; Banks, Christopher

    2014-05-01

    Geological and geophysical evidence is presented for a newly discovered, probable remnant complex impact structure. The structure, located near Bow City, southern Alberta, has no obvious morphological expression at surface. The geometry of the structure in the shallow subsurface, mapped using downhole geophysical well logs, is a semicircular structural depression approximately 8 km in diameter with a semicircular uplifted central region. Detailed subsurface mapping revealed evidence of localized duplication of stratigraphic section in the central uplift area and omission of strata within the surrounding annular region. Field mapping of outcrop confirmed an inlier of older rocks present within the center of the structure. Evidence of deformation along the eastern margin of the central uplift includes thrust faulting, folding, and steeply dipping bedding. Normal faults were mapped along the northern margin of the annular region. Isopach maps reveal that structural thickening and thinning were accommodated primarily within the Belly River Group. Evidence from legacy 2-D seismic data is consistent with the subsurface mapping and reveals additional insight into the geometry of the structure, including a series of listric normal faults in the annular region and complex faulting within the central uplift. The absence of any ejecta blanket, breccia, suevite, or melt sheet (based on available data) is consistent with the Bow City structure being the remnant of a deeply eroded, complex impact structure. Accordingly, the Bow City structure may provide rare access and insight into zones of deformation remaining beneath an excavated transient crater in stratified siliciclastic target rocks.

  19. Reconstructing the Guitar: Blowing Bubbles with a Pulsar Bow Shock Backflow

    NASA Astrophysics Data System (ADS)

    van Kerkwijk, Marten H.; Ingle, Ashleigh

    2008-08-01

    The Guitar Nebula is an Hα nebula produced by the interaction of the relativistic wind of a very fast pulsar, PSR B2224+65, with the interstellar medium. It consists of a ram-pressure confined bow shock near its head and a series of semicircular bubbles further behind, the two largest of which form the body of the Guitar. We present a scenario in which this peculiar morphology is due to instabilities in the backflow from the pulsar bow shock. From simulations, these backflows appear similar to jets and their kinetic energy is a large fraction of the total energy in the pulsar's relativistic wind. We suggest that, like jets, these flows become unstable some distance downstream, leading to rapid dissipation of the kinetic energy into heat, and the formation of an expanding bubble. We show that in this scenario the sizes, velocities, and surface brightnesses of the bubbles depend mostly on observables, and that they match roughly what is seen for the Guitar. Similar instabilities may account for features seen in other bow shocks.

  20. The multifrequency parsec-scale structure of PKS 2254-367 (IC 1459): a luminosity-dependent break in morphology for the precursors of radio galaxies?

    NASA Astrophysics Data System (ADS)

    Tingay, S. J.; Edwards, P. G.

    2015-03-01

    We present the first multifrequency very long baseline interferometry (VLBI) images of PKS 2254-367, a gigahertz-peaked spectrum (GPS) radio source hosted by the nearby galaxy IC 1459 (D = 20.5 Mpc). PKS 2254-367 and the radio source in NGC 1052 (PKS 0238-084; D = 17.2 Mpc) are the two closest GPS radio sources to us, far closer than the next closest example, PKS 1718-649 (D = 59 Mpc). As such, IC 1459 and NGC 1052 offer opportunities to study the details of the parsec-scale radio sources as well as the environments that the radio sources inhabit, across the electromagnetic spectrum. Given that some models for the origin and evolution of GPS radio sources require a strong connection between the radio source morphology and the gaseous nuclear environment, such opportunities for detailed study are important. Our VLBI images of PKS 2254-367 show that the previously identified similarities between IC 1459 and NGC 1052 continue on to the parsec-scale. Both compact radio sources appear to have symmetric jets of approximately the same luminosity, much lower than typically noted in compact double GPS sources. Similarities between PKS 2254-367 and NGC 1052, and differences with respect to other GPS galaxies, lead us to speculate that a sub-class of GPS radio sources, with low luminosity and with jet-dominated morphologies, exists and would be largely absent from radio source surveys with ˜1 Jy flux density cut-offs. We suggest that this possible low-luminosity, jet-dominated population of GPS sources could be an analogue of the Fanaroff-Riley type I (FR I) radio galaxies, with the higher luminosity lobe-dominated GPS sources being the analogue of the FR II radio galaxies.

  1. Fermi-LAT detection of a GeV gamma-ray flare from the blazar PKS 1313-333

    NASA Astrophysics Data System (ADS)

    Ciprini, Stefano

    2016-01-01

    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 1313-333 (also known as TXS 1313-333, OP -322, 2EG J1314-3430 and 3FGL J1316.0-3338), with radio counterpart position R.A.: 199.033275 deg, Dec.: -33.64977 deg, (J2000.0, Johnston et al. 1995, AJ, 110, 880) and with redshift z=1.210 (Jauncey et al. 1982, AJ, 87, 763).

  2. Evidence for quasi-periodic oscillations in the optical polarization of the blazar PKS 2155-304

    NASA Astrophysics Data System (ADS)

    Pekeur, N. W.; Taylor, A. R.; Potter, S. B.; Kraan-Korteweg, R. C.

    2016-10-01

    Evidence for the presence of quasi-periodic oscillations (QPOs) in the optical polarization of the blazar PKS 2155-304, during a period of enhanced gamma-ray brightness, is presented. The periodogram of the polarized flux revealed the existence of a prominent peak at T ˜ 13 min, detected at >99.7 per cent significance, and T ˜ 30 min, which was nominally significant at >99 per cent. This is the first evidence of QPOs in the polarization of an active galactic nucleus, potentially opening up a new avenue of studying this phenomenon.

  3. Enormous Disc of Cool Gas Surrounding the Nearby Powerful Radio Galaxy NGC 612 (PKS 0131-36)

    DTIC Science & Technology

    2008-05-22

    scale H I disc (MHI = 1.5 × 10 10M⊙ and diameter = 127 kpc for H0 = 71 km s −1 Mpc−1) is the early-type galaxy PKS 1718-649 ( Veron -Cetty et al. 1995...99, 1781 Véron-Cetty M. P., Véron P., 2001, A&A, 375, 791 Veron -Cetty M.-P., Woltjer L., Ekers R. D., Staveley-Smith L., 1995, A&A, 297, L79+ Wall

  4. Broadband Spectral Modeling of the Extreme Gigahertz-peaked Spectrum Radio Source PKS B0008-421

    NASA Astrophysics Data System (ADS)

    Callingham, J. R.; Gaensler, B. M.; Ekers, R. D.; Tingay, S. J.; Wayth, R. B.; Morgan, J.; Bernardi, G.; Bell, M. E.; Bhat, R.; Bowman, J. D.; Briggs, F.; Cappallo, R. J.; Deshpande, A. A.; Ewall-Wice, A.; Feng, L.; Greenhill, L. J.; Hazelton, B. J.; Hindson, L.; Hurley-Walker, N.; Jacobs, D. C.; Johnston-Hollitt, M.; Kaplan, D. L.; Kudrayvtseva, N.; Lenc, E.; Lonsdale, C. J.; McKinley, B.; McWhirter, S. R.; Mitchell, D. A.; Morales, M. F.; Morgan, E.; Oberoi, D.; Offringa, A. R.; Ord, S. M.; Pindor, B.; Prabu, T.; Procopio, P.; Riding, J.; Srivani, K. S.; Subrahmanyan, R.; Udaya Shankar, N.; Webster, R. L.; Williams, A.; Williams, C. L.

    2015-08-01

    We present broadband observations and spectral modeling of PKS B0008-421 and identify it as an extreme gigahertz-peaked spectrum (GPS) source. PKS B0008-421 is characterized by the steepest known spectral slope below the turnover, close to the theoretical limit of synchrotron self-absorption, and the smallest known spectral width of any GPS source. Spectral coverage of the source spans from 0.118 to 22 GHz, which includes data from the Murchison Widefield Array and the wide bandpass receivers on the Australia Telescope Compact Array. We have implemented a Bayesian inference model fitting routine to fit the data with internal free-free absorption (FFA), single- and double-component FFA in an external homogeneous medium, FFA in an external inhomogeneous medium, or single- and double-component synchrotron self-absorption models, all with and without a high-frequency exponential break. We find that without the inclusion of a high-frequency break these models cannot accurately fit the data, with significant deviations above and below the peak in the radio spectrum. The addition of a high-frequency break provides acceptable spectral fits for the inhomogeneous FFA and double-component synchrotron self-absorption models, with the inhomogeneous FFA model statistically favored. The requirement of a high-frequency spectral break implies that the source has ceased injecting fresh particles. Additional support for the inhomogeneous FFA model as being responsible for the turnover in the spectrum is given by the consistency between the physical parameters derived from the model fit and the implications of the exponential spectral break, such as the necessity of the source being surrounded by a dense ambient medium to maintain the peak frequency near the gigahertz region. This implies that PKS B0008-421 should display an internal H i column density greater than 1020 cm-2. The discovery of PKS B0008-421 suggests that the next generation of low radio frequency surveys could reveal a

  5. Fermi-LAT detection of a GeV gamma-ray flare from the blazar PKS 0514-459

    NASA Astrophysics Data System (ADS)

    Ciprini, Stefano

    2016-01-01

    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 0514-459 (also known as RX J0515.7-4556 and 3FGL J0515.3-4557), with radio counterpart position R.A.: 78.938767 deg, Dec.: -45.945369 deg (J2000.0, Costa & Loyola 1996, A & AS, 115, 75) and with redshift z=0.194 (Stickel, Kuehr, & Fried 1993, A & AS, 97, 483).

  6. Fermi LAT detection of increasing gamma-ray emission from the radio-loud NLSy1 PKS 1502+036

    NASA Astrophysics Data System (ADS)

    D'Ammando, Filippo; Ciprini, Stefano

    2015-12-01

    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 radio-loud narrow-line Seyfert 1 PKS 1502+036 (also known as 3FGL J1505.1+0326, Acero et al. 2015, ApJS, 218, 23), with radio coordinates (J2000.0), R.A.: 226.2769879 deg, Dec.: 3.4418922 deg (Fey et al. 2004, AJ, 127, 3587) at redshift z = 0.4078 (Hewett & Wild 2010, MNRAS, 405, 2302).

  7. Record cm/mm-band radio flux levels of the gamma-ray flaring blazar PKS 1510-089

    NASA Astrophysics Data System (ADS)

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

    2011-10-01

    Responding to the ATel #3694 reporting the recent flaring activity of PKS 1510-089 at gamma-rays mid of October 2011, we here report its latest behavior at radio bands (cm to mm) as observed by the F-GAMMA program. Previous activity of the source at radio bands have been reported in ATels #3500 and #3523. 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 was following a continuously decaying long-term trend at low to intermediate frequencies, though with smaller "sub-flares" superimposed.

  8. Measurement of bow tie profiles in CT scanners using a real-time dosimeter

    SciTech Connect

    Whiting, Bruce R.; Evans, Joshua D.; Williamson, Jeffrey F.; Dohatcu, Andreea C.; Politte, David G.

    2014-10-15

    Purpose: Several areas of computed tomography (CT) research require knowledge about the intensity profile of the x-ray fan beam that is introduced by a bow tie filter. This information is considered proprietary by CT manufacturers, so noninvasive measurement methods are required. One method using real-time dosimeters has been proposed in the literature. A commercially available dosimeter was used to apply that method, and analysis techniques were developed to extract fan beam profiles from measurements. Methods: A real-time ion chamber was placed near the periphery of an empty CT gantry and the dose rate versus time waveform was recorded as the x-ray source rotated about the isocenter. In contrast to previously proposed analysis methods that assumed a pointlike detector, the finite-size ion chamber received varying amounts of coverage by the collimated x-ray beam during rotation, precluding a simple relationship between the source intensity as a function of fan beam angle and measured intensity. A two-parameter model for measurement intensity was developed that included both effective collimation width and source-to-detector distance, which then was iteratively solved to minimize the error between duplicate measurements at corresponding fan beam angles, allowing determination of the fan beam profile from measured dose-rate waveforms. Measurements were performed on five different scanner systems while varying parameters such as collimation, kVp, and bow tie filters. On one system, direct measurements of the bow tie profile were collected for comparison with the real-time dosimeter technique. Results: The data analysis method for a finite-size detector was found to produce a fan beam profile estimate with a relative error between duplicate measurement intensities of <5%. It was robust over a wide range of collimation widths (e.g., 1–40 mm), producing fan beam profiles that agreed with a relative error of 1%–5%. Comparison with a direct measurement technique on

  9. First Fermi LAT detection of a strong GeV gamma-ray flare from blazar PKS 0403-13

    NASA Astrophysics Data System (ADS)

    Ciprini, Stefano

    2016-07-01

    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 0403-13 (also known as TXS 0403-132, OF -105, RX J0405.5-1308, and 3FGL J0405.5-1307), with radio counterpart position R.A.: 61.391680 deg, Dec.: -13.137136 deg (J2000.0, Fey et al. 2004, AJ, 127, 3587) and with redshift z=0.5706+/-0.0001 (Marziani et al. 1996, ApJS, 104, 37). Preliminary analysis indicates that on 2016 July 11, PKS 0403-13 was in a high state with a daily averaged gamma-ray flux (E > 100 MeV) of (1.6+/-0.3) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only), about 140 times greater than its four-year average flux reported in the third Fermi-LAT source catalog (3FGL, Acero et al. 2015, ApJS, 218, 23). The corresponding daily averaged spectral photon index (E > 100 MeV) of 2.3+/-0.2 (statistical uncertainty only) is compatible with the 3FGL catalog value of 2.35+/-0.11.

  10. A Highly Doppler Blueshifted Fe-K Emission Line in the High-Redshift QSO PKS 2149-306.

    PubMed

    Yaqoob; George; Nandra; Turner; Zobair; Serlemitsos

    1999-11-01

    We report the results from an ASCA observation of the high-luminosity, radio-loud quasar PKS 2149-306 (redshift 2.345), covering the approximately 1.7-30 keV band in the quasar frame. We find the source to have a luminosity approximately 6x1047 ergs s-1 in the 2-10 keV band (quasar frame). We detect an emission line centered at approximately 17 keV in the quasar frame. Line emission at this energy has not been observed in any other active galaxy or quasar to date. We present evidence rejecting the possibility that this line is the result of instrumental artifacts or a serendipitous source. The most likely explanation is blueshifted Fe-K emission (the equivalent width is EW approximately 300+/-200 eV, quasar frame). Bulk velocities of the order of 0.75c are implied by the data. We show that Fe-K line photons originating in an accretion disk and Compton scattering off a leptonic jet aligned along the disk axis can account for the emission line. Curiously, if the emission-line feature recently discovered in another quasar (PKS 0637-752, z=0.654) at 1.6 keV in the quasar frame is due to blueshifted O vii emission, the Doppler blueshifting factor in both quasars is similar ( approximately 2.7-2.8).

  11. DISCOVERY OF VERY HIGH ENERGY GAMMA RAYS FROM PKS 1424+240 AND MULTIWAVELENGTH CONSTRAINTS ON ITS REDSHIFT

    SciTech Connect

    Acciari, V. A.; Benbow, W.; Aliu, E.; Boltuch, D.; Arlen, T.; Chow, Y. C.; Aune, T.; Bautista, M.; Cogan, P.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Boettcher, M.; Bradbury, S. M.; Byrum, K.; Cannon, A.; Cesarini, A.; Ciupik, L.; Cui, W.; Duke, C. E-mail: amy.furniss@gmail.com

    2010-01-10

    We report the first detection of very high energy{sup 83}Gamma-ray emission above 100 GeV. (VHE) gamma-ray emission above 140 GeV from PKS 1424+240, a BL Lac object with an unknown redshift. The photon spectrum above 140 GeV measured by VERITAS is well described by a power law with a photon index of 3.8 {+-} 0.5{sub stat} {+-} 0.3{sub syst} and a flux normalization at 200 GeV of (5.1 {+-} 0.9{sub stat} {+-} 0.5{sub syst}) x 10{sup -11} TeV{sup -1} cm{sup -2} s{sup -1}, where stat and syst denote the statistical and systematical uncertainties, respectively. The VHE flux is steady over the observation period between MJD 54881 and 55003 (from 2009 February 19 to June 21). Flux variability is also not observed in contemporaneous high-energy observations with the Fermi Large Area Telescope. Contemporaneous X-ray and optical data were also obtained from the Swift XRT and MDM observatory, respectively. The broadband spectral energy distribution is well described by a one-zone synchrotron self-Compton model favoring a redshift of less than 0.1. Using the photon index measured with Fermi in combination with recent extragalactic background light absorption models it can be concluded from the VERITAS data that the redshift of PKS 1424+240 is less than 0.66.

  12. Discovery of Very High Energy Gamma Rays from PKS 1424+240 and Multiwavelength Constraints on its Redshift

    SciTech Connect

    Acciari, V.A.; Aliu, E.; Arlen, T.; Aune, T.; Bautista, M.; Beilicke, M. Benbow, W.; Bottcher, M.; Boltuch, D.; Bradbury, S.M.; Buckley, J.H.; Bugaev, V.; Byrum, K.; Cannon, A.; Cesarini, A.; Chow, Y.C.; Ciupik, L.; Cogan, P.; Cui, W.; Duke, C.; Falcone, A.; /more authors..

    2012-04-05

    We report the first detection of very-high-energy (VHE) gamma-ray emission above 140GeV from PKS 1424+240, a BL Lac object with an unknown redshift. The photon spectrum above 140GeV measured by VERITAS is well described by a power law with a photon index of 3.8 {+-}0.5{sub stat} {+-} 0.3{sub syst} and a flux normalization at 200 GeV of (5.1 {+-} 0.9{sub stat} {+-} 0.5{sub syst}) x 10{sup -11} TeV{sup -1} cm{sup -2} s{sup -1}, where stat and syst denote the statistical and systematical uncertainty, respectively. The VHE flux is steady over the observation period between MJD 54881 and 55003 (2009 February 19 to June 21). Flux variability is also not observed in contemporaneous high energy observations with the Fermi Large Area Telescope (LAT). Contemporaneous X-ray and optical data were also obtained from the Swift XRT and MDM observatory, respectively. The broadband spectral energy distribution (SED) is well described by a one-zone synchrotron self-Compton (SSC) model favoring a redshift of less than 0.1. Using the photon index measured with Fermi in combination with recent extragalactic background light (EBL) absorption models it can be concluded from the VERITAS data that the redshift of PKS 1424+240 is less than 0.66.

  13. Polyketide synthase (PKS) reduces fusion of Legionella pneumophila-containing vacuoles with lysosomes and contributes to bacterial competitiveness during infection.

    PubMed

    Shevchuk, Olga; Pägelow, Dennis; Rasch, Janine; Döhrmann, Simon; Günther, Gabriele; Hoppe, Julia; Ünal, Can Murat; Bronietzki, Marc; Gutierrez, Maximiliano Gabriel; Steinert, Michael

    2014-11-01

    L. pneumophila-containing vacuoles (LCVs) exclude endocytic and lysosomal markers in human macrophages and protozoa. We screened a L. pneumophila mini-Tn10 transposon library for mutants, which fail to inhibit the fusion of LCVs with lysosomes by loading of the lysosomal compartment with colloidal iron dextran, mechanical lysis of infected host cells, and magnetic isolation of LCVs that have fused with lysosomes. In silico analysis of the mutated genes, D. discoideum plaque assays and infection assays in protozoa and U937 macrophage-like cells identified well established as well as novel putative L. pneumophila virulence factors. Promising candidates were further analyzed for their co-localization with lysosomes in host cells using fluorescence microscopy. This approach corroborated that the O-methyltransferase, PilY1, TPR-containing protein and polyketide synthase (PKS) of L. pneumophila interfere with lysosomal degradation. Competitive infections in protozoa and macrophages revealed that the identified PKS contributes to the biological fitness of pneumophila strains and may explain their prevalence in the epidemiology of Legionnaires' disease.

  14. Fermi-LAT detection of a GeV gamma-ray flare from the blazar PKS 2023-07

    NASA Astrophysics Data System (ADS)

    Ciprini, Stefano; Fermi Large Area Telescope Collaboration

    2016-04-01

    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 2023-07 (also known as NRAO 629, TXS 2022-077, 3EG J2025-0744, 1AGLR J2027-0747 and 3FGL J2025.6-0736), with radio counterpart position R.A.: 306.419418 deg, Dec.: -7.597969 deg (J2000.0, Beasley et al. 2002, ApJS, 141, 13) and with redshift z=1.388 (Drinkwater et al. 1997, MNRAS, 284, 85). Preliminary analysis indicates that on 2016 April 9, PKS 2023-07 was in a high state with a daily averaged gamma-ray flux (E > 100 MeV) of (2.0+/-0.3) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only), about 16 times greater than its four-year average flux reported in the third Fermi-LAT source catalog (3FGL, Acero et al. 2015, ApJS, 218, 23). The corresponding daily averaged spectral photon index (E > 100 MeV) of 2.4+/-0.2 (statistical uncertainty only) is compatible with the 3FGL catalog value of 2.18+/-0.03.

  15. Multiwavelength monitoring of the BL Lacertae object PKS 2155-304. 4: Multiwavelength analysis

    NASA Technical Reports Server (NTRS)

    Edelson, R.; Krolik, J.; Madejski, G.; Maraschi, L.; Pike, G.; Urry, C. M.; Brinkmann, W.; Courvoisier, T. J.-L.; Ellithorpe, J.; Horne, K.

    1995-01-01

    Simultaneous X-ray, ultraviolet, optical, infrared, and radio monitoring data were used to test and constrain models of continuum emission from the BL Lacertae object PKS 2155-304. Intensively sampled ultraviolet and soft X-ray light curves showed a clear temporal correlation with the X-rays leading the ultraviolet by 2-3 hr. This lag was found to be significantly different from zero after an exhaustive comparison of four different techniques for measuring temporal correlations. Variations in the ultraviolet trough optical wave bands were also strongly correlated, with no measurable lag down to limiting timescales of approximately less than 1-2 hr. This strong correlation extends to the near-infrared, but the less intensive sampling precludes measurement of any lag beyomnd an upper limit of approximately less than 1 day. These lags and limits of the order of hours are much shorter than most rapid observed single-band variations. Because of the very sparse radio sampling, it was not possible to measure quantitatively the correlation and lag with shorter wavelengths, but the data do suggest that the radio may lag the optical/ultraviolet by approximately 1 week, with longer delays and weaker variations to longer radio wavelengths. The epoch-folding Q(exp 2) statistic was used to test for periodicity, and no evidence for strict or quasi-periodicity was found in any of the light curves. Because they lead the lower frequencies, the soft X-rays (approximately less than 1 keV) cannot arise from synchrotron self-Compton scattering. These results also rule out the accretion disk model, which predicts a measurable lag between ultraviolet/optical wavelength bands and a correlation between hardness and brightness, neither of which were seen. They are consistent with the entire radio through X-ray continuum arising from direct synchrotron emission from a relativistic jet. However, the tapered jet model, in which the X-ray emission is produced closer in, has problems explaining

  16. Long-term monitoring of PKS 0537-441 with Fermi-LAT and multiwavelength observations

    NASA Astrophysics Data System (ADS)

    D'Ammando, F.; Antolini, E.; Tosti, G.; Finke, J.; Ciprini, S.; Larsson, S.; Ajello, M.; Covino, S.; Gasparrini, D.; Gurwell, M.; Hauser, M.; Romano, P.; Schinzel, F.; Wagner, S. J.; Impiombato, D.; Perri, M.; Persic, M.; Pian, E.; Polenta, G.; Sbarufatti, B.; Treves, A.; Vercellone, S.; Wehrle, A.; Zook, A.

    2013-05-01

    We report on multiwavelength observations of the blazar PKS 0537-441 (z = 0.896) obtained from microwaves through γ-rays by Submillimeter Array, Rapid Eye Mounting, Automatic Telescope for Optical Monitoring (ATOM), Swift and Fermi mostly during 2008 August-2010 April. Strong variability has been observed in γ-rays, with two major flaring episodes (2009 July and 2010 March) and a harder-when-brighter behaviour, quite common for flat spectrum radio quasars and low-synchrotron-peaked BL Lacertae objects (BL Lacs), in 2010 March. In the same way, the spectral energy distribution (SED) of the source cannot be modelled by a simple synchrotron self-Compton model, as opposed to many BL Lacs, but the addition of an external Compton component of seed photons from a dust torus is needed. The 230 GHz light curve showed an increase simultaneous with the γ-ray one, indicating co-spatiality of the mm and γ-ray emission region likely at large distance from the central engine. The low, average, and high activity SED of the source could be fit changing only the electron distribution parameters, but two breaks in the electron distribution are necessary. The ensuing extra spectral break, located at near-infrared (NIR)-optical frequencies, together with that in γ-rays seem to indicate a common origin, most likely due to an intrinsic feature in the underlying electron distribution. An overall correlation between the γ-ray band with the R band and K band has been observed with no significant time lag. On the other hand, when inspecting the light curves on short time-scales some differences are evident. In particular, flaring activity has been detected in NIR and optical bands with no evident γ-ray counterparts in 2009 September and November. Moderate variability has been observed in X-rays with no correlation between flux and photon index. An increase of the detected X-ray flux with no counterpart at the other wavelengths has been observed in 2008 October, suggesting once more a

  17. Hubble/COS Observations of Intergalactic Gas Toward PKS 0405-123

    NASA Astrophysics Data System (ADS)

    Shull, J. Michael; Danforth, C.; Froning, C.; Green, J.; Keeney, B.; Stocke, J.; Yao, Y.; Savage, B.; Narayanan, A.; Sembach, K.

    2010-01-01

    We present an overview of far-UV Hubble Space Telescope observations (1150-1780 A, at 17 km/s resolution) taken by the Cosmic Origins Spectrograph (COS) of the QSO PKS 0405-123 at redshift zem = 0.5726 and FUV flux 3.5x10-14 erg/s/cm2/A. This spectrum illustrates the the power of COS for studying metal-enriched gas between the galaxies, distributed throughout the multiphase intergalactic medium (IGM). We used 7 orbits with 9 FP-split positions, obtained S/N = 35-45 over much of the G130M band (1150-1440 A), and detected numerous absorption features of hydrogen (Lya, Lyb) and heavy-element probes of metallicity. Ions that can be studied include lines (O VI, N V, Ne VIII) sensitive to hot gas produced by strong shocks produced in gravitational inflows to the Cosmic Web, in circumgalactic gas, and in galactic winds. The high S/N allows a search for broad Ly-alpha possibly associated with O VI in hot gas (105 to 106 K). This sight line also intercepts a high-velocity cloud seen in Si III at 110-170 km/s (LSR) and b = -37.55 in the Galactic halo. In the absorption system at z = 0.495, the Ne VIII doublet (770.41, 780.32 A) shifts into the COS band, allowing us to probe the warm-hot IGM at log T = 5.5-6.0, several times deeper than previous (STIS) studies (Prochaska et al. 2004; Howk et al. 2009). In other posters, members of the COS science team describe the detection of O VI absorbers at redshifts z = 0.16710, 0.18292, 0.36156, 0.36332, and 0.49501, including a Lyman Limit system at z = 0.16710 with log N(HI) = 16.45 +/- 0.05. The high S/N observations allow us to measure important ions previously not detected and to evaluate the kinematical relationships and physical conditions among the detected ions.

  18. Effect of bow-type initial imperfection on the buckling load and mass of graphite-epoxy blade-stiffened panels

    NASA Technical Reports Server (NTRS)

    Stroud, W. J.; Anderson, M. S.; Hennessy, K. W.

    1977-01-01

    A structural synthesis computer code which accounts for first order effects of an initial bow and which can be used for sizing stiffened composite panels having an arbitrary cross section is used to study graphite blade-stiffened panels. The effect of a small initial bow on both the load carrying ability of panels and on the mass of panels designed to carry a specified load is examined. Large reductions in the buckling load caused by a small initial bow emphasize the need for considering a bow when a panel is designed.

  19. An Aspergillus flavus secondary metabolic gene cluster containing a hybrid PKS-NRPS is necessary for synthesis of the 2-pyridones, leporins

    Technology Transfer Automated Retrieval System (TEKTRAN)

    The genome of the filamentous fungus, Aspergillus flavus, has been shown to harbor as many as 55 putative secondary metabolic gene clusters including the one responsible for production of the toxic and carcinogenic, polyketide synthase (PKS)-derived family of secondary metabolites termed aflatoxins....

  20. Phylogeny of type I polyketide synthases (PKSs) in fungal entomopathogens and expression analysis of PKS genes in Beauveria bassiana BCC 2660.

    PubMed

    Punya, Juntira; Swangmaneecharern, Pratchya; Pinsupa, Suparat; Nitistaporn, Pornpen; Phonghanpot, Suranat; Kunathigan, Viyada; Cheevadhanarak, Supapon; Tanticharoen, Morakot; Amnuaykanjanasin, Alongkorn

    2015-06-01

    Entomopathogenic fungi are able to invade and kill insects. Various secondary metabolites can mediate the interaction of a fungal pathogen with an insect host and also help the fungus compete with other microbes. Here we screened 23 isolates of entomopathogenic fungi for polyketide synthase (PKS) genes and amplified 72 PKS gene fragments using degenerate PCR. We performed a phylogenetic analysis of conserved ketosynthase and acyltransferase regions in these 72 sequences and 72 PKSs identified from four insect fungal genome sequences. The resulting genealogy indicated 47 orthologous groups with 99-100 % bootstrap support, suggesting shared biosynthesis of identical or closely related compounds from different fungi. Three insect-specific groups were identified among the PKSs in reducing clades IIa, IIb, and III, which comprised PKSs from 12, 9, and 30 fungal isolates, respectively. A IIa-IIb pair could be found in seven fungi. Expression analyses revealed that eleven out of twelve PKS genes identified in Beauveria bassiana BCC 2660 were expressed in culture. PKS genes from insect-specific clades IIa and IIb were expressed only in insect-containing medium, while others were expressed only in PDB or in CYB, PDB and SDY. The data suggest the potential production of several polyketides in culture.

  1. MASTER-SAAO follow-up to Fermi-LAT detection of FSRQ PKS B1035-281 activity. And OTs

    NASA Astrophysics Data System (ADS)

    Lipunov, V. M.; Buckley, D. A. H.; Shurpakov, S.; Balanutsa, P.; Gress, O.; Gorbovskoy, E.; Tiurina, N.; Kuznetsov, A.; Vladimirov, V.; Kornilov, V.; Vlasenko, D.; Gorbunov, I.; Popova, E.; Kuvshinov, D.; Kniazev, A.; Potter, S. B.; Kotze, M.; Rebolo, R.; Ricart, M. Serra; Israelian, G.; Lodieu, N.

    2016-02-01

    MASTER-SAAO auto-detection system (Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 349171 ) detected the brightening of the FSRQ PKS B1035-281 (RA=10 37 42.457 -28 23 04.11) during inspection of Fermi-LAT Detection of its unusual hard spectrum (Carpenter et al., ATEL #8740).

  2. Identification of a hybrid PKS-NRPS required for the biosynthesis of NG-391 and NG-393 metabolites in Metarhizium anisopliae

    Technology Transfer Automated Retrieval System (TEKTRAN)

    A 19,818 kb genomic region harboring six predicted ORFs was identified in M. anisopliae ARSEF 2575. The ORF4 CDS, putatively encoding a hybrid polyketide synthase/nonribosomal peptide synthetase (PKS-NRPS) was targeted using Agrobacterium-mediated gene knockout. Homologous, but not heterolog...

  3. Application of the global Land-Potential Knowledge System (LandPKS) mobile apps to land degradation, restoration and climate change adaptation

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Combatting land degradation, promoting restoration and adapting to climate change all require an understanding of land potential. A global Land-Potential Knowledge System (LandPKS) is being developed that will address many of these limitations using an open source approach designed to allow anyone w...

  4. Gamma-ray blazar spectra with H.E.S.S. II mono analysis: The case of PKS 2155-304 and PG 1553+113

    NASA Astrophysics Data System (ADS)

    H.E.S.S. Collaboration; Abdalla, H.; Abramowski, A.; Aharonian, F.; Ait Benkhali, F.; Akhperjanian, A. G.; Andersson, T.; Angüner, E. O.; Arrieta, M.; Aubert, P.; Backes, M.; Balzer, A.; Barnard, M.; Becherini, Y.; Becker Tjus, J.; Berge, D.; Bernhard, S.; Bernlöhr, K.; Blackwell, R.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bordas, P.; Brun, F.; Brun, P.; Bryan, M.; Bulik, T.; Capasso, M.; Carr, J.; Casanova, S.; Cerruti, M.; Chakraborty, N.; Chalme-Calvet, R.; Chaves, R. C. G.; Chen, A.; Chevalier, J.; Chrétien, M.; Colafrancesco, S.; Cologna, G.; Condon, B.; Conrad, J.; Couturier, C.; Cui, Y.; Davids, I. D.; Degrange, B.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati-Ataï, A.; Domainko, W.; Donath, A.; Drury, L. O.'C.; Dubus, G.; Dutson, K.; Dyks, J.; Edwards, T.; Egberts, K.; Eger, P.; Ernenwein, J.-P.; Eschbach, S.; Farnier, C.; Fegan, S.; Fernandes, M. V.; Fiasson, A.; Fontaine, G.; Förster, A.; Funk, S.; Füßling, M.; Gabici, S.; Gajdus, M.; Gallant, Y. A.; Garrigoux, T.; Giavitto, G.; Giebels, B.; Glicenstein, J. F.; Gottschall, D.; Goyal, A.; Grondin, M.-H.; Hadasch, D.; Hahn, J.; Haupt, M.; Hawkes, J.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hervet, O.; Hillert, A.; Hinton, J. A.; Hofmann, W.; Hoischen, C.; Holler, M.; Horns, D.; Ivascenko, A.; Jacholkowska, A.; Jamrozy, M.; Janiak, M.; Jankowsky, D.; Jankowsky, F.; Jingo, M.; Jogler, T.; Jouvin, L.; Jung-Richardt, I.; Kastendieck, M. A.; Katarzyński, K.; Katz, U.; Kerszberg, D.; Khélifi, B.; Kieffer, M.; King, J.; Klepser, S.; Klochkov, D.; Kluźniak, W.; Kolitzus, D.; Komin, Nu.; Kosack, K.; Krakau, S.; Kraus, M.; Krayzel, F.; Krüger, P. P.; Laffon, H.; Lamanna, G.; Lau, J.; Lees, J.-P.; Lefaucheur, J.; Lefranc, V.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J.-P.; Leser, E.; Lohse, T.; Lorentz, M.; Liu, R.; López-Coto, R.; Lypova, I.; Marandon, V.; Marcowith, A.; Mariaud, C.; Marx, R.; Maurin, G.; Maxted, N.; Mayer, M.; Meintjes, P. J.; Meyer, M.; Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Morå, K.; Moulin, E.; Murach, T.; de Naurois, M.; Niederwanger, F.; Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka, H.; Öttl, S.; Ohm, S.; Ostrowski, M.; Oya, I.; Padovani, M.; Panter, M.; Parsons, R. D.; Paz Arribas, M.; Pekeur, N. W.; Pelletier, G.; Perennes, C.; Petrucci, P.-O.; Peyaud, B.; Pita, S.; Poon, H.; Prokhorov, D.; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Reimer, A.; Reimer, O.; Renaud, M.; de los Reyes, R.; Rieger, F.; Romoli, C.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Sahakian, V.; Salek, D.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schwanke, U.; Schwemmer, S.; Settimo, M.; Seyffert, A. S.; Shafi, N.; Shilon, I.; Simoni, R.; Sol, H.; Spanier, F.; Spengler, G.; Spies, F.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Stycz, K.; Sushch, I.; Tavernet, J.-P.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tibaldo, L.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Viana, A.; Vincent, P.; Vink, J.; Voisin, F.; Völk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.; Wagner, P.; Wagner, R. M.; White, R.; Wierzcholska, A.; Willmann, P.; Wörnlein, A.; Wouters, D.; Yang, R.; Zabalza, V.; Zaborov, D.; Zacharias, M.; Zdziarski, A. A.; Zech, A.; Zefi, F.; Ziegler, A.; Żywucka, N.; LAT Collaboration; Ackermann, M.; Ajello, M.; Baldini, L.; Barbiellini, G.; Bellazzini, R.; Blandford, R. D.; Bonino, R.; Bregeon, J.; Bruel, P.; Buehler, R.; Caliandro, G. A.; Cameron, R. A.; Caragiulo, M.; Caraveo, P. A.; Cavazzuti, E.; Cecchi, C.; Chiang, J.; Chiaro, G.; Ciprini, S.; Cohen-Tanugi, J.; Costanza, F.; Cutini, S.; D'Ammando, F.; de Palma, F.; Desiante, R.; Di Lalla, N.; Di Mauro, M.; Di Venere, L.; Donaggio, B.; Favuzzi, C.; Focke, W. B.; Fusco, P.; Gargano, F.; Gasparrini, D.; Giglietto, N.; Giordano, F.; Giroletti, M.; Guillemot, L.; Guiriec, S.; Horan, D.; Jóhannesson, G.; Kamae, T.; Kensei, S.; Kocevski, D.; Larsson, S.; Li, J.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Maldera, S.; Manfreda, A.; Mazziotta, M. N.; Michelson, P. F.; Mizuno, T.; Monzani, M. E.; Morselli, A.; Negro, M.; Nuss, E.; Orienti, M.; Orlando, E.; Paneque, D.; Perkins, J. S.; Pesce-Rollins, M.; Piron, F.; Pivato, G.; Porter, T. A.; Principe, G.; Rainò, S.; Razzano, M.; Simone, D.; Siskind, E. J.; Spada, F.; Spinelli, P.; Thayer, J. B.; Torres, D. F.; Torresi, E.; Troja, E.; Vianello, G.; Wood, K. S.

    2017-04-01

    Context. The addition of a 28 m Cherenkov telescope (CT5) to the H.E.S.S. array extended the experiment's sensitivityto lower energies. The lowest energy threshold is obtained using monoscopic analysis of data taken with CT5, providing access to gamma-ray energies below 100 GeV for small zenith angle observations. Such an extension of the instrument's energy range is particularly beneficial for studies of active galactic nuclei with soft spectra, as expected for those at a redshift ≥0.5. The high-frequency peaked BL Lac objects PKS 2155-304 (z = 0.116) and PG 1553+113 (0.43 < z < 0.58) are among the brightest objects in the gamma-ray sky, both showing clear signatures of gamma-ray absorption at E > 100 GeV interpreted as being due to interactions with the extragalactic background light (EBL). Aims: The aims of this work are twofold: to demonstrate the monoscopic analysis of CT5 data with a low energy threshold, and to obtain accurate measurements of the spectral energy distributions (SED) of PKS 2155-304 and PG 1553+113 near their SED peaks at energies ≈100 GeV. Methods: Multiple observational campaigns of PKS 2155-304 and PG 1553+113 were conducted during 2013 and 2014 using the full H.E.S.S. II instrument (CT1-5). A monoscopic analysis of the data taken with the new CT5 telescope was developed along with an investigation into the systematic uncertainties on the spectral parameters which are derived from this analysis. Results: Using the data from CT5, the energy spectra of PKS 2155-304 and PG 1553+113 were reconstructed down to conservative threshold energies of 80 GeV for PKS 2155-304, which transits near zenith, and 110 GeV for the more northern PG 1553+113. The measured spectra, well fitted in both cases by a log-parabola spectral model (with a 5.0σ statistical preference for non-zero curvature for PKS 2155-304 and 4.5σ for PG 1553+113), were found consistent with spectra derived from contemporaneous Fermi-LAT data, indicating a sharp break in the

  5. Phylogeny and Expression Analyses Reveal Important Roles for Plant PKS III Family during the Conquest of Land by Plants and Angiosperm Diversification

    PubMed Central

    Xie, Lulu; Liu, Pingli; Zhu, Zhixin; Zhang, Shifan; Zhang, Shujiang; Li, Fei; Zhang, Hui; Li, Guoliang; Wei, Yunxiao; Sun, Rifei

    2016-01-01

    Polyketide synthases (PKSs) utilize the products of primary metabolism to synthesize a wide array of secondary metabolites in both prokaryotic and eukaryotic organisms. PKSs can be grouped into three distinct classes, types I, II, and III, based on enzyme structure, substrate specificity, and catalytic mechanisms. The type III PKS enzymes function as homodimers, and are the only class of PKS that do not require acyl carrier protein. Plant type III PKS enzymes, also known as chalcone synthase (CHS)-like enzymes, are of particular interest due to their functional diversity. In this study, we mined type III PKS gene sequences from the genomes of six aquatic algae and 25 land plants (1 bryophyte, 1 lycophyte, 2 basal angiosperms, 16 core eudicots, and 5 monocots). PKS III sequences were found relatively conserved in all embryophytes, but not exist in algae. We also examined gene expression patterns by analyzing available transcriptome data, and identified potential cis-regulatory elements in upstream sequences. Phylogenetic trees of dicots angiosperms showed that plant type III PKS proteins fall into three clades. Clade A contains CHS/STS-type enzymes coding genes with diverse transcriptional expression patterns and enzymatic functions, while clade B is further divided into subclades b1 and b2, which consist of anther-specific CHS-like enzymes. Differentiation regions, such as amino acids 196-207 between clades A and B, and predicted positive selected sites within α-helixes in late appeared branches of clade A, account for the major diversification in substrate choice and catalytic reaction. The integrity and location of conserved cis-elements containing MYB and bHLH binding sites can affect transcription levels. Potential binding sites for transcription factors such as WRKY, SPL, or AP2/EREBP may contribute to tissue- or taxon-specific differences in gene expression. Our data shows that gene duplications and functional diversification of plant type III PKS enzymes

  6. GYROSURFING ACCELERATION OF IONS IN FRONT OF EARTH's QUASI-PARALLEL BOW SHOCK

    SciTech Connect

    Kis, Arpad; Lemperger, Istvan; Wesztergom, Viktor; Agapitov, Oleksiy; Krasnoselskikh, Vladimir; Dandouras, Iannis E-mail: Kis.Arpad@csfk.mta.hu

    2013-07-01

    It is well known that shocks in space plasmas can accelerate particles to high energies. However, many details of the shock acceleration mechanism are still unknown. A critical element of shock acceleration is the injection problem; i.e., the presence of the so called seed particle population that is needed for the acceleration to work efficiently. In our case study, we present for the first time observational evidence of gyroresonant surfing acceleration in front of Earth's quasi-parallel bow shock resulting in the appearance of the long-suspected seed particle population. For our analysis, we use simultaneous multi-spacecraft measurements provided by the Cluster spacecraft ion (CIS), magnetic (FGM), and electric field and wave instrument (EFW) during a time period of large inter-spacecraft separation distance. The spacecraft were moving toward the bow shock and were situated in the foreshock region. The results show that the gyroresonance surfing acceleration takes place as a consequence of interaction between circularly polarized monochromatic (or quasi-monochromatic) transversal electromagnetic plasma waves and short large amplitude magnetic structures (SLAMSs). The magnetic mirror force of the SLAMS provides the resonant conditions for the ions trapped by the waves and results in the acceleration of ions. Since wave packets with circular polarization and different kinds of magnetic structures are very commonly observed in front of Earth's quasi-parallel bow shock, the gyroresonant surfing acceleration proves to be an important particle injection mechanism. We also show that seed ions are accelerated directly from the solar wind ion population.

  7. Statistical analysis of diffuse ion events upstream of the Earth's bow shock

    NASA Technical Reports Server (NTRS)

    Trattner, K. J.; Mobius, E.; Scholer, M.; Klecker, B.; Hilchenbach, M.; Luehr, H.

    1994-01-01

    A statistical study of diffuse energetic ion events and their related waves upstream of the Earth's bow shock was performed using data from the Active Magnetospheric Particle Tracer Explorers/Ion Release Module (AMPTE/IRM) satellite over two 5-month periods in 1984 and 1985. The data set was used to test the assumption in the self-consistent model of the upstream wave and particle populations by Lee (1982) that the particle acceleration through hydromagnetic waves and the wave generation are directly coupled. The comparison between the observed wave power and the wave power predicted on the observed energetic particle energy density and solar wind parameters results in a high correlation coefficient of about 0.89. The intensity of diffuse ions falls off approximately exponentially with the distance upstream from the bow shock parallel to the magnetic field with e-folding distances which vary from approximately 3.3 R(sub E) to approximately 11.7 R(sub E) over the energy range from 10 keV/e to 67.3 keV/e for both protons and alpha particles. After normalizing the upstream particle densities to zero bow shock distance by using these exponential variations, a good correlation (0.7) of the density of the diffuse ions with the solar wind density was found. This supports the suggestion that the solar wind is the source of the diffuse ions. Furthermore, the spectral slope of the diffuse ions correlates well with the solar wind velocity component in the direction of the interplanetary magnetic field (0.68 and 0.66 for protons and alpha particles) which concurs with the notion that the solar wind plays an important role in the acceleration of the upstream particles.

  8. Vocal Fold Bowing in Elderly Male Monozygotic Twins: A Case Study

    PubMed Central

    Tanner, Kristine; Sauder, Cara; Thibeault, Susan L.; Dromey, Christopher; Smith, Marshall E.

    2009-01-01

    Objectives This study examined case histories, diagnostic features, and treatment response in two 79-year-old male monozygotic (identical) twins with vocal fold bowing, exploring both genetic and environmental factors. Study Design Case study. Methods DNA concordance was examined via cheek swab. Case histories, videostroboscopy, auditory- and visual-perceptual assessment, electromyography, acoustic measures, and Voice Handicap ratings were undertaken. Both twins underwent surgical intervention and subsequent voice therapy. Results Monozygosity was confirmed for DNA polymorphisms, with 10 of 10 concordance for STR DNA markers. For both twins, auditory and visual-perceptual assessments indicated severe bowing, hoarseness and breathiness, although Twin 1 was judged to be extremely severe. Differences in RMS amplitudes were observed for TA and LCA muscles, with smaller relative amplitudes observed for the Twin 1 versus Twin 2. No consistent voice improvement was observed following surgical intervention(s), despite improved mid-membranous vocal fold closure. Marked reductions in Voice Handicap Index total scores were observed following behavioral voice therapy, coinciding with increased mid-membranous and posterior laryngeal (interarytenoid) glottal closure. No substantive differences in acoustic measures were observed. Conclusions Vocal fold bowing was more severe for Twin 1 versus Twin 2 despite identical heritability factors. Overall voice improvement with treatment was greater for Twin 2 than Twin 1. Environmental factors might partially account for the differences observed between the twins, including variability in their responsiveness to behavioral voice therapy. Voice therapy was useful in improving mid-membranous and posterior laryngeal closure, although dysphonia remained severe in both cases. PMID:19664899

  9. Discovering Massive Runaway Stars with Infrared Bow Shock Nebulae: Four OB Stars Found in WISE

    NASA Astrophysics Data System (ADS)

    Wernke, Heather N.; Kobulnicky, Henry A.; Dale, Daniel A.; Povich, Matthew S.; Andrews, Julian E.; Chick, William T.; Munari, Stephan; Olivier, Grace M.; Schurhammer, Danielle; Sorber, Rebecca L.

    2016-01-01

    Supernovae, pulsars, and gamma-ray bursts are examples of the result of the death of massive (late-O and early-B type) stars. Determining stellar mass loss rates can help us predict the type of death the star will endure. We focus on stars that are located at the center of an infrared bow shock nebula, indicating that the star was flung from its birthplace at supersonic speed. Observing these massive, high-velocity, runaway stars with bow shock nebulae to determine their spectral type will help in the measurements of their stellar mass loss rates. The spectra of four OB stars driving bow shock candidates are presented. These four candidates were found by searching through the Wide-field Infrared Survey Explorer (WISE) All-Sky Data Release and were the most visible in the WISE 21µm band. The spectrum for each star was obtained with the Longslit Spectrograph at the Wyoming Infrared Observatory (WIRO). The spectral types of G077.3617+01.16 (HD 229159), G079.8219+00.096 ([CPR2002]A10), G092.7265+00.18, and G076.0752-02.2044 (TYC 2697-1046-1) were found to be B1.0I, O9.0V, B0.0V, and B0.0V respectively. As predicted, the candidates are all either late-O or early-B type stars. Now that the spectral types of these stars are known, further analysis can be done to determine the velocities, temperatures, masses, and stellar mass loss rates.This work is supported by the National Science Foundation under grants AST-1063146 (REU), AST-1411851 (RUI), and AST-1412845.

  10. EVOLUTION OF THE PARSEC-SCALE STRUCTURE OF PKS 1934-638 REVISITED: FIRST SCIENCE WITH THE ASKAP AND NEW ZEALAND TELESCOPES

    SciTech Connect

    Tzioumis, A. K.; Reynolds, J. E.; Phillips, C. J.; Amy, S. W.; Edwards, P. G.; Bowen, M. A.; Leach, M. R.; Kesteven, M. J.; Chung, Y.; Stevens, J.; Forsyth, A. R.; Tingay, S. J.; Stansby, B.; Macquart, J.-P.; Reynolds, C.; Wayth, R. B.; Bignall, H. E.; Hotan, A.; Gulyaev, S.; Natusch, T.

    2010-11-15

    We have studied the archetypal Gigahertz Peaked Spectrum radio galaxy, PKS 1934 - 638, using the Australian Long Baseline Array augmented with two new telescopes that greatly improve the angular resolution of the array. These very long baseline interferometry observations represent the first scientific results from a new antenna in New Zealand and the first antenna of the Australian SKA Pathfinder. A compact double radio source, PKS 1934 - 638 has been monitored over a period of 40 years and the observation described here provides the latest datum, eight years after the previous observation, to aid in the study of the long-term evolution of the source structure. We take advantage of these new long baselines to probe PKS 1934 - 638 at the relatively low frequency of 1.4 GHz in order to examine the effects of optical depth on the structure of the radio source. Optical depth effects, resulting in the observation of frequency-dependent structure, may have previously been interpreted in terms of an expansion of the source as a function of time. Expansion and frequency-dependent effects are important to disentangle in order to estimate the age of PKS 1934 - 638. We show that frequency-dependent structure effects are likely to be important in PKS 1934 - 638 and present a simple two-dimensional synchrotron source model in which opacity effects due to synchrotron self-absorption are taken into account. Evidence for expansion of the radio source over 40 years is therefore weak with consequences for the estimated age of the radio source.

  11. Optimization of Bow-Bulb Forms for Resistance and Seakeeping Characteristics.

    DTIC Science & Technology

    2014-09-26

    effort looked into _J the effects of a bow bulb similar to that found on the Italian frigate, - .2 • ---- au ab. ., I.,Wm .,.I._ , dm ~m,,m~m~~u...the other assumes the transom is completely dry . Since the model tests showed that the transom stern of the FFG-7 was dry at all speeds above 16 knots...curves represents the uncertainty " .] which is present in the transition from the wet transom to a dry stern. From these curves, the EHP ratio

  12. Plasma wave system measurements of the Martian bow shock from the Phobos 2 spacecraft

    SciTech Connect

    Trotignon, J.G. ); Grard, R. ); Savin, S. )

    1991-07-01

    The high-resolution data of the electric field observations performed by the plasma wave system (PWS) during some of the Martian bow shock intersections by Phobos 2 were analyzed. Plasma and wave detectors are very useful instruments for locating the shock transition region and studying structures in the upstream region, such as the foot or the electron foreshock. The electron plasma oscillations that develop in the latter give access to the plasma density of the solar wind. Shock surface models derived from the PWS data are compared to those obtained by other authors, and attention is paid to similarities and differences between the electric field measurements obtained for Mars, Venus, and Earth

  13. Primary task-specific bowing tremor: an entity of its own?

    PubMed

    Lee, André; Altenmüller, Eckart

    2012-12-01

    A professional violinist in his early 60s, playing in a prestigious German orchestra for more than 20 years, presented to our institute because of a task-induced tremor in his right arm when playing the violin. We describe the phenomenology of this tremor and its treatment options and compare it to findings in primary writing tremor (PWT). We then discuss whether primary bowing tremor is an entity of its own (similar to PWT) and propose hypotheses that would derive from such a definition.

  14. Interplanetary magnetic field control of the Venus magnetosheath field and bow shock location

    NASA Technical Reports Server (NTRS)

    Phillips, J. L.; Luhmann, J. G.; Russell, C. T.; Alexander, C. J.

    1986-01-01

    Six Venus years of Pioneer Venus Orbiter (PVO) data are analyzed in a coordinate system which isolates magnetic effects. The field draping pattern features two lobes easily identifiable even in the near planet region. The magnetosheath magnetic magnitude has a hemispherical asymmetry controlled by the IMF orientation in a manner suggesting preferrential ion pickup in one hemisphere. This result complements recent findings that the bow shock position is responsive to IMF direction. Examination of the ionopause position to evaluate ionospheric effects on the overall asymmetry of thfe Venus-solar wind interaction produces negative but not conclusive results.

  15. Homotopy method for inverse design of the bulbous bow of a container ship

    NASA Astrophysics Data System (ADS)

    Huang, Yu-jia; Feng, Bai-wei; Hou, Guo-xiang; Gao, Liang; Xiao, Mi

    2017-03-01

    The homotopy method is utilized in the present inverse hull design problem to minimize the wave-making coefficient of a 1300 TEU container ship with a bulbous bow. Moreover, in order to improve the computational efficiency of the algorithm, a properly smooth function is employed to update the homotopy parameter during iteration. Numerical results show that the homotopy method has been successfully applied in the inverse design of the ship hull. This method has an advantage of high performance on convergence and it is credible and valuable for engineering practice.

  16. 3-D Hybrid Simulation of Quasi-Parallel Bow Shock and Its Effects on the Magnetosphere

    SciTech Connect

    Lin, Y.; Wang, X.Y.

    2005-08-01

    A three-dimensional (3-D) global-scale hybrid simulation is carried out for the structure of the quasi-parallel bow shock, in particular the foreshock waves and pressure pulses. The wave evolution and interaction with the dayside magnetosphere are discussed. It is shown that diamagnetic cavities are generated in the turbulent foreshock due to the ion beam plasma interaction, and these compressional pulses lead to strong surface perturbations at the magnetopause and Alfven waves/field line resonance in the magnetosphere.

  17. Heavy Solar Wind Ion Dynamics at and Downstream from the Bow Shock

    NASA Technical Reports Server (NTRS)

    Dougherty, Virginia M.

    1997-01-01

    This is a contract under the NASA Supporting Research and Technology Program for the analysis and interpretation of the scientific data from the Plasma Composition Experiment on the International Sun Earth Explorer 1 (ISEE-1) spacecraft and the Fast Plasma Experiment on the ISEE-1 and -2 spacecraft. These combined data sets will be used in a comprehensive study of the heavy solar wind ion dynamics at and downstream from the Earth's bow shock. The report summarizes activities during the above period and outlines expected activities during the forthcoming quarter.

  18. Near-field enhanced ultraviolet resonance Raman spectroscopy using aluminum bow-tie nano-antenna

    PubMed Central

    Li, Ling; Fang Lim, Shuang; Puretzky, Alexander A.; Riehn, Robert; Hallen, H. D.

    2012-01-01

    An aluminum bow-tie nano-antenna is combined with the resonance Raman effect in the deep ultraviolet to dramatically increase the sensitivity of Raman spectra to a small volume of material, such as benzene used here. We further demonstrate gradient-field Raman peaks for several strong infrared modes. We achieve a gain of ∼105 in signal intensity from the near field enhancement due to the surface plasmon resonance in the aluminum nanostructure. The on-line resonance enhancement contributes another factor of several thousands, limited by the laser line width. Thus, an overall gain of hundreds of million is achieved. PMID:23066168

  19. Critical experiment tests of bowing and expansion reactivity calculations for LMRS

    SciTech Connect

    Schaefer, R.W.

    1988-01-01

    Experiments done in several LMR-type critical assemblies simulated core axial expansion, core radial expansion and bowing, coolant expansion, and control driveline expansion. For the most part new experimental techniques were developed to do these experiments. Calculations of the experiments basically used design-level methods, except when it was necessary to investigate complexities peculiar to the experiments. It was found that these feedback reactivities generally are overpredicted, but the predictions are within 30% of the experimental values. 14 refs., 2 figs., 4 tabs.

  20. Analytic MHD Theory for Earth's Bow Shock at Low Mach Numbers

    NASA Technical Reports Server (NTRS)

    Grabbe, Crockett L.; Cairns, Iver H.

    1995-01-01

    A previous MHD theory for the density jump at the Earth's bow shock, which assumed the Alfven M(A) and sonic M(s) Mach numbers are both much greater than 1, is reanalyzed and generalized. It is shown that the MHD jump equation can be analytically solved much more directly using perturbation theory, with the ordering determined by M(A) and M(s), and that the first-order perturbation solution is identical to the solution found in the earlier theory. The second-order perturbation solution is calculated, whereas the earlier approach cannot be used to obtain it. The second-order terms generally are important over most of the range of M(A) and M(s) in the solar wind when the angle theta between the normal to the bow shock and magnetic field is not close to 0 deg or 180 deg (the solutions are symmetric about 90 deg). This new perturbation solution is generally accurate under most solar wind conditions at 1 AU, with the exception of low Mach numbers when theta is close to 90 deg. In this exceptional case the new solution does not improve on the first-order solutions obtained earlier, and the predicted density ratio can vary by 10-20% from the exact numerical MHD solutions. For theta approx. = 90 deg another perturbation solution is derived that predicts the density ratio much more accurately. This second solution is typically accurate for quasi-perpendicular conditions. Taken together, these two analytical solutions are generally accurate for the Earth's bow shock, except in the rare circumstance that M(A) is less than or = 2. MHD and gasdynamic simulations have produced empirical models in which the shock's standoff distance a(s) is linearly related to the density jump ratio X at the subsolar point. Using an empirical relationship between a(s) and X obtained from MHD simulations, a(s) values predicted using the MHD solutions for X are compared with the predictions of phenomenological models commonly used for modeling observational data, and with the predictions of a

  1. Treatment of pseudo Class III malocclusion by modified Hawleys appliance with inverted labial bow.

    PubMed

    Negi, K S; Sharma, K R

    2011-01-01

    Pseudo Class III malocclusion is characterized by an anterior crossbite with functional forward mandibular displacement. Various appliances have been devised for early treatment of a pseudo Class III. The aim of this article is to highlight the method of construction and use a simple removable appliance termed as "Modified Hawleys appliance with inverted labial bow" to treat psuedo class III malocclusion in the mixed dentition period. It also emphasizes the importance of differentiating between true Class III and pseudo Class III. This appliance in this type of malocclusion enabled the correction of a dental malocclusion in a few months and therapeutic stability of a mesially positioned mandible encouraging favorable skeletal growth.

  2. The Quatro appliance: a removable aligner with a changeable labial bow.

    PubMed

    Singh, P; Ash, S; Mizrahi, E

    2007-12-01

    Lower labial segment irregularity is a feature that is presenting more frequently as greater emphasis is placed on aesthetics than ever before. The authors report on a removable appliance that is easy to construct and use and is designed to deal with mild labial tooth irregularity. In cases of crowding the aligner can be used in conjunction with inter-proximal stripping. The device incorporates a removable labial bow attached bilaterally to a sliding lock. This lock permits the addition of sectional archwires to the labial part of the appliance. The versatility of the aligner allows round and rectangular wires of different materials and dimensions to be placed with or without bends.

  3. PKS 2005-489 at VHE: four years of monitoring with HESS and simultaneous multi-wavelength observations

    NASA Astrophysics Data System (ADS)

    H.E.S.S. Collaboration; 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.; 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.; 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, 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.; Marandon, V.; Martineau-Huynh, O.; 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.; 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.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; 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.; 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.

    2010-02-01

    Aims: Our aim is to study the very high energy (VHE; E>100 GeV) γ-ray emission from BL Lac objects and the evolution in time of their broad-band spectral energy distribution (SED). Methods: VHE observations of the high-frequency peaked BL Lac object PKS 2005-489 were made with the High Energy Stereoscopic System (HESS) from 2004 through 2007. Three simultaneous multi-wavelength campaigns at lower energies were performed during the HESS data taking, consisting of several individual pointings with the XMM-Newton and RXTE satellites. Results: A strong VHE signal, ~17σ total, from PKS 2005-489 was detected during the four years of HESS observations (90.3 h live time). The integral flux above the average analysis threshold of 400 GeV is ~3% of the flux observed from the Crab Nebula and varies weakly on time scales from days to years. The average VHE spectrum measured from ~300 GeV to ~5 TeV is characterized by a power law with a photon index, Γ = 3.20± 0.16_stat± 0.10_syst. At X-ray energies the flux is observed to vary by more than an order of magnitude between 2004 and 2005. Strong changes in the X-ray spectrum (ΔΓX ≈ 0.7) are also observed, which appear to be mirrored in the VHE band. Conclusions: The SED of PKS 2005-489, constructed for the first time with contemporaneous data on both humps, shows significant evolution. The large flux variations in the X-ray band, coupled with weak or no variations in the VHE band and a similar spectral behavior, suggest the emergence of a new, separate, harder emission component in September 2005. Supported by CAPES Foundation, Ministry of Education of Brazil.Now at Harvard-Smithsonian Center for Astrophysics, Cambridge, USA.Now at W.W. Hansen Experimental Physics Laboratory & Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, USA.

  4. High-energy properties of the high-redshift flat spectrum radio quasar PKS 2149-306

    NASA Astrophysics Data System (ADS)

    D'Ammando, F.; Orienti, M.

    2016-01-01

    We investigate the γ-ray and X-ray properties of the flat spectrum radio quasar PKS 2149-306 at redshift z = 2.345. A strong γ-ray flare from this source was detected by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope satellite in 2013 January, reaching on January 20 a daily peak flux of (301 ± 36) × 10-8 ph cm-2 s-1 in the 0.1-100 GeV energy range. This flux corresponds to an apparent isotropic luminosity of (1.5 ± 0.2) × 1050 erg s-1, comparable to the highest values observed by a blazar so far. During the flare the increase of flux was accompanied by a significant change of the spectral properties. Moreover significant flux variations on a 6-h time-scale were observed, compatible with the light crossing time of the event horizon of the central black hole. The broad-band X-ray spectra of PKS 2149-306 observed by Swift-XRT and NuSTAR are well described by a broken power-law model, with a very hard spectrum (Γ1 ˜ 1) below the break energy, at E break = 2.5-3.0 keV, and Γ2 ˜ 1.4-1.5 above the break energy. The steepening of the spectrum below ˜3 keV may indicate that the soft X-ray emission is produced by the low-energy relativistic electrons. This is in agreement with the small variability amplitude and the lack of spectral changes in that part of the X-ray spectrum observed between the two NuSTAR and Swift joint observations. As for the other high-redshift FSRQ detected by both Fermi-LAT and Swift-BAT, the photon index of PKS 2149-306 in hard X-ray is 1.6 or lower and the average γ-ray luminosity higher than 2 × 1048 erg s-1.

  5. Preliminary report on radioactive conglomerates of Middle Precambrian age in the Sierra Madre and Medicine Bow Mountains of southeastern Wyoming

    USGS Publications Warehouse

    Houston, Robert Stroud; Graff, P.J.; Karlstrom, K.E.; Root, Forrest

    1977-01-01

    Middle Precambrian miogeosynclinal metasedimentary rocks o# the Sierra Madre and Medicine Bow Mountains of southeastern Wyoming contain radioactive quartz-pebble conglomerates of possible economic interest. These conglomerates do not contain ore-grade uranium in surface outcrops, but an earlier report on the geochemistry of the Arrastre Lake area of the Medicine Bow Mountains shows that ore-grade deposits may be present in the subsurface. This report describes the stratigraphy of the host metasedimentary rocks and the stratigraphic setting of the radioactive conglomerates in both the Sierra Madre and Medicine Bow Mountains, and compares these rock units with those of the Blind River-Elliot Lake uranium district in Canada. The location of radioactive .conglomerates is given so that further exploration may be undertaken by interested parties.

  6. Comparison of theory with atomic oxygen 130.4 nm radiation data from the Bow Shock ultraviolet 2 rocket flight

    NASA Technical Reports Server (NTRS)

    Levin, Deborah A.; Candler, Graham V.; Collins, Robert J.; Howlett, Carl L.; Espy, Patrick; Whiting, Ellis; Park, Chul

    1993-01-01

    Comparison is made between the results obtained from a state-of-the-art flow and radiative model and bow shock vacuum ultraviolet (VUV) data obtained the recent Bow Shock 2 Flight Experiment. An extensive data set was obtained from onboard rocket measurements at a reentry speed of 5 km/sec between the altitudes of approximately 65-85 km. A description of the NO photoionization cell used, the data, and the interpretation of the data will be presented. The primary purpose of the analyses is to assess the utility of the data and to propose a radiation model appropriate to the flight conditions of Bow Shock 2. Theoretical predictions based on flow modeling discussed in earlier work and a new radiation model are compared with data.

  7. Correlated observations of energetic particles upstream of the bow shock, in the magnetosheath, and in the magnetosphere

    SciTech Connect

    Scholer, M.; Moebius, E.; Kistler, L.M. ); Ipavich, F.M.

    1990-12-01

    Simultaneous measurements of energetic protons and alpha particles by the ISEE 1 and AMPTE/IRM spacecraft in the region upstream of the Earth's bow shock are reported during the period 0700-0900 UT on October 19, 1984. IRM observes a diffuse distribution over the whole two hour period. In the spacecraft frame an anisotropy exists with more particles streaming toward the bow shock. ISEE 1 observes occasional bursts of energetic ions which exhibit a beam like distribution along the magnetic field away from the bow shock. The occurrence of these beams is in most cases correlated with a change of the longitudinal interplanetary magnetic field direction, such that a field line from the position of the spacecraft meets the shock with a smaller angle between magnetic field and shock normal. The differential intensity at IRM is about one order of magnitude higher than at ISEE 1. Simultaneously measured spectra by AMPTE/CCE within the magnetosphere close to the magnetopause are considerably harder than the spectra at both upstream locations. A comparison of a CCE spectrum in the magnetosheath with an upstream IRM spectrum shows that the proton intensity observed just outside of the magnetopause between 15 and 80 keV is lower than the upstream spectrum. In the magnetosheath the protons stream away from the bow shock toward the magnetopause and the anisotropy increases with energy. Predictions of the magnetospheric leakage model and of the bow shock acceleration model are compared, and it is shown that the observations are consistent with bow shock acceleration, whereas there are extreme difficulties with an explanation in terms of magnetospheric leakage.

  8. A new technique to characterize CT scanner bow-tie filter attenuation and applications in human cadaver dosimetry simulations

    PubMed Central

    Li, Xinhua; Shi, Jim Q.; Zhang, Da; Singh, Sarabjeet; Padole, Atul; Otrakji, Alexi; Kalra, Mannudeep K.; Xu, X. George; Liu, Bob

    2015-01-01

    Purpose: To present a noninvasive technique for directly measuring the CT bow-tie filter attenuation with a linear array x-ray detector. Methods: A scintillator based x-ray detector of 384 pixels, 307 mm active length, and fast data acquisition (model X-Scan 0.8c4-307, Detection Technology, FI-91100 Ii, Finland) was used to simultaneously detect radiation levels across a scan field-of-view. The sampling time was as short as 0.24 ms. To measure the body bow-tie attenuation on a GE Lightspeed Pro 16 CT scanner, the x-ray tube was parked at the 12 o’clock position, and the detector was centered in the scan field at the isocenter height. Two radiation exposures were made with and without the bow-tie in the beam path. Each readout signal was corrected for the detector background offset and signal-level related nonlinear gain, and the ratio of the two exposures gave the bow-tie attenuation. The results were used in the geant4 based simulations of the point doses measured using six thimble chambers placed in a human cadaver with abdomen/pelvis CT scans at 100 or 120 kV, helical pitch at 1.375, constant or variable tube current, and distinct x-ray tube starting angles. Results: Absolute attenuation was measured with the body bow-tie scanned at 80–140 kV. For 24 doses measured in six organs of the cadaver, the median or maximum difference between the simulation results and the measurements on the CT scanner was 8.9% or 25.9%, respectively. Conclusions: The described method allows fast and accurate bow-tie filter characterization. PMID:26520720

  9. A new technique to characterize CT scanner bow-tie filter attenuation and applications in human cadaver dosimetry simulations

    SciTech Connect

    Li, Xinhua; Shi, Jim Q.; Zhang, Da; Singh, Sarabjeet; Padole, Atul; Otrakji, Alexi; Kalra, Mannudeep K.; Liu, Bob; Xu, X. George

    2015-11-15

    Purpose: To present a noninvasive technique for directly measuring the CT bow-tie filter attenuation with a linear array x-ray detector. Methods: A scintillator based x-ray detector of 384 pixels, 307 mm active length, and fast data acquisition (model X-Scan 0.8c4-307, Detection Technology, FI-91100 Ii, Finland) was used to simultaneously detect radiation levels across a scan field-of-view. The sampling time was as short as 0.24 ms. To measure the body bow-tie attenuation on a GE Lightspeed Pro 16 CT scanner, the x-ray tube was parked at the 12 o’clock position, and the detector was centered in the scan field at the isocenter height. Two radiation exposures were made with and without the bow-tie in the beam path. Each readout signal was corrected for the detector background offset and signal-level related nonlinear gain, and the ratio of the two exposures gave the bow-tie attenuation. The results were used in the GEANT4 based simulations of the point doses measured using six thimble chambers placed in a human cadaver with abdomen/pelvis CT scans at 100 or 120 kV, helical pitch at 1.375, constant or variable tube current, and distinct x-ray tube starting angles. Results: Absolute attenuation was measured with the body bow-tie scanned at 80–140 kV. For 24 doses measured in six organs of the cadaver, the median or maximum difference between the simulation results and the measurements on the CT scanner was 8.9% or 25.9%, respectively. Conclusions: The described method allows fast and accurate bow-tie filter characterization.

  10. Revisiting Quasi-periodic Modulation in γ-Ray Blazar PKS 2155-304 with Fermi Pass 8 Data

    NASA Astrophysics Data System (ADS)

    Zhang, Peng-fei; Yan, Da-hai; Liao, Neng-hui; Wang, Jian-cheng

    2017-02-01

    We examine the gamma-ray quasi-periodic variability of PKS 2155-304 with the latest publicly available Fermi-LAT Pass 8 data, which covers the years from 2008 August to 2016 October. We produce the light curves in two ways: the exposure-weighted aperture photometry and the maximum likelihood optimization. The light curves are then analyzed by using Lomb-Scargle Periodogram (LSP) and Weighted Wavelet Z-transform, and the results reveal a significant quasi-periodicity with a period of 1.74 ± 0.13 years and a significance of ∼4.9σ. The constraint of multifrequencies quasi-periodic variabilities on blazar emission model is discussed.

  11. The spatial extent of the z = 2. 04 absorber in the spectrum of PKS 0458-020

    SciTech Connect

    Briggs, F.H.; Wolfe, A.M.; Liszt, H.S.; Davis, M.M.; Turner, K.L.; Mount Wilson and Las Campanas Observatories, Pasadena, CA; National Radio Astronomy Observatory, Charlottesville, VA )

    1989-06-01

    Radio observations of the z = 2.29 QSO PKS 0458-020 are presented which probe the spatial extent of the gas that gives rise to damped Ly-alpha and 21 cm absorption lines at z = 2.04. Previous observations suggest an extended H I disk that would cover the large-scale structure of the background radio source, and are also consistent with smaller configurations of gas that only cover the compact core of the source. VLBI data of the line and continuum are presented which rule out small configurations such as dwarf galaxies or isolated, gravitationally bound clouds. Rather, the evidence points to an extended disklike structure with a radius of curvature larger than (8/h)kpc, where h = H(0)/100 km/s/Mpc. 21 refs.

  12. Detection of high-energy gamma rays from quasar PKS 0528 + 134 by EGRET on the Compton Gamma Ray Observatory

    NASA Technical Reports Server (NTRS)

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

    1993-01-01

    The first several pointing directions of the Compton Gamma Ray Observatory, launched on 1991 April 5, were toward the Galactic anticenter. In addition to the known gamma-ray sources, Crab and Geminga, high-energy gamma-ray emission was observed from the quasar PKS 0528 + 134 by the Energetic Gamma Ray Experiment Telescope (EGRET). A redshift measurement, reported here, of 2.07 confirms the identification of this object as a quasar. The differential photon spectrum is well represented by a power law with an exponent of 2.56 +/- 0.09 and a photon intensity above 100 MeV of (8.4 +/- 1.0) x 10 exp -7 photons sq cm/s. There is evidence for time variability on a time scale of a few days.

  13. The New Surprising Behaviour of the Two 'Prototype' Blazars PKS 2155-304 and 3C 279

    SciTech Connect

    Costamante, Luigi; Aharonian, Felix; Buhler, Rolf; Khangulyan, Dmitry; Reimer, Anita; Reimer, Olaf; /Stanford U., HEPL /KIPAC, Menlo Park

    2011-11-21

    Recent VHE observations have unveiled a surprising behaviour in two well-known blazars at opposite sides of the blazar sequence. PKS 2155-304 have shown for the first time in an HBL a large Compton dominance, high {gamma}-ray luminosities and a cubic relation between X-ray and VHE fluxes. 3C 279 is the first FSRQ detected at VHE. The high luminosity required to overcome the significant absorption caused by the BLR emission cannot be easily reconciled with the historical and quasi-simultaneous SED properties. Both cases shed a new light on the structure and ambient fields of blazars. Contrary to previous claims, it is also shown that 3C 279 - as any FSRQ - cannot provide robust constraints on the EBL.

  14. Discovery of neutral hydrogen 21 centimeter absorption at redshift 0.25 toward PKS 1413+135

    NASA Technical Reports Server (NTRS)

    Carilli, C. L.; Perlman, Eric S.; Stocke, John T.

    1992-01-01

    A strong H I 21-cm absorption line is identified toward PKS 1413+135 at the redshift of the host galaxy and argued to indicate that the IR-optical cutoff of the BL Lac object's spectrum is caused by extinction. The BL Lac object is shown to have strong neutral 21-cm absorption at the redshift range z = 0.24671 +/- 0.00001, and the implied H I column density is derived. The H I covering factor is assumed to be not more than 0.1, suggesting that a high degree of extinction exists in the galaxy. The host galaxy is theorized to be a spiral of type later than S0 based on the redshift of the H I absorption line and the host. The statistical and observational conclusions are found to support the theories of Stock et al. (1992) regarding the red spectrum of the object.

  15. A hydrodynamical model for the Fermi-LAT γ-ray light curve of blazar PKS 1510-089

    NASA Astrophysics Data System (ADS)

    Cabrera, J. I.; Coronado, Y.; Benítez, E.; Mendoza, S.; Hiriart, D.; Sorcia, M.

    2013-12-01

    A physical description of the formation and propagation of working surfaces inside the relativistic jet of the blazar PKS 1510-089 are used to model its γ -ray variability light curve using Fermi-LAT data from 2008 to 2012. The physical model is based on conservation laws of mass and momentum at the working surface as explained by Mendoza et al. (2009). The hydrodynamical description of a working surface is parametrized by the initial velocity and mass injection rate at the base of the jet. We show that periodic variations on the injected velocity profiles are able to account for the observed luminosity, fixing model parameters such as mass ejection rates of the central engine injected at the base of the jet, oscillation frequencies of the flow and maximum Lorentz factors of the bulk flow during a particular burst.

  16. On nonstationarity and rippling of the quasiperpendicular zone of the Earth bow shock: Cluster observations

    NASA Astrophysics Data System (ADS)

    Lobzin, V. V.; Krasnoselskikh, V. V.; Musatenko, K.; Dudok de Wit, T.

    2008-09-01

    A new method for remote sensing of the quasiperpendicular part of the bow shock surface is presented. The method is based on analysis of high frequency electric field fluctuations corresponding to Langmuir, upshifted, and downshifted oscillations in the electron foreshock. Langmuir waves usually have maximum intensity at the upstream boundary of this region. All these waves are generated by energetic electrons accelerated by quasiperpendicular zone of the shock front. Nonstationary behavior of the shock, in particular due to rippling, should result in modulation of energetic electron fluxes, thereby giving rise to variations of Langmuir waves intensity. For upshifted and downshifted oscillations, the variations of both intensity and central frequency can be observed. For the present study, WHISPER measurements of electric field spectra obtained aboard Cluster spacecraft are used to choose 48 crossings of the electron foreshock boundary with dominating Langmuir waves and to perform for the first time a statistical analysis of nonstationary behavior of quasiperpendicular zone of the Earth's bow shock. Analysis of hidden periodicities in plasma wave energy reveals shock front nonstationarity in the frequency range 0.33 fBi

  17. Numerical modeling of a glow discharge through a supersonic bow shock in air

    NASA Astrophysics Data System (ADS)

    Rassou, S.; Packan, D.; Elias, P.-Q.; Tholin, F.; Chemartin, L.; Labaune, J.

    2017-03-01

    The interaction between a glow discharge and the bow shock of a Mach 3 air flow around a truncated conical model with a central spike is modeled, and comparison is made with prior experimental results. The KRONOS workflow for plasma modeling in flow fields, which has recently been developed at ONERA, was used for the modeling. Based on the quasi-neutral approximation, it couples hypersonic and reactive flow fields with electron chemistry, including the effect of non-Maxwellian electron energy distribution function. The model used for the discharge involves 12 species and 82 reactions, including ionization, electronic and vibrational excitation, and attachment. The simulations reproduce the main features of the discharge observed experimentally well, in particular, the very recognizable topology of the discharge. It was found from the simulations that behind the bow shock, in the afterglow, the negative ion flow ensures the electrical conduction and the establishment of the glow discharge. The influence of kinetic rates on the voltage-current characteristics is discussed.

  18. Diversity of sponges (Porifera) from cryptic habitats on the Belize barrier reef near Carrie Bow Cay.

    PubMed

    Rützler, Klaus; Piantoni, Carla; Van Soest, Rob W M; Díaz, M Cristina

    2014-05-29

    The Caribbean barrier reef near Carrie Bow Cay, Belize, has been a focus of Smithsonian Institution (Washington) reef and mangrove investigations since the early 1970s. Systematics and biology of sponges (Porifera) were addressed by several researchers but none of the studies dealt with cryptic habitats, such as the shaded undersides of coral rubble, reef crevices, and caves, although a high species diversity was recognized and samples were taken for future reference and study. This paper is the result of processing samples taken between 1972 and 2012. In all, 122 species were identified, 14 of them new (including one new genus). The new species are Tetralophophora (new genus) mesoamericana, Geodia cribrata, Placospongia caribica, Prosuberites carriebowensis, Timea diplasterina, Timea oxyasterina, Rhaphidhistia belizensis, Wigginsia curlewensis, Phorbas aurantiacus, Myrmekioderma laminatum, Niphates arenata, Siphonodictyon occultum, Xestospongia purpurea, and Aplysina sciophila. We determined that about 75 of the 122 cryptic sponge species studied (61%) are exclusive members of the sciophilic community, 47 (39 %) occur in both, light-exposed and shaded or dark habitats. Since we estimate the previously known sponge population of Carrie Bow reefs and mangroves at about 200 species, the cryptic fauna makes up 38 % of total diversity.

  19. Investigation of radiative bow-shocks in magnetically accelerated plasma flows

    SciTech Connect

    Bott-Suzuki, S. C. Caballero Bendixsen, L. S.; Cordaro, S. W.; Blesener, I. C.; Hoyt, C. L.; Cahill, A. D.; Kusse, B. R.; Hammer, D. A.; Gourdain, P. A.; Seyler, C. E.; Greenly, J. B.; Chittenden, J. P.; Niasse, N.; Lebedev, S. V.; Ampleford, D. J.

    2015-05-15

    We present a study of the formation of bow shocks in radiatively cooled plasma flows. This work uses an inverse wire array to provide a quasi-uniform, large scale hydrodynamic flow accelerated by Lorentz forces to supersonic velocities. This flow impacts a stationary object placed in its path, forming a well-defined Mach cone. Interferogram data are used to determine a Mach number of ∼6, which may increase with radial position suggesting a strongly cooling flow. Self-emission imaging shows the formation of a thin (<60 μm) strongly emitting shock region, where T{sub e} ∼ 40–50 eV, and rapid cooling behind the shock. Emission is observed upstream of the shock position which appears consistent with a radiation driven phenomenon. Data are compared to 2-dimensional simulations using the Gorgon MHD code, which show good agreement with the experiments. The simulations are also used to investigate the effect of magnetic field in the target, demonstrating that the bow-shocks have a high plasma β, and the influence of B-field at the shock is small. This consistent with experimental measurement with micro bdot probes.

  20. Compound semiconductor alloys: From atomic-scale structure to bandgap bowing

    NASA Astrophysics Data System (ADS)

    Schnohr, C. S.

    2015-09-01

    Compound semiconductor alloys such as InxGa1-xAs, GaAsxP1-x, or CuInxGa1-xSe2 are increasingly employed in numerous electronic, optoelectronic, and photonic devices due to the possibility of tuning their properties over a wide parameter range simply by adjusting the alloy composition. Interestingly, the material properties are also determined by the atomic-scale structure of the alloys on the subnanometer scale. These local atomic arrangements exhibit a striking deviation from the average crystallographic structure featuring different element-specific bond lengths, pronounced bond angle relaxation and severe atomic displacements. The latter, in particular, have a strong influence on the bandgap energy and give rise to a significant contribution to the experimentally observed bandgap bowing. This article therefore reviews experimental and theoretical studies of the atomic-scale structure of III-V and II-VI zincblende alloys and I-III-VI2 chalcopyrite alloys and explains the characteristic findings in terms of bond length and bond angle relaxation. Different approaches to describe and predict the bandgap bowing are presented and the correlation with local structural parameters is discussed in detail. The article further highlights both similarities and differences between the cubic zincblende alloys and the more complex chalcopyrite alloys and demonstrates that similar effects can also be expected for other tetrahedrally coordinated semiconductors of the adamantine structural family.

  1. Jupiter's magnetopause, bow shock, and 10-hour modulated magnetosheath: Voyagers 1 and 2

    NASA Technical Reports Server (NTRS)

    Lepping, R. P.; Burlaga, L. F.; Klein, L. W.

    1980-01-01

    Fine scale magnetic field data from the Voyager 1 and 2 magnetopause and bow shock crossings at Jupiter were analyzed. Explicit models of the dawnside magnetopause and bow shock in Jupiter's orbital plane employ an axisymmetric parabola and hyperbola, respectively, and are determined separately for the encounters. A new phenomenon was discovered in the magnetosheath. It is manifested as (5 or) 10 hour quasi-periodic modulation of the direction of the magnetic field in the outbound magnetosheath, predominantly in the northward (N) and southward (S) directions. It was seen to occur during both encounters and appears most evident in Voyager 2 outbound observations, probably due to the extreme tailward extent of the Voyager 2 trajectory through the magnetosheath. The durations of the N to and from S transitions range from tens of minutes to approximately 3 hours. The directional variation of the field during these transitions is fairly well restricted to a plane parallel to the local model magnetopause location. These signatures may be due to magnetosheath field line draping modulated by the large scale motion of the magnetospheric plasma disk.

  2. COMPUTING THE DUST DISTRIBUTION IN THE BOW SHOCK OF A FAST-MOVING, EVOLVED STAR

    SciTech Connect

    Van Marle, A. J.; Meliani, Z.; Keppens, R.; Decin, L.

    2011-06-20

    We study the hydrodynamical behavior occurring in the turbulent interaction zone of a fast-moving red supergiant star, where the circumstellar and interstellar material collide. In this wind-interstellar-medium collision, the familiar bow shock, contact discontinuity, and wind termination shock morphology form, with localized instability development. Our model includes a detailed treatment of dust grains in the stellar wind and takes into account the drag forces between dust and gas. The dust is treated as pressureless gas components binned per grain size, for which we use 10 representative grain size bins. Our simulations allow us to deduce how dust grains of varying sizes become distributed throughout the circumstellar medium. We show that smaller dust grains (radius <0.045 {mu}m) tend to be strongly bound to the gas and therefore follow the gas density distribution closely, with intricate fine structure due to essentially hydrodynamical instabilities at the wind-related contact discontinuity. Larger grains which are more resistant to drag forces are shown to have their own unique dust distribution, with progressive deviations from the gas morphology. Specifically, small dust grains stay entirely within the zone bound by shocked wind material. The large grains are capable of leaving the shocked wind layer and can penetrate into the shocked or even unshocked interstellar medium. Depending on how the number of dust grains varies with grain size, this should leave a clear imprint in infrared observations of bow shocks of red supergiants and other evolved stars.

  3. Optical hydrogen absorption consistent with a bow shock around the hot Jupiter HD 189733 b

    NASA Astrophysics Data System (ADS)

    Cauley, P. Wilson; Redfield, Seth; Jensen, Adam G.; Barman, Travis; Endl, Michael; Cochran, William D.

    Hot Jupiters, i.e., Jupiter-mass planets with orbital semi major axes of <10 stellar radii, can interact strongly with their host stars. If the planet is moving supersonically through the stellar wind, a bow shock will form ahead of the planet where the planetary magnetosphere slams into the the stellar wind or where the planetary outflow and stellar wind meet. Here we present high resolution spectra of the hydrogen Balmer lines for a single transit of the hot Jupiter HD 189733 b. Transmission spectra of the Balmer lines show strong absorption ~70 minutes before the predicted optical transit, implying a significant column density of excited hydrogen orbiting ahead of the planet. We show that a simple geometric bow shock model is able to reproduce the important features of the absorption time series while simultaneously matching the line profile morphology. Our model suggests a large planetary magnetic field strength of ~28 G. Follow-up observations are needed to confirm the pre-transit signal and investigate any variability in the measurement.

  4. Technical Note: Measurement of bow tie profiles in CT scanners using radiochromic film

    PubMed Central

    Whiting, Bruce R.; Dohatcu, Andreea C.; Evans, Joshua D.; Politte, David G.; Williamson, Jeffrey F.

    2015-01-01

    Purpose: To provide a noninvasive technique to measure the intensity profile of the fan beam in a computed tomography (CT) scanner that is cost effective and easily implemented without the need to access proprietary scanner information or service modes. Methods: The fabrication of an inexpensive aperture is described, which is used to expose radiochromic film in a rotating CT gantry. A series of exposures is made, each of which is digitized on a personal computer document scanner, and the resulting data set is analyzed to produce a self-consistent calibration of relative radiation exposure. The bow tie profiles were analyzed to determine the precision of the process and were compared to two other measurement techniques, direct measurements from CT gantry detectors and a dynamic dosimeter. Results: The radiochromic film method presented here can measure radiation exposures with a precision of ∼6% root-mean-square relative error. The intensity profiles have a maximum 25% root-mean-square relative error compared with existing techniques. Conclusions: The proposed radiochromic film method for measuring bow tie profiles is an inexpensive (∼$100 USD + film costs), noninvasive method to measure the fan beam intensity profile in CT scanners. PMID:26127044

  5. Evolution of the Magnetic Field during Chondrule Formation in Planetary Bow Shocks

    NASA Astrophysics Data System (ADS)

    Mai, Chuhong; Desch, Steven; Boley, Aaron C.

    2016-10-01

    Recent laboratory efforts (Fu et al., 2014, 2015) have constrained the remanent magnetizations of chondrules and the magnetic field strengths they were exposed to as they cooled below their Curie points. An outstanding question is whether these fields represent the background magnetic field of the solar nebula or were unique to the chondrule-forming environment. We investigate the amplification of the magnetic field above background values in a planetary bow shock, which is one proposed mechanism for chondrule formation. We use a hydrodynamic code to model the temperature and pressure around a 3000 km-radius planetary embryo as it moves supersonically through the nebula gas. We calculate the ionization of hot, shocked gas considering thermionic emission of electrons and ions from grains and thermal ionization of potassium. We calculate the magnetic diffusion rate, including Ohmic dissipation and ambipolar diffusion (assuming a magnetic field strength comparable to 0.5 G). We compute the steady-state magnetic field around in the bow shock and find that behind the planet the field is amplified, but everywhere else it quickly diffuses out of the shocked region and recovers the background value. We consider the trajectories taken by chondrules behind the shock and present likely values of the magnetic field amplification experienced by chondrules as they cool after melting in the shock.

  6. Relativistic Electrons Produced by Foreshock Disturbances Observed Upstream of Earth's Bow Shock

    NASA Technical Reports Server (NTRS)

    Wilson, L. B., III; Sibeck, D. G.; Turner, D. L.; Osmane, A.; Caprioli, D.; Angelopoulos, V.

    2016-01-01

    Charged particles can be reflected and accelerated by strong (i.e., high Mach number) astrophysical collisionless shock waves, streaming away to form a foreshock region in communication with the shock. Foreshocks are primarily populated by suprathermal ions that can generate foreshock disturbances-largescale (i.e., tens to thousands of thermal ion Larmor radii), transient (approximately 5-10 per day) structures. They have recently been found to accelerate ions to energies of several keV. Although electrons in Saturn's high Mach number (M > 40) bow shock can be accelerated to relativistic energies (nearly 1000 keV), it has hitherto been thought impossible to accelerate electrons beyond a few tens of keV at Earth's low Mach number (1 =M <20) bow shock. Here we report observations of electrons energized by foreshock disturbances to energies up to at least approximately 300 keV. Although such energetic electrons have been previously observed, their presence has been attributed to escaping magnetospheric particles or solar events. These relativistic electrons are not associated with any solar or magnetospheric activity. Further, due to their relatively small Larmor radii (compared to magnetic gradient scale lengths) and large thermal speeds (compared to shock speeds), no known shock acceleration mechanism can energize thermal electrons up to relativistic energies. The discovery of relativistic electrons associated with foreshock structures commonly generated in astrophysical shocks could provide a new paradigm for electron injections and acceleration in collisionless plasmas.

  7. Modeling plasma glow discharges in Air near a Mach 3 bow shock with KRONOS

    NASA Astrophysics Data System (ADS)

    Rassou, Sebastien; Labaune, Julien; Packan, Denis; Elias, Paul-Quentin

    2016-09-01

    In this work, plasma glow discharge in Air is modeled near a Mach 3 bow shock. Numerical simulations are performed using the coupling KRONOS which have been developed at ONERA. The flow field is modeled using the code CFD: CEDRE from ONERA and the electrical and plasma part by the EDF open-source code CODE_SATURNE. The plasma kinetic modeling consists on a two-term Boltzmann equation solver and a chemical reaction solver depending of the electric field. The coupling KRONOS is fully parallelized and run on ONERA supercomputers. The shock wave is formed by the propagation of a supersonic flow (M = 3) through a truncated conical model mounted with a central spike. Depending on the spike's voltage value, corona, glow or arc regime could be obtained in a steady flow. The parameters for the supersonic flow and the spike configurations are chosen to be in glow discharge regime and to reproduce the experimental setup. In our simulations, 12 species and 80 reactions (ionization, electronic or vibrational excitation, attachment etc ...) are considered to properly model the glow discharge and the afterglow. In a stationary flow, glow discharge is observed only at the upstream of the shock wave near the high voltage spike. Behind the bow shock, in the afterglow, negative ions are provided by electrons attachment with O2. The negative ions flow convection ensures the electrical conduction and the establishment of the glow discharge.

  8. O+ ion beams reflected below the Martian bow shock: MAVEN observations

    NASA Astrophysics Data System (ADS)

    Masunaga, K.; Seki, K.; Brain, D. A.; Fang, X.; Dong, Y.; Jakosky, B. M.; McFadden, J. P.; Halekas, J. S.; Connerney, J. E. P.

    2016-04-01

    We investigate a generation mechanism of O+ ion beams observed above the Martian bow shock by analyzing ion velocity distribution functions (VDFs) measured by the Suprathermal and Thermal Ion Composition instrument on the Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft. In the solar wind near Mars, MAVEN often observes energetic O+ ion beams (~10 keV or higher). Accompanied with the O+ ion beam events, we sometimes observe characteristic ion VDFs in the magnetosheath: a partial ring distribution. The partial ring distribution corresponds to pickup ions with a finite initial velocity (i.e., not newborn pickup ions), and its phase space density is much smaller than that of local pickup O+ ions of the magnetosheath. Thus, the partial ring distribution is most likely produced by the reflection of pickup O+ ions precipitating from the upstream solar wind below the bow shock. After being injected into the magnetosheath from the solar wind, the precipitating O+ ions are subject to the significantly enhanced magnetic field in this region and start to gyrate around the guiding center of the plasma frame in the magnetosheath. Consequently, a part of precipitating O+ ions are reflected back to the solar wind, generating O+ beams in the solar wind. The beams direct quasi-sunward near the subsolar region but have large angle with respect to the sunward direction at high solar zenith angles (>50°). The reflected O+ beams are accelerated by the convection electric field of the solar wind and may escape Mars.

  9. Technical Note: Measurement of bow tie profiles in CT scanners using radiochromic film

    SciTech Connect

    Whiting, Bruce R.; Dohatcu, Andreea C.; Evans, Joshua D.; Williamson, Jeffrey F.; Politte, David G.

    2015-06-15

    Purpose: To provide a noninvasive technique to measure the intensity profile of the fan beam in a computed tomography (CT) scanner that is cost effective and easily implemented without the need to access proprietary scanner information or service modes. Methods: The fabrication of an inexpensive aperture is described, which is used to expose radiochromic film in a rotating CT gantry. A series of exposures is made, each of which is digitized on a personal computer document scanner, and the resulting data set is analyzed to produce a self-consistent calibration of relative radiation exposure. The bow tie profiles were analyzed to determine the precision of the process and were compared to two other measurement techniques, direct measurements from CT gantry detectors and a dynamic dosimeter. Results: The radiochromic film method presented here can measure radiation exposures with a precision of ∼6% root-mean-square relative error. The intensity profiles have a maximum 25% root-mean-square relative error compared with existing techniques. Conclusions: The proposed radiochromic film method for measuring bow tie profiles is an inexpensive (∼$100 USD + film costs), noninvasive method to measure the fan beam intensity profile in CT scanners.

  10. Relativistic Electrons Produced by Foreshock Disturbances Observed Upstream of Earth's Bow Shock

    NASA Astrophysics Data System (ADS)

    Wilson, L. B.; Sibeck, D. G.; Turner, D. L.; Osmane, A.; Caprioli, D.; Angelopoulos, V.

    2016-11-01

    Charged particles can be reflected and accelerated by strong (i.e., high Mach number) astrophysical collisionless shock waves, streaming away to form a foreshock region in communication with the shock. Foreshocks are primarily populated by suprathermal ions that can generate foreshock disturbances—large-scale (i.e., tens to thousands of thermal ion Larmor radii), transient (˜5 - 10 per day ) structures. They have recently been found to accelerate ions to energies of several keV. Although electrons in Saturn's high Mach number (M >40 ) bow shock can be accelerated to relativistic energies (nearly 1000 keV), it has hitherto been thought impossible to accelerate electrons beyond a few tens of keV at Earth's low Mach number (1 ≤M <20 ) bow shock. Here we report observations of electrons energized by foreshock disturbances to energies up to at least ˜300 keV . Although such energetic electrons have been previously observed, their presence has been attributed to escaping magnetospheric particles or solar events. These relativistic electrons are not associated with any solar or magnetospheric activity. Further, due to their relatively small Larmor radii (compared to magnetic gradient scale lengths) and large thermal speeds (compared to shock speeds), no known shock acceleration mechanism can energize thermal electrons up to relativistic energies. The discovery of relativistic electrons associated with foreshock structures commonly generated in astrophysical shocks could provide a new paradigm for electron injections and acceleration in collisionless plasmas.

  11. Cluster II Constraints on Electron Acceleration and Langmuir Waves at Earth's Bow Shock

    NASA Astrophysics Data System (ADS)

    Cairns, I. H.; Krasnoselskikh, V. V.; Lobzin, V. V.; Lucek, E.; Lefebvre, B.

    2005-12-01

    Electron acceleration, Langmuir waves and radio emissions at multiples of the plasma frequency are associated with numerous shocks in the heliosphere, including Earth's bow shock and the shocks producing coronal and interplanetary type II radio bursts. Here Cluster data from the Whisper, FGM, and PEACE instruments are used to study electron acceleration at Earth's bow shock and by SLAMS, as well as the production of electron beams and Langmuir waves in Earth's foreshock. The results found include: (1) The most intense Langmuir waves are found where Cluster is magnetically connected to almost perpendicular regions of the shock with |θbn| > 70°. (2) The wave characteristics and analytic theory strongly imply that the `standard'' foreshock model is relevant: these electrons are produced by the magnetic mirror reflection/shock-drift acceleration (SDA) at the shock, the beams are produced by time-of-flight effects, and the waves are driven by beams with speeds greater than the electron thermal speed. (3) Weak bursts of broadband waves are found where |θbn| <70° and cutoff effects are unimportant. This is consistent with another electron acceleration or beam formation process being active. (4) Isolated SLAMS, even in periods between two SLAMS, produce only very weak, irregular bursts of Langmuir waves, implying that they are ineffective in accelerating electrons and/or forming beam distributions. This argues against SLAMS playing a role in type II bursts.

  12. A Parametric Investigation of Breaking Bow Waves using a 2D+T Wave Maker

    NASA Astrophysics Data System (ADS)

    Maxeiner, E. A.; Shakeri, M.; Duncan, J. H.

    2008-11-01

    An experimental study of bow waves generated by a 2D+T (Two Dimensions plus Time) wave maker in a tank that is 14.8 m long, 1.2 m wide and 2.2 m deep is presented. Rather than simulating a specific ship hull, here we use a parametric set of wave maker motions with each parameter simulating a common feature of a ship hull form. Three categories of wave maker motions are used: ``slap'' (rotation of the wave board (held flat) about the keel), ``fixed'' (translation the wave board while it is upper part remains flat and at a fixed angle relative to horizontal), and ``full'' (simultaneous rotation and translation). The wave maker motions are run over a range of speeds and, in the ``fixed'' cases, over a range of angles. The temporal histories of the wave profiles were measured using a cinematic LIF technique. The relationship between various geometrical features of the waves and the wave maker motion parameters is explored. Each category of wave maker motions produces waves that develop and break in markedly different ways, thus highlighting the complex nature of bow waves. The wave crest speeds vary between 2 and 2.5 times the maximum speed of the wave maker and, for a given class of wave maker motion, vary with wave maker speed.

  13. The Enigmatic Guitar Nebula: Bow Shock Nebulae, Pulsar Parallaxes and the Interstellar Medium

    NASA Astrophysics Data System (ADS)

    Chatterjee, S.; Cordes, J. M.

    Bow shocks and pulsar wind nebulae probe the interaction of neutron star relativistic winds with the interstellar medium. We utilize scaling laws derived for bow shock nebulae, in combination with estimates of neutron star distances and velocities, to extract information about the interstellar medium as well as relativistic winds. Specifically, we report on Chandra X-ray Observatory and Hubble Space Telescope observations of the spectacular Guitar Nebula, produced by a high velocity but otherwise unremarkable neutron star. The observed time evolution in the position and morphology of the nebula leads us to infer the existence of small scale density fluctuations in the interstellar medium, while X-ray observations reveal potential evidence for magnetic reconnection. Increases in the sample of precise astrometric measurements, coupled with multi-wavelength observations, will enable a deeper understanding of neutron star relativistic winds: we introduce an ongoing project with the Very Long Baseline Array, which is expected to at least double the number of measured pulsar parallaxes in the next two years.

  14. Hydroelastic Response of Surface-Effect Ship Bow Seals: Large-Scale Experiments and Post-Buckling Analysis

    NASA Astrophysics Data System (ADS)

    Wiggins, Andrew D.

    Bow seals are critical components on advanced marine vehicles that rely on aerostatic support to reduce drag. They consist of a series of open-ended fabric cylinders ("fingers") that contact the free surface and, when inflated, form a compliant pressure barrier. Bow seals are unique in that, unlike a majority of structures in civil and mechanical engineering, bow seals operate in a buckled state. The response characteristics of these structures are of practical interest due to unacceptable wear rates on seal components and difficulties in predicting seal performance. Despite this, the hydroelastic response of the seal system, particularly basic information on seal vibration modes and the mechanisms responsible for seal wear, remains largely unknown. Similarly, estimates of the hydrodynamic loads on the seal system are inaccurate and based on heuristic scaling of data from small-scale experiments, where similitude is challenging to maintain. Thus, a large-scale test system is necessary to obtain accurate estimates of bow seal response. The work is comprised of three parts. Part one presents detailed observations of bow seal response acquired using a large-scale test platform developed as part of the present study. These high-resolution observations, the first of their kind, show bow seal response to be characterized by complex post-buckling behavior. Part two proposes an analytical framework for interpreting the wide range of behavior observed at large scale. Using this framework, key parameters driving seal conformation and stability are identified. It is found that, due to their buckled state, bow seals are highly susceptible to a mode switching instability, which may be a potential mechanism responsible for the damaging vibrations. In part three, a benchtop experiment is used to demonstrate that the scalings identified in this study hold across a wide range of bending rigidities. This work has implications for improving drag and wear characteristics in future bow

  15. Two case presentations and surgical management of Bow Hunter's syndrome associated with bony abnormalities of the C7 vertebra.

    PubMed

    Lee, Victoria; Riles, Thomas S; Stableford, Jennifer; Berguer, Ramon

    2011-05-01

    Bow Hunter's syndrome is a condition in which patients experience vertebrobasilar symptoms on head turn. It may be a consequence of intrinsic factors such as atherosclerosis, or it may be secondary to mechanical compression. Most commonly, this occurs at the level of C2 or above. We present two rare cases of Bow Hunter's syndrome secondary to mechanical compression at the level of C7. Discussed are the anatomic conditions leading to this syndrome in these two patients, the methodology for confirming the diagnosis, and the successful management by partial resection of the transverse processes compressing the vertebral arteries.

  16. Study of relation between Pc 3 micropulsations and magnetosheath fluctuations, and multisatellite investigation of earth's bow shock

    NASA Technical Reports Server (NTRS)

    Greenstadt, E. W.

    1975-01-01

    The validity is investigated of a suggested model according to which Pc 3 and/or Pc 4 micropulsations are excited by magnetosheath field (and plasma) fluctuations arising in the quasi-parallel structure of the subsolar bow shock. The influence of solar wind plasma parameters on local shock structure and on the configuration of the entire bow shock system is included. Simultaneous data from two or more spacecraft and from multiple diagnostics is used to evaluate the geometrical factor, field-to-shock normal angle, or its B-X equivalent, and the principal plasma parameters. Results are presented and discussed.

  17. Recent H-alpha Results on Pulsar B2224+65's Bow-Shock Nebula, the "Guitar"

    NASA Astrophysics Data System (ADS)

    Dolch, Timothy; Chatterjee, Shami; Clemens, Dan P.; Cordes, James M.; Cashmen, Lauren R.; Taylor, Brian W.

    2016-09-01

    We used the 4 m Discovery Channel Telescope (DCT) at Lowell observatory in 2014 to observe the Guitar Nebula, an Hα bow-shock nebula around the high-velocity radio pulsar B2224+65. Since the nebula's discovery in 1992, the structure of the bow-shock has undergone significant dynamical changes. We have observed the limb structure, targeting the “body” and “neck” of the guitar. Comparing the DCT observations to 1995 observations with the Palomar 200-inch Hale telescope, we found changes in both spatial structure and surface brightness in the tip, head, and body of the nebula.

  18. A benign form of congenital anterolateral bowing of the tibia associated with ipsilateral polydactyly of the hallux: case report and literature review.

    PubMed

    Han, Jiuhui; Qu, Lei; Li, Yazhou; Luo, Junzhong; Cao, Jinchao; Zhao, Wanyu

    2012-07-01

    Congenital anterolateral bowing of the tibia is generally considered a precursor of congenital pseudarthrosis of the tibia (CPT), which is usually associated with neurofibromatosis type 1 (NF1), a common autosomal dominant genetic disorder. In many cases, NF1 is initially suspected following the presentation of a child with anterolateral tibial bowing. The prognosis of CPT is poor, and amputation may be required. Congenital anterolateral bowing of the tibia combined with ipsilateral polydactyly of the hallux (CABTP) is a rare entity that resembles the anterolateral tibial bowing that occurs in association with CPT, and may be misdiagnosed as NF1. However, spontaneous correction of the tibial bowing with an almost normal fibula has been described in all previously reported cases. Here, we report three patients with CABTP and discuss the physical and imaging characteristics and follow-up results. We suggest that given the spontaneous resolution of bowing, the absence of neurocutaneous signs and the relatively favorable prognosis, CABTP is a distinct entity that merits its own place within the field of anterolateral bowing of the tibia and has no association with CPT or NF1. This should help avoid unnecessary investigations and interventions for NF1. This article shows for the first time tibial duplication in the area of bowing, with two medullary canals surrounded by well-defined cortex on CT.

  19. Gamma-Ray Flaring Activity from the Gravitationally Lensed Blazar PKS 1830-211 Observed by Fermi LAT

    SciTech Connect

    Abdo, A. A.; et al.

    2015-01-23

    The Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope routinely detects the MeV-peaked flat-spectrum radio quasar PKS 1830–211 (z = 2.507). Its apparent isotropic γ-ray luminosity (E > 100 MeV), averaged over ~3 years of observations and peaking on 2010 October 14/15 at 2.9 × 10(50) erg s(–)(1), makes it among the brightest high-redshift Fermi blazars. No published model with a single lens can account for all of the observed characteristics of this complex system. Based on radio observations, one expects time-delayed variability to follow about 25 days after a primary flare, with flux about a factor of 1.5 less. Two large γ-ray flares of PKS 1830–211 have been detected by the LAT in the considered period, and no substantial evidence for such a delayed activity was found. This allows us to place a lower limit of about 6 on the γ-ray flux ratio between the two lensed images. Swift XRT observations from a dedicated Target of Opportunity program indicate a hard spectrum with no significant correlation of X-ray flux with the γ-ray variability. The spectral energy distribution can be modeled with inverse Compton scattering of thermal photons from the dusty torus. The implications of the LAT data in terms of variability, the lack of evident delayed flare events, and different radio and γ-ray flux ratios are discussed. Microlensing effects, absorption, size and location of the emitting regions, the complex mass distribution of the system, an energy-dependent inner structure of the source, and flux suppression by the lens galaxy for one image path may be considered as hypotheses for understanding our results.

  20. A dwarf galaxy near the sight line to PKS 0454+0356 - A fading 'faint blue galaxy'?

    NASA Technical Reports Server (NTRS)

    Steidel, Charles C.; Dickinson, Mark; Bowen, David V.

    1993-01-01

    We report the discovery of a dwarf galaxy (MB = -17.2 for H0 = 50 km/s per Mpc) at z = 0.072 which is only 4 arcsec (3.7/h(100) kpc) in projection from the line of sight to the bright quasar PKS 0454+0356 (z(em) = 1.345). The dwarf has very blue optical and optical/IR colors and exhibits line emission indicative of ongoing or recent star formation. However, there is no detection of Ca II 3934 A, 3969 A absorption at z(abs) = 0.072 to equivalent width limits (3 sigma) of about 40 mA, which would suggest an H I column density along the line of sight of less than 5 x 10 exp 19/sq cm, if the Ca II/H I ratio is similar to sight lines in the Galaxy. Based on the absence of Ca II absorption and the unusually weak line emission given the very blue color of the dwarf, we speculate that it may be close to exhausting its supply of gas. As its star formation rate declines, the galaxy's blue magnitude should fade substantially, eventually reaching a quiescent state in accord with its K luminosity of about 0.005 L*. Future observations of the sight line to PKS 0454+0356 using HST in search of Mg II resonance lines, or a search for 21 cm absorption against the quasar radio continuum, could place even more stringent limits on the extent of the gas associated with an intrinsically faint, star-forming dwarf.

  1. GAMMA-RAY FLARING ACTIVITY FROM THE GRAVITATIONALLY LENSED BLAZAR PKS 1830–211 OBSERVED BY Fermi LAT

    SciTech Connect

    Abdo, A. A.; Ackermann, M.; Buehler, R.; Ajello, M.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Caliandro, G. A.; Cameron, R. A.; Amin, M. A.; Baldini, L.; Bellazzini, R.; Barbiellini, G.; Bastieri, D.; Buson, S.; Bonamente, E.; Bregeon, J.; Bulmash, D. E-mail: stefano.ciprini@asdc.asi.it E-mail: dammando@ira.inaf.it E-mail: sara.buson@pd.infn.it E-mail: dammando@ira.inaf.it; and others

    2015-02-01

    The Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope routinely detects the MeV-peaked flat-spectrum radio quasar PKS 1830–211 (z = 2.507). Its apparent isotropic γ-ray luminosity (E > 100 MeV), averaged over ∼3 years of observations and peaking on 2010 October 14/15 at 2.9 × 10{sup 50} erg s{sup –1}, makes it among the brightest high-redshift Fermi blazars. No published model with a single lens can account for all of the observed characteristics of this complex system. Based on radio observations, one expects time-delayed variability to follow about 25 days after a primary flare, with flux about a factor of 1.5 less. Two large γ-ray flares of PKS 1830–211 have been detected by the LAT in the considered period, and no substantial evidence for such a delayed activity was found. This allows us to place a lower limit of about 6 on the γ-ray flux ratio between the two lensed images. Swift XRT observations from a dedicated Target of Opportunity program indicate a hard spectrum with no significant correlation of X-ray flux with the γ-ray variability. The spectral energy distribution can be modeled with inverse Compton scattering of thermal photons from the dusty torus. The implications of the LAT data in terms of variability, the lack of evident delayed flare events, and different radio and γ-ray flux ratios are discussed. Microlensing effects, absorption, size and location of the emitting regions, the complex mass distribution of the system, an energy-dependent inner structure of the source, and flux suppression by the lens galaxy for one image path may be considered as hypotheses for understanding our results.

  2. INTERSTELLAR SILICATE DUST IN THE z = 0.89 ABSORBER TOWARD PKS 1830-211: CRYSTALLINE SILICATES AT HIGH REDSHIFT?

    SciTech Connect

    Aller, Monique C.; Kulkarni, Varsha P.; Som, Debopam; York, Donald G.; Welty, Daniel E.; Vladilo, Giovanni

    2012-03-20

    We present evidence of a >10{sigma} detection of the 10 {mu}m silicate dust absorption feature in the spectrum of the gravitationally lensed quasar PKS 1830-211, produced by a foreground absorption system at redshift 0.886. We have examined more than 100 optical depth templates, derived from both observations of Galactic and extragalactic sources and laboratory measurements, in order to constrain the chemical structure of the silicate dust. We find that the best fit to the observed absorption profile is produced by laboratory crystalline olivine, with a corresponding peak optical depth of {tau}{sub 10} = 0.27 {+-} 0.05. The fit is slightly improved upon by including small contributions from additional materials, such as silica, enstatite, or serpentine, which suggests that the dust composition may consist of a blend of crystalline silicates. Combining templates for amorphous and crystalline silicates, we find that the fraction of crystalline silicates needs to be at least 95%. Given the rarity of extragalactic sources with such a high degree of silicate crystallinity, we also explore the possibility that the observed spectral features are produced by amorphous silicates in combination with other molecular or atomic transitions, or by foreground source contamination. While we cannot rule out these latter possibilities, they lead to much poorer profile fits than for the crystalline olivine templates. If the presence of crystalline interstellar silicates in this distant galaxy is real, it would be highly unusual, given that the Milky Way interstellar matter contains essentially only amorphous silicates. It is possible that the z = 0.886 absorber toward PKS 1830-211, well known for its high molecular content, has a unique star-forming environment that enables crystalline silicates to form and prevail.

  3. Is "Bow" for an Arrow or for Hair? A Classroom Demonstration on Gender Differences in Interpreting Ambiguous Information

    ERIC Educational Resources Information Center

    Fa-Kaji, Naomi; Nguyen, Linda; Hebl, Mikki; Skorinko, Jeanine

    2016-01-01

    This article details a classroom demonstration of how gender differences in cognitive schemas can result in men and women differentially interpreting the same information. Students heard a series of six homonyms (e.g., bow and nail) spoken aloud and wrote down the first word with which they free-associated each homonym. When hearing the words…

  4. Radiohumeral synostosis, femoral bowing, other skeletal anomalies and anal atresia, a variant example of Antley-Bixler syndrome?

    PubMed

    Antich, J; Iriondo, M; Lizarraga, I; Manzanares, R; Cusi, V

    1993-01-01

    We report a newborn with radiohumeral synostosis, femoral bowing, anal atresia, a prominent nose (pear shaped nose), slender ribs, long tapering fingers with distal camptodactyly, genital hypoplasia and a neonatal humeral fracture. Among the possible differential diagnoses a variant example of Antley-Bixler syndrome is considered to be the most likely final diagnosis.

  5. 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.... working within the Mailing Solutions Management Division who are located in remote work sites, including... partially separated from employment on or after June 23, 2009, through September 10, 2010, and all...

  6. 76 FR 78234 - Medicine Bow-Routt National Forests and Thunder Basin National Grassland, Campbell County, WY...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-12-16

    ... Forest Service Medicine Bow-Routt National Forests and Thunder Basin National Grassland, Campbell County... System (NFS) land on Thunder Basin National Grassland. The proposal comprises new construction of... Forests and Thunder Basin National Grassland, 2250 East Richards Street, Douglas, Wyoming 82633, or...

  7. 76 FR 35398 - Scoria Mining Addition, Medicine Bow-Routt National Forests and Thunder Basin National Grassland...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-06-17

    ... Grassland; Campbell County, WY AGENCY: Forest Service, USDA. ACTION: Notice of intent to prepare an... on parcels of National Forest System (NFS) lands on Thunder Basin National Grassland. NFS lands..., Medicine Bow-Routt National Forests and Thunder Basin National Grassland, 2250 East Richards...

  8. FEASIBILITY OF WIND TO SERVE UPPER SKAGIT'S BOW HILL TRIBAL LANDS AND FEASIBILITY UPDATE FOR RESIDENTIAL RENEWABLE ENERGY.

    SciTech Connect

    RICH, LAUREN

    2013-09-30

    A two year wind resource assessment was conducted to determine the feasibility of developing a community scale wind generation system for the Upper Skagit Indian Tribe's Bow Hill land base, and the project researched residential wind resource technologies to determine the feasibility of contributing renewable wind resource to the mix of energy options for our single and multi-family residential units.

  9. Measurement of the potential drop across the earth's collisionless bow shock

    NASA Technical Reports Server (NTRS)

    Formisano, V.

    1982-01-01

    The normal component of the dc electric field measured on ISEE-1 ordinarily exhibits an enhancement of a few mV/m over both upstream and downstream values at the earth's bow shock. Using the measured relative velocity between the shock and the spacecraft (from the ISEE-1/2 time delay in the magnetometer data), it is possible to transform the observed E enhancement to a potential drop (delta phi). For a subcritical shock the potential drop is found to be very close to the measured change of particle kinetic energy (delta phi, approximately 280 V on day 330, 1977), whereas for a supercritical shock the potential drop is only a fraction of the measured change of kinetic energy (delta phi, approximately 140 V on day 324, 1977).

  10. Diffusive shock acceleration - comparison of a unified shock model to bow shock observations

    SciTech Connect

    Ellison, D.C.; Moebius, E.

    1987-07-01

    A comparison is made between recent AMPTE/IRM observations of diffuse ions detected upstream of the earth's bow shock when the interplanetary magnetic field was nearly parallel to the solar wind direction and a known collisionless quasi-parallel shock model. These observations, which provide the proton spectrum for all of velocity space, give a direct measure of the shock acceleration efficiency and show how thermal solar winds are injected into the diffusive shock acceleration mechanism. The model accurately describes the proton spectrum; moreover, it predicts the shock structure, the complete particle spectrum, the relative velocity distributions of different ion species in the down stream region, and the enhancement of heavy ions over protons relative to the unshocked solar wind. 68 references.

  11. Method for measuring violin sound radiation based on bowed glissandi and its application to sound synthesis.

    PubMed

    Perez Carrillo, Alfonso; Bonada, Jordi; Patynen, Jukka; Valimaki, Vesa

    2011-08-01

    This work presents a method for measuring and computing violin-body directional frequency responses, which are used for violin sound synthesis. The approach is based on a frame-weighted deconvolution of excitation and response signals. The excitation, consisting of bowed glissandi, is measured with piezoelectric transducers built into the bridge. Radiation responses are recorded in an anechoic chamber with multiple microphones placed at different angles around the violin. The proposed deconvolution algorithm computes impulse responses that, when convolved with any source signal (captured with the same transducer), produce a highly realistic violin sound very similar to that of a microphone recording. The use of motion sensors allows for tracking violin movements. Combining this information with the directional responses and using a dynamic convolution algorithm, helps to improve the listening experience by incorporating the violinist motion effect in stereo.

  12. Quantitative spectroscopy on individual wire, slot, bow-tie, rectangular, and square-shaped optical antennas.

    PubMed

    Husnik, Martin; Niegemann, Jens; Busch, Kurt; Wegener, Martin

    2013-11-15

    By using a recently introduced approach combining a focus-modulation technique with a common-path interferometer, we measure quantitatively the extinction, scattering, and absorption cross-section spectra of individual optical antennas. The experimental results on thin-wire antennas, slot antennas, bow-tie antennas, rectangular antennas, and square-shaped antennas resonating at around 1.4 μm wavelength are discussed. We find increased resonant scattering cross sections for the latter four antennas compared to the thin-wire antenna, both in absolute terms and relative to the absorption cross section. The square-shaped antenna's resonant extinction cross section approaches the limit of a coherent point dipole. However, the ratio of the resonant extinction cross section to the geometrical cross section of 38 is largest for the simple thin-wire antenna.

  13. Diffusive shock acceleration - Comparison of a unified shock model to bow shock observations

    NASA Technical Reports Server (NTRS)

    Ellison, Donald C.; Moebius, Eberhard

    1987-01-01

    A comparison is made between recent AMPTE/IRM observations of diffuse ions detected upstream of the earth's bow shock when the interplanetary magnetic field was nearly parallel to the solar wind direction and a known collisionless quasi-parallel shock model. These observations, which provide the proton spectrum for all of velocity space, give a direct measure of the shock acceleration efficiency and show how thermal solar winds are injected into the diffusive shock acceleration mechanism. The model accurately describes the proton spectrum; moreover, it predicts the shock structure, the complete particle spectrum, the relative velocity distributions of different ion species in the down stream region, and the enhancement of heavy ions over protons relative to the unshocked solar wind.

  14. Detection of singly ionized energetic lunar pick-up ions upstream of earth's bow shock

    NASA Technical Reports Server (NTRS)

    Hilchenbach, M.; Hovestadt, D.; Klecker, B.; Moebius, E.

    1992-01-01

    Singly ionized suprathermal ions upstream of the earth's bow shock have been detected by using the time-of-flight spectrometer SULEICA on the AMPTE/IRM satellite. The data were collected between August and December 1985. The flux of the ions in the mass range between 23 and 37 amu is highly anisotropic towards the earth. The ions are observed with a period of about 29 days around new moon (+/- 3 days). The correlation of the energy of the ions with the solar wind speed and the interplanetary magnetic field orientation indicates the relation to the pick-up process. We conclude that the source of these pick-up ions is the moon. We argue that due to the impinging solar wind, atoms are sputtered off the lunar surface, ionized in the sputtering process or by ensuing photoionization and picked up by the solar wind.

  15. Structure of a quasi-parallel, quasi-laminar bow shock

    NASA Technical Reports Server (NTRS)

    Greenstadt, E. W.; Russell, C. T.; Formisano, V.; Hedgecock, P. C.; Scarf, F. L.; Neugebauer, M.; Holzer, R. E.

    1976-01-01

    A thick, quasi-parallel bow shock structure was observed with field and particle detectors of both HEOS 1 and OGO 5. The typical magnetic pulsation structure was at least 1 to 2 earth radii thick radially and was accompanied by irregular but distinct plasma distributions characteristic of neither the solar wind nor the magnetosheath. Waves constituting the large pulsations were polarized principally in the plane of the nominal shock, therefore also in the plane perpendicular to the average interplanetary field. A separate interpulsation regime detected between bursts of large amplitude oscillations was similar to the upstream wave region magnetically, but was characterized by disturbed plasma flux and enhanced noise around the ion plasma frequency. The shock structure appeared to be largely of an oblique, whistler type, probably complicated by counterstreaming high energy protons. Evidence for firehose instability-based structure was weak at best and probably negative.

  16. Simultaneous plasma wave and electron flux observations upstream of the Martian bow shock

    NASA Astrophysics Data System (ADS)

    Skalsky, A.; Grard, R.; Kiraly, P.; Klimov, S.; Kopanyi, V.; Schwingenschuh, K.; Trotignon, J. G.

    1993-03-01

    Flux enhancements of electrons with energies between 100 and 530 eV are observed simultaneously with electron plasma waves in the upstream region of the Martian bow shock. The electron flux appears to reach its maximum when the pitch angle is close to 0 deg, which corresponds to particles reflected from the shock region and backstreaming in the solar wind along the magnetic field. The correlation between high-frequency waves and enhanced electron fluxes is reminiscent of several studies on the electron foreshock of the Earth. Such a similarity indicates that, in spite of major differences between the global shock structures, the microscopic processes operating in the foreshocks of Earth and Mars are probably identical.

  17. Oxidation of graphene 'bow tie' nanofuses for permanent, write-once-read-many data storage devices.

    PubMed

    Pearson, A C; Jamieson, S; Linford, M R; Lunt, B M; Davis, R C

    2013-04-05

    We have fabricated nanoscale fuses from CVD graphene sheets with a 'bow tie' geometry for write-once-read-many data storage applications. The fuses are programmed using thermal oxidation driven by Joule heating. Fuses that were 250 nm wide with 2.5 μm between contact pads were programmed with average voltages and powers of 4.9 V and 2.1 mW, respectively. The required voltages and powers decrease with decreasing fuse sizes. Graphene shows extreme chemical and electronic stability; fuses require temperatures of about 400 °C for oxidation, indicating that they are excellent candidates for permanent data storage. To further demonstrate this stability, fuses were subjected to applied biases in excess of typical read voltages; stable currents were observed when a voltage of 10 V was applied to the devices in the off state and 1 V in the on state for 90 h each.

  18. On the origin of hot diamagnetic cavities near the earth's bow shock

    NASA Technical Reports Server (NTRS)

    Thomsen, M. F.; Gosling, J. T.; Bame, S. J.; Quest, K. B.; Russell, C. T.

    1988-01-01

    The origin of hot diamagnetic cavities (HDCs) observed occasionally upstream from the earth's bow shock is investigated by examining the results of November 16, 1977, observation, when four of these events occurred on a single day, as well as plasma and field data from that day. The results suggest that HDCs may form as a result of an unusually strong interaction between shock-reflected ions and the incoming solar wind. It is proposed that this interaction stems from a temporary and localized reflection of a larger-than-normal fraction of the incident ions, which is stimulated by sudden changes in the upstream field orientation; the consequences of such a temporary overreflection are found to be consistent with many of the observed features of HDCs, including the strong slowing, deflection, and heating of the flow, as well as the localization, internal recoveries, and occasional formation upstream from the shock itself.

  19. Dynamics of bow-tie shaped bursting: Forced pendulum with dynamic feedback

    NASA Astrophysics Data System (ADS)

    Hongray, Thotreithem; Balakrishnan, Janaki

    2016-12-01

    A detailed study is performed on the parameter space of the mechanical system of a driven pendulum with damping and constant torque under feedback control. We report an interesting bow-tie shaped bursting oscillatory behaviour, which is exhibited for small driving frequencies, in a certain parameter regime, which has not been reported earlier in this forced system with dynamic feedback. We show that the bursting oscillations are caused because of a transition of the quiescent state to the spiking state by a saddle-focus bifurcation, and because of another saddle-focus bifurcation, which leads to cessation of spiking, bringing the system back to the quiescent state. The resting period between two successive bursts (Trest) is estimated analytically.

  20. Dynamics of bow-tie shaped bursting: Forced pendulum with dynamic feedback.

    PubMed

    Hongray, Thotreithem; Balakrishnan, Janaki

    2016-12-01

    A detailed study is performed on the parameter space of the mechanical system of a driven pendulum with damping and constant torque under feedback control. We report an interesting bow-tie shaped bursting oscillatory behaviour, which is exhibited for small driving frequencies, in a certain parameter regime, which has not been reported earlier in this forced system with dynamic feedback. We show that the bursting oscillations are caused because of a transition of the quiescent state to the spiking state by a saddle-focus bifurcation, and because of another saddle-focus bifurcation, which leads to cessation of spiking, bringing the system back to the quiescent state. The resting period between two successive bursts (Trest) is estimated analytically.

  1. Juvenile Cerebral Infarction Caused by Bow Hunter’s Syndrome during Sport: Two Case Reports

    PubMed Central

    KAGEYAMA, Hiroto; YOSHIMURA, Shinichi; IIDA, Tomoko; SHIRAKAWA, Manabu; UCHIDA, Kazutaka; TOMOGANE, Yusuke; MIYAJI, Yuki

    2016-01-01

    We report two cases of juvenile cerebral infarction caused by bow hunter’s syndrome (BHS) during sport. Case 1 was a 17-year-old male who developed a partial visual field defect after playing basketball. BHS was diagnosed because cervical ultrasonography demonstrated occlusion of the vertebral artery when the neck was rotated. After C1–2 posterior fixation was performed, his symptoms resolved. Case 2 was an 18-year-old male with recurrent visual disturbance after playing handball. Cerebral infarction occurred repeatedly despite antiplatelet therapy. After 3 years, vertebral artery dissection was diagnosed and stenting was performed, but his symptoms did not resolve. BHS was diagnosed when he was examined at our department. C1–2 posterior fixation was performed and his symptoms resolved. In these two cases, BHS was caused by sporting activity. For accurate diagnosis and treatment of BHS, neuroimaging with cervical rotation is mandatory. PMID:27053329

  2. Magnetised bow shocks and oblique shock interactions: HEDLA experiments on the Magpie pulsed-power facility

    NASA Astrophysics Data System (ADS)

    Burdiak, G. C.; Lebedev, S. V.; Chittenden, J. P.; Clayson, T.; Garcia, C.; Hare, J. D.; Niasse, N.; Suttle, L. G.; Suzuki-Vidal, F.; Frank, A.; Ciardi, A.

    2016-10-01

    We present results from magnetised shock experiments performed on the Magpie ( 1 MA, 250 ns) pulsed-power facility. Shocks are formed around cylindrical and oblique planar obstacles positioned in a supersonic, super-Alfvenic plasma flow (MS = 5 , MA = 2.5 , vf = 70 km/s). The plasma flow is produced by an inverse, exploding wire array z-pinch and carries an embedded magnetic field that is well frozen in (ReM = 20). We show how the structure of bow and oblique shocks is dramatically affected by the orientation of the advected magnetic field with respect to the obstacles. More complex obstacle geometries allow us to study the interaction of multiple magnetised oblique shocks. These systems can cause the annihilation of magnetic flux and the generation of shear flow along a slip layer. Work supported by DOE cooperative agreements No. DE-F03- 02NA00057 and No. DE-SC-0001063.

  3. Pseudomorphic GeSn/Ge(001) quantum wells: Examining indirect band gap bowing

    SciTech Connect

    Tonkikh, Alexander A.; Eisenschmidt, Christian; Schmidt, Georg; Talalaev, Vadim G.; Zakharov, Nikolay D.; Werner, Peter; Schilling, Joerg

    2013-07-15

    A study of the bandgap character of compressively strained GeSn{sub 0.060-0.091}/Ge(001) quantum wells grown by molecular beam epitaxy is reported. The built-in strain in GeSn wells leads to an increased separation between L and {Gamma} conduction band minima. The prevalent indirect interband transitions in GeSn were probed by photoluminescence spectroscopy. As a result we could simulate the L-valley bowing parameter in GeSn alloys, b{sub L} = 0.80 {+-} 0.06 eV at 10 K. From this we conclude that even compressively strained GeSn/Ge(001) alloys could become direct band gap semiconductors at the Sn-fraction higher than 17.0 at. %.

  4. Plasma waves associated with energetic particles streaming into the solar wind from the earth's bow shock

    NASA Technical Reports Server (NTRS)

    Anderson, R. R.; Eastman, T. E.; Gurnett, D. A.; Frank, L. A.; Parks, G. K.

    1981-01-01

    Plasma wave and plasma data from ISEE 1 and 2 are examined. In the upstream solar wind, three dominant types of plasma waves are observed which are associated with energetic particle streams coming from the bow shock: ion acoustic waves, electron plasma oscillations, and whistler mode waves. The ion acoustic waves occur simultaneously with either ion beams or a dispersed ion population in the energy range from 0.5 to greater than 45 keV. The electron plasma oscillations are long-wavelength, nearly monochromatic electrostatic waves which are closely correlated with the flux of low-energy electrons, especially in the 0.2-1.5 keV range. Electromagnetic waves with frequencies below 200 Hz are observed when either ion beams or dispersed ion distributions are present; for these waves the refractive index determined from the wave B to E ratio is consistent with whistler mode radiation.

  5. Theory for the 2f(p) radiation upstream of the earth's bow shock

    SciTech Connect

    Cairns, I.H.; Melrose, D.B.

    1985-07-01

    The mechanism responsible for the radiation observed near the earth bow shock at twice the plasma frequency f(p) is investigated theoretically. A model comprising two three-wave steps and involving Langmuir (L), ion-sound (S), and EM (t) waves is proposed: L + or - S yields L-prime; L + L-prime yields t. This model is shown to be consistent with observations of low-frequency S-like waves (Anderson et al., 1981), and further observational tests are suggested. A critical examination of the theory of Fung et al. (1982) is included, and it is found that an important term in the absorption coefficient was neglected. Correcting this error leads to an intrinsic theoretical brightness-temperature limit of 3 x 10 to the 9th K, well below the observed brightness temperature of the 2 f(p) radiation, about 10 to the 11th K. 18 references.

  6. A model for generation of bow-shock-associated upstream waves. [in solar wind

    NASA Technical Reports Server (NTRS)

    Fredricks, R. W.

    1975-01-01

    A model is proposed for the generation of upstream hydromagnetic waves by proton beams reflected at the earth's bow shock. It is assumed that the reflection process can produce some gyrophase bunching of the protons, thus creating a gyrophase disturbance that propagates with the beam as it streams back along interplanetary field lines. This leads to the production of driven hydromagnetic waves in the left-hand mode. The resulting theory predicts a wave amplitude, frequency, and polarization in the solar wind rest frame. The amplitude depends on the fraction of protons assumed to be phase coherent in their gyromotion and on the plasma beta, beam velocity, temperatures, and the Alfven Mach number. The theory also predicts the Doppler-shifted frequencies and the apparent sense of polarization that would be observed in satellite measurement frames.

  7. The Guitar Nebula: A Bow Shock that Traces ISM Turbulence and Accelerates Relativistic Particles

    NASA Astrophysics Data System (ADS)

    Chatterjee, Shamibrata

    2005-09-01

    We propose joint Chandra and HST observations of the Guitar Nebula, an extraordinary bow-shock nebula produced by a very high-velocity but otherwise ordinary pulsar. Prior HST observations show epoch dependent changes in shock structure that signify changing ISM conditions. An enigmatic jet or filament is seen in a Chandra ACIS image (year 2000), unlike jets from the Crab or other young pulsars. New Chandra observations will reveal the relative motion of the jet and the pulsar (which has moved by 0.9 arcsec) and thus determine if self confinement or special structure in the ISM plays a dominant role in shaping the jet, and will constrain the particle acceleration mechanism. We request joint high-resolution HST observations to contemporaneously determine the ISM density profile.

  8. The Guitar Nebula: A Bow Shock that Traces ISM Turbulence and Accelerates Relativistic Particles

    NASA Astrophysics Data System (ADS)

    Chatterjee, Shami

    2005-07-01

    We propose joint Chandra and HST observations of the Guitar Nebula, an extraordinary bow-shock nebula produced by a very high-velocity but otherwise ordinary pulsar. Prior HST observations show epoch dependent changes in shock structure that signify changing ISM conditions. An enigmatic jet or filament is seen in a Chandra ACIS image {year 2000}, unlike jets from the Crab or other young pulsars. New Chandra observations will reveal the relative motion of the jet and the pulsar {which has moved by 0.9 arcsec} and thus determine if self confinement or special structure in the ISM plays a dominant role in shaping the jet, and will constrain the particle acceleration mechanism. We request joint high-resolution HST observations to contemporaneously determine the ISM density profile.

  9. On the proper Mach number and ratio of specific heats for modeling the Venus bow shock

    NASA Technical Reports Server (NTRS)

    Tatrallyay, M.; Russell, C. T.; Luhmann, J. G.; Barnes, A.; Mihalov, J. D.

    1984-01-01

    Observational data from the Pioneer Venus Orbiter are used to investigate the physical characteristics of the Venus bow shock, and to explore some general issues in the numerical simulation of collisionless shocks. It is found that since equations from gas-dynamic (GD) models of the Venus shock cannot in general replace MHD equations, it is not immediately obvious what the optimum way is to describe the desired MHD situation with a GD code. Test case analysis shows that for quasi-perpendicular shocks it is safest to use the magnetospheric Mach number as an input to the GD code. It is also shown that when comparing GD predicted temperatures with MHD predicted temperatures total energy should be compared since the magnetic energy density provides a significant fraction of the internal energy of the MHD fluid for typical solar wind parameters. Some conclusions are also offered on the properties of the terrestrial shock.

  10. HIGH-TEMPERATURE PROCESSING OF SOLIDS THROUGH SOLAR NEBULAR BOW SHOCKS: 3D RADIATION HYDRODYNAMICS SIMULATIONS WITH PARTICLES

    SciTech Connect

    Boley, A. C.; Morris, M. A.; Desch, S. J.

    2013-10-20

    A fundamental, unsolved problem in solar system formation is explaining the melting and crystallization of chondrules found in chondritic meteorites. Theoretical models of chondrule melting in nebular shocks have been shown to be consistent with many aspects of thermal histories inferred for chondrules from laboratory experiments; but, the mechanism driving these shocks is unknown. Planetesimals and planetary embryos on eccentric orbits can produce bow shocks as they move supersonically through the disk gas, and are one possible source of chondrule-melting shocks. We investigate chondrule formation in bow shocks around planetoids through three-dimensional radiation hydrodynamics simulations. A new radiation transport algorithm that combines elements of flux-limited diffusion and Monte Carlo methods is used to capture the complexity of radiative transport around bow shocks. An equation of state that includes the rotational, vibrational, and dissociation modes of H{sub 2} is also used. Solids are followed directly in the simulations and their thermal histories are recorded. Adiabatic expansion creates rapid cooling of the gas, and tail shocks behind the embryo can cause secondary heating events. Radiative transport is efficient, and bow shocks around planetoids can have luminosities ∼few× 10{sup –8} L{sub ☉}. While barred and radial chondrule textures could be produced in the radiative shocks explored here, porphyritic chondrules may only be possible in the adiabatic limit. We present a series of predicted cooling curves that merit investigation in laboratory experiments to determine whether the solids produced by bow shocks are represented in the meteoritic record by chondrules or other solids.

  11. Stellar Bow Shocks in the Northern Arm of the Galactic Center: More Members and Kinematics of the Massive Star Population

    NASA Astrophysics Data System (ADS)

    Tanner, A.; Ghez, A. M.; Morris, M. R.; Christou, J. C.

    2005-05-01

    We present new 2.2 μm diffraction-limited images from the W. M. Keck 10 m and Gemini 8 m telescopes of the cool Galactic center sources, IRS 1W, 5, 8, 10W, and 21, along with new proper motions for IRS 1W, 10W, and 21. These observations were carried out to test the bow shock hypothesis presented by Tanner et al. as an alternative to a very recent (104 yr) epoch of star formation within the tidal stream of gas and dust known as the northern arm. Resolved asymmetric structure is detected in all the sources, with bow shock morphologies associated with IRS 1W, 5, 8, and 10W. For IRS 1W and 10W, there is an agreement between the position angle of the asymmetry and that of the inferred relative velocity vector of the near-infrared source with respect to the northern arm gas, strengthening the bow shock hypothesis. We therefore conclude that the observed morphology is indeed a bow shock generated by sources plowing through the northern arm. Furthermore, the large extent of the resolved structures (310-1340 AU), along with their luminosities (~104-105 Lsolar), suggests that their central sources are Wolf-Rayet stars, comparable to the broad He emission-line stars, which have strong winds on the order of 1000 km s-1. The bow shock geometry, along with the proper motion measurements, provide three-dimensional orbital solutions for this enigmatic class of objects. The orientations of the orbital planes of IRS 1W and 10W are consistent with that of the putative clockwise plane which has been proposed as a solution for the He I emission-line stars. While these observations eliminate the need to invoke star formation within the northern arm, they increase by 10% the total known population of massive, young stars with strong winds, whose origin remains unexplained in the context of the nearby supermassive black hole.

  12. The Very High Alfvén Mach Number Bow Shock of Saturn

    NASA Astrophysics Data System (ADS)

    Sulaiman, A.; Masters, A.; Dougherty, M. K.

    2014-12-01

    Collisionless shock waves are ubiquitous in the universe and fundamental to understanding the nature of collisionless plasmas. The interplay between particles (ions and electrons) and fields (electromagnetic) introduces a variety of both physical and geometrical parameters such as Mach numbers (e.g. MA, Mf), β, and θbn. These vary drastically from terrestrial to astrophysical regimes resulting in radically different characteristics of shocks. This poses two complexities. Firstly, separating the influences of these parameters on physical mechanisms such as energy dissipation. Secondly, correlating observations of shock waves over a wide range of each parameter, enough to span across different regimes. Investigating the latter has been restricted since the majority of studies on shocks at exotic regimes (such as supernova remnants) have been achieved either remotely or via simulations, but rarely by means of in-situ observations. It is not clear what happens in the higher MA regime. Here we show the parameter space of MA for all bow shock crossings from 2004-2012 as measured by the Cassini spacecraft. We found that the Saturnian bow shock exhibits characteristics akin to both terrestrial and astrophysical regimes (MA of order 100), which is principally controlled by the upstream magnetic field strength. Moreover, we estimated the θbn­ of each crossing and were able to further constrain the sample into categories of similar features. Our results demonstrate how MA plays a central role in controlling the onset of physical mechanisms in collisionless shocks, particularly instabilities, non-time stationarity and electron acceleration. We anticipate our comprehensive assessment to give deeper insight to high MA collisionless shocks and provide a broader scope for understanding the structures and mechanisms of collisionless shocks. This can potentially bridge the gap between more modest MA observed in near-Earth space and more exotic astrophysical regimes where shock

  13. Using Collaborative Modeling to Inform Policy Decisions in the Bow River Basin

    NASA Astrophysics Data System (ADS)

    Sheer, A. S.; Sheer, D. P.; Hill, D.

    2011-12-01

    The Bow River in Alberta, Canada serves a wide range of municipal, agricultural, recreational, and industrial purposes in the province. In 2006, the basin was deemed over-allocation and closed to new licenses. The Calgary region, however, continues to expand. In the next 60 to 70 years, population levels are expected to reach 2.8 million (more than double the current 1.2 million) with 800,000 new jobs. This increasing pressure led several stakeholders to work together in the development of a new management model to improve the management of the system as an integrated watershed. The major previous model of the system allowed only limited flexibility in management, focusing instead on strict license based operations. Over a 6 month period, with numerous multi-party meetings, the group developed the Bow River Operations Model (BROM). Based in OASIS software, this model integrated input from the major water users in the region to emulate the real-life decisions that are actually made on a daily bases, even when technically in violation of the strict license agreements (e.x. junior licensees receiving water despite senior priority due to exceedingly low volume requirements). Using historical records as forecasts, and performance measures developed with the best available science through expert opinion, participants jointly developed a new reservoir operation strategy. Even with such a short timeframe, the BROM exercise showed that there was substantial room for improvement. Utilizing a "Water Bank" of purchased storage, downstream flows could be significantly improved without affecting quality. Additional benefits included fishery improvement, new recreation opportunities, dissolved oxygen improvement during critical periods, and the ability to accommodate long-term demand forecasts for surrounding municipalities. This strategy has been presented to, and favorably received by, the Alberta Minister of Environment for guidance during negotiations with the local

  14. ION ACCELERATION AT THE QUASI-PARALLEL BOW SHOCK: DECODING THE SIGNATURE OF INJECTION

    SciTech Connect

    Sundberg, Torbjörn; Haynes, Christopher T.; Burgess, D.; Mazelle, Christian X.

    2016-03-20

    Collisionless shocks are efficient particle accelerators. At Earth, ions with energies exceeding 100 keV are seen upstream of the bow shock when the magnetic geometry is quasi-parallel, and large-scale supernova remnant shocks can accelerate ions into cosmic-ray energies. This energization is attributed to diffusive shock acceleration; however, for this process to become active, the ions must first be sufficiently energized. How and where this initial acceleration takes place has been one of the key unresolved issues in shock acceleration theory. Using Cluster spacecraft observations, we study the signatures of ion reflection events in the turbulent transition layer upstream of the terrestrial bow shock, and with the support of a hybrid simulation of the shock, we show that these reflection signatures are characteristic of the first step in the ion injection process. These reflection events develop in particular in the region where the trailing edge of large-amplitude upstream waves intercept the local shock ramp and the upstream magnetic field changes from quasi-perpendicular to quasi-parallel. The dispersed ion velocity signature observed can be attributed to a rapid succession of ion reflections at this wave boundary. After the ions’ initial interaction with the shock, they flow upstream along the quasi-parallel magnetic field. Each subsequent wavefront in the upstream region will sweep the ions back toward the shock, where they gain energy with each transition between the upstream and the shock wave frames. Within three to five gyroperiods, some ions have gained enough parallel velocity to escape upstream, thus completing the injection process.

  15. Anatomy of the internal bow shocks in the IRAS 04166+2706 protostellar jet

    NASA Astrophysics Data System (ADS)

    Tafalla, M.; Su, Y.-N.; Shang, H.; Johnstone, D.; Zhang, Q.; Santiago-García, J.; Lee, C.-F.; Hirano, N.; Wang, L.-Y.

    2017-01-01

    Context. Highly collimated jets and wide-angle outflows are two related components of the mass-ejection activity associated with stellar birth. Despite decades of research, the relation between these two components remains poorly understood. Aims: We study the relation between the jet and the outflow in the IRAS 04166+2706 protostar. This Taurus protostar drives a molecular jet that contains multiple emission peaks symmetrically located from the central source. The protostar also drives a wide-angle outflow consisting of two conical shells. Methods: We have used the Atacama Large Millimeter/submillimeter Array (ALMA) interferometer to observe two fields along the IRAS 04166+2706 jet. The fields were centered on a pair of emission peaks that correspond to the same ejection event. The observations were carried out in CO(2-1), SiO(5-4), and SO(JN = 65-54). Results: Both ALMA fields present spatial distributions that are approximately elliptical and have their minor axes aligned with the jet direction. As the velocity increases, the emission in each field moves gradually across the elliptical region. This systematic pattern indicates that the emitting gas in each field lies in a disk-like structure that is perpendicular to the jet axis and whose gas is expanding away from the jet. A small degree of curvature in the first-moment maps indicates that the disks are slightly curved in the manner expected for bow shocks moving away from the IRAS source. A simple geometrical model confirms that this scenario fits the main emission features. Conclusions: The emission peaks in the IRAS 04166+2706 jet likely represent internal bow shocks where material is being ejected laterally away from the jet axis. While the linear momentum of the ejected gas is dominated by the component in the jet direction, the sideways component is not negligible, and can potentially affect the distribution of gas in the surrounding outflow and core.

  16. Plasma and wave properties downstream of Martian bow shock: Hybrid simulations and MAVEN observations

    NASA Astrophysics Data System (ADS)

    Dong, Chuanfei; Winske, Dan; Cowee, Misa; Bougher, Stephen W.; Andersson, Laila; Connerney, Jack; Epley, Jared; Ergun, Robert; McFadden, James P.; Ma, Yingjuan; Toth, Gabor; Curry, Shannon; Nagy, Andrew; Jakosky, Bruce

    2015-04-01

    Two-dimensional hybrid simulation codes are employed to investigate the kinetic properties of plasmas and waves downstream of the Martian bow shock. The simulations are two-dimensional in space but three dimensional in field and velocity components. Simulations show that ion cyclotron waves are generated by temperature anisotropy resulting from the reflected protons around the Martian bow shock. These proton cyclotron waves could propagate downward into the Martian ionosphere and are expected to heat the O+ layer peaked from 250 to 300 km due to the wave-particle interaction. The proton cyclotron wave heating is anticipated to be a significant source of energy into the thermosphere, which impacts atmospheric escape rates. The simulation results show that the specific dayside heating altitude depends on the Martian crustal field orientations, solar cycles and seasonal variations since both the cyclotron resonance condition and the non/sub-resonant stochastic heating threshold depend on the ambient magnetic field strength. The dayside magnetic field profiles for different crustal field orientation, solar cycle and seasonal variations are adopted from the BATS-R-US Mars multi-fluid MHD model. The simulation results, however, show that the heating of O+ via proton cyclotron wave resonant interaction is not likely in the relatively weak crustal field region, based on our simplified model. This indicates that either the drift motion resulted from the transport of ionospheric O+, or the non/sub-resonant stochastic heating mechanism are important to explain the heating of Martian O+ layer. We will investigate this further by comparing the simulation results with the available MAVEN data. These simulated ion cyclotron waves are important to explain the heating of Martian O+ layer and have significant implications for future observations.

  17. Ion Acceleration at the Quasi-parallel Bow Shock: Decoding the Signature of Injection

    NASA Astrophysics Data System (ADS)

    Sundberg, Torbjörn; Haynes, Christopher T.; Burgess, D.; Mazelle, Christian X.

    2016-03-01

    Collisionless shocks are efficient particle accelerators. At Earth, ions with energies exceeding 100 keV are seen upstream of the bow shock when the magnetic geometry is quasi-parallel, and large-scale supernova remnant shocks can accelerate ions into cosmic-ray energies. This energization is attributed to diffusive shock acceleration however, for this process to become active, the ions must first be sufficiently energized. How and where this initial acceleration takes place has been one of the key unresolved issues in shock acceleration theory. Using Cluster spacecraft observations, we study the signatures of ion reflection events in the turbulent transition layer upstream of the terrestrial bow shock, and with the support of a hybrid simulation of the shock, we show that these reflection signatures are characteristic of the first step in the ion injection process. These reflection events develop in particular in the region where the trailing edge of large-amplitude upstream waves intercept the local shock ramp and the upstream magnetic field changes from quasi-perpendicular to quasi-parallel. The dispersed ion velocity signature observed can be attributed to a rapid succession of ion reflections at this wave boundary. After the ions’ initial interaction with the shock, they flow upstream along the quasi-parallel magnetic field. Each subsequent wavefront in the upstream region will sweep the ions back toward the shock, where they gain energy with each transition between the upstream and the shock wave frames. Within three to five gyroperiods, some ions have gained enough parallel velocity to escape upstream, thus completing the injection process.

  18. Unusual locations of Earth's bow shock on September 24 - 25, 1987: Mach number effects

    NASA Technical Reports Server (NTRS)

    Cairns, Iver H.; Fairfield, Donald H.; Anderson, Oger R.; Carlton, Victoria E. H.; Paularena, Karolen I.; Lazarus, Alan J.

    1995-01-01

    International Sun Earth Explorer 1 (ISEE 1) and Interplanetary Monitoring Platform 8 (IMP 8) data are used to identify 19 crossings of Earth's bow shock during a 30-hour period following 0000 UT on September 24, 1987. Apparent standoff distances for the shock are calculated for each crossing using two methods and the spacecraft location; one method assumes the average shock shape, while the other assumes a ram pressure-dependent shock shape. The shock's apparent standoff distance, normally approximately 14 R(sub E), is shown to increase from near 10 R(sub E) initially to near 19 R(sub E) during an 8-hour period, followed by an excursion to near 35 R(sub E) (where two IMP 8 shock crossings occur) and an eventual return to values smaller than 19 R(sub E). The Alfven M(sub A) and fast magnetosonic M(sub ms). Mach numbers remain above 2 and the number density above 4/cu cm for almost the entire period. Ram pressure effects produce the initial near-Earth shock location, whereas expansions and contractions of the bow shock due to low Mach number effects account, qualitatively and semiquantitatively, for the timing and existence of almost all the remaining ISEE crossings and both IMP 8 crossings. Significant quantitative differences exist between the apparent standoff distances for the shock crossings and those predicted using the observed plasma parameters and the standard model based on Spreiter et al.'s (1966) gasdynamic equation. These differences can be explained in terms of either a different dependence of the standoff distance on Mach number at low M(sub A) and M(sub ms), or variations in shock shape with M(sub A) and M(sub ms) (becoming increasingly "puffed up" with decreasing M(sub A) and M(sub ms), as expected theoretically), or by a combination of both effects.

  19. Neutron Star Kinematics: Pulsar Parallaxes, Bow Shock Nebulae and the Interstellar Medium

    NASA Astrophysics Data System (ADS)

    Chatterjee, S.

    2003-12-01

    The measurement of distances is a fundamental problem in astronomy. Parallaxes and proper motions of pulsars provide model-independent estimates of their distances and velocities, allowing us to probe the physics of neutron stars, constrain core collapse phenomena in supernovae, and investigate the distribution of matter in the interstellar medium. Here we present high-precision measurements of the trigonometric parallaxes and proper motions of three radio pulsars using the NRAO Very Long Baseline Array, and discuss how they have been used to investigate the interstellar medium, as well as the birth sites, cooling curves, and velocity distribution of neutron stars. Bow shocks and pulsar wind nebulae probe the interaction of neutron star relativistic winds with the interstellar medium. We utilize scaling laws derived for bow shock nebulae, in combination with estimates of neutron star distances and velocities, to extract information about the interstellar medium. The spectacular Guitar nebula, produced by a high velocity but otherwise unremarkable neutron star, was observed at two epochs with the Hubble Space Telescope. We report time evolution in the position and morphology of the nebula, and infer the existence of small scale density fluctuations in the interstellar medium. Increases in the sample of precise astrometric measurements will enable many such scientific applications: we introduce an ongoing project with the Very Long Baseline Array, which is expected to at least double the number of measured pulsar parallaxes in the next two years. This work was supported in part by NSF grants AST 9819931 and AST 0206036 to Cornell University. NRAO is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. Observations made with the NASA/ESA Hubble Space Telescope were obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc.

  20. Metabolic Effects of the pksCT Gene on Monascus aurantiacus Li As3.4384 Using Gas Chromatography--Time-of-Flight Mass Spectrometry-Based Metabolomics.

    PubMed

    Huang, Zhibing; Zhang, Shuyun; Xu, Yang; Li, Laisheng; Li, Yanping

    2016-02-24

    Monascus spp. have been used for the production of natural pigments and bioactive compounds in China for several centuries. Monascus can also produce the mycotoxin citrinin, restricting its use. Disruption of the pksCT gene in Monascus aurantiacus Li AS3.4384 reduces citrinin production capacity of this strain (Monascus PHDS26) by over 98%. However, it is unclear how other metabolites of M. aurantiacus Li AS3.4384 (the wild-type strain) are affected by the pksCT gene. Here, we used metabolomic analyses to compare red yeast rice (RYR) metabolite profiles of the wild-type strain and Monascus PHDS26 at different stages of solid-state fermentation. A total of 18 metabolites forming components within the glycolysis, acetyl-CoA, amino acid, and tricarboxylic acid (TCA) cycle metabolic processes were found to be altered between the wild-type strain and Monascus PHDS26 at different stages of solid-state fermentation. Thus, these findings provide important insights into the metabolic pathways affected by the pksCT gene in M. aurantiacus.