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  • Other Sources  (5)
  • Astrophysics  (5)
  • 2005-2009  (5)
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  • Other Sources  (5)
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  • 1
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    All-Sky Hard X-Ray Spectral Line Survey with EXIST (2006)
    In:  Other Sources
    Details
    Publication Date: 2018-06-12
    Description: The Energetic X-ray Imaging Survey Telescope (EXIST), under study to be the Black Hole Finder Probe in NASA's Beyond Einstein Program, would image the sky every 95 min in the energy range 10-600 keV. Although the main scientific objectives of EXIST are the systematic, all-sky survey of heavily obscured AGNs and gamma-ray bursts, there is a substantial capability of EXIST for the observation of transient and persistent hard X-ray lines from several astrophysical sources.
    Keywords: Astrophysics
    Type: New Astronomy Reviews (ISSN 1387-6473); Volume 50; 637-639
    Format: text
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  • 2
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    Microscopic Processes in Relativistic Jets (2008)
    In:  Other Sources
    Details
    Publication Date: 2019-07-19
    Description: Nonthermal radiation observed from astrophysical systems containing relativistic jets and shocks, e.g., gamma-ray bursts (GRBs), active galactic nuclei (AGNs), and Galactic microquasar systems usually have power-law emission spectra. Recent PIC simulations of relativistic electron-ion (electro-positron) jets injected into a stationary medium show that particle acceleration occurs within the downstream jet. In the collisionless relativistic shock particle acceleration is due to plasma waves and their associated instabilities (e.g., the Buneman instability, other two-streaming instability, and the Weibel (filamentation) instability) created in the shocks are responsible for particle (electron, positron, and ion) acceleration. The simulation results show that the Weibel instability is responsible for generating and amplifying highly nonuniform, small-scale magnetic fields. These magnetic fields contribute to the electron's transverse deflection behind the jet head. The 'jitter' radiation from deflected electrons has different properties than synchrotron radiation which is calculated in a uniform magnetic field. This jitter radiation may be important to understanding the complex time evolution and/or spectral structure in gamma-ray bursts, relativistic jets, and supernova remnants.
    Keywords: Astrophysics
    Type: MSFC-2129 , Kinetic Modeling of Astrophysical Plasmas; Oct 05, 2008 - Oct 09, 2008; Cracow; Poland
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    NASA TECHNICAL REPORTS
  • 3
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    Microscopic Processes On Radiation from Accelerated Particles in Relativistic Jets (2009)
    In:  Other Sources
    Details
    Publication Date: 2019-07-19
    Description: Nonthermal radiation observed from astrophysical systems containing relativistic jets and shocks, e.g., gamma-ray bursts (GRBs), active galactic nuclei (AGNs), and Galactic microquasar systems usually have power-law emission spectra. Recent PIC simulations of relativistic electron-ion (electro-positron) jets injected into a stationary medium show that particle acceleration occurs within the downstream jet. In the collisionless relativistic shock particle acceleration is due to plasma waves and their associated instabilities (e.g., the Buneman instability, other two-streaming instability, and the Weibel (filamentation) instability) created in the shocks are responsible for particle (electron, positron, and ion) acceleration. The simulation results show that the Weibel instability is responsible for generating and amplifying highly nonuniform, small-scale magnetic fields. These magnetic fields contribute to the electron's transverse deflection behind the jet head. The jitter'' radiation from deflected electrons has different properties than synchrotron radiation which is calculated in a uniform magnetic field. This jitter radiation may be important to understanding the complex time evolution and/or spectral structure in gamma-ray bursts, relativistic jets, and supernova remnants.
    Keywords: Astrophysics
    Type: M09-0403 , Modern Challenges in Nonliner Plasma Physics; Jun 15, 2009 - Jun 19, 2009; Halkidiki; Greece
    Format: text
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  • 4
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    Relativistic Particle-In-Cell Simulations of Particle Accleration in Relativistic Jets (2008)
    In:  Other Sources
    Details
    Publication Date: 2019-07-19
    Description: Highly accelerated particles are observed in astrophysical systems containing relativistic jets and shocks, e.g., active galactic nuclei (AGNs), microquasars, and Gamma-Ray Bursts (GRBs). Particle-In-Cell (PIC) simulations of relativistic electron-ion and electron-positron jets injected into a stationary medium show that efficient acceleration occurs downstream in the jet. In collisionless relativistic shocks particle acceleration is due to plasma waves and their associated instabilities, e.g., the Buneman instability, other two-stream instabilities, and the Weibel (filamentation) instability. Simulations show that the Weibel instability is responsible for generating and amplifying highly non-uniform, small-scale magnetic fields. The instability depends on strength and direction of the magnetic field. Particles in relativistic jets may be accelerated in a complicated dynamics of relativistic jets with magnetic field. We present results of our recent PIC simulations.
    Keywords: Astrophysics
    Type: 37th COSPAR Scientific Assembly; Jul 13, 2008 - Jul 20, 2008; Montreal; Canada
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  • 5
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    GRMHD Simulations of Jet Formation with RAISHIN (2006)
    In:  Other Sources
    Details
    Publication Date: 2019-07-19
    Description: We have developed a new three dimensional general relativistic magnetohydrodynamic (GRMHD) code, RAISHIN, using a conservative, high-resolution shock capturing scheme. Numerical fluxes are calculated using the Harten, Lax, & van Leer (HLL) approximate Riemann solver scheme. The flux-interpolated, constrained transport scheme is used to maintain a divergence-free magnetic field. We describe code performance on some test problems in both special and general relativity. Our new GRMHD code has proven to be accurate to second order and has successfully passed several numerical test problems including highly relativistic and magnetized tests in both special and general relativity. We have performed several simulations of non-rotating and rotating black hole systems with a geometrically thin accretion disk. The simulations show the formation of jets driven by the Lorentz force and the gas pressure. It appears that the rotating black hole creates an additional faster, and more collimated outflow inside a broader, slower outflow that is also generated by the rotating accretion disk around a non-rotating black hole. The kinematic jet structure could thus be a sensitive function of black hole rotation.
    Keywords: Astrophysics
    Type: The 6th INTEGRAL Workshop: The Obscured Universe; Jul 02, 2006 - Jul 08, 2006; Moscow; Russia
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