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Record 20 of 272
Microscopic Processes in Relativistic Jets
Author and Affiliation:
Nishikawa, K.-I.(NASA Marshall Space Flight Center, Huntsville, AL, United States)
Hardee, P.(NASA Marshall Space Flight Center, Huntsville, AL, United States)
Mizuno, Y.(NASA Marshall Space Flight Center, Huntsville, AL, United States)
Medvedev, M.(NASA Marshall Space Flight Center, Huntsville, AL, United States)
Zhang, B.(NASA Marshall Space Flight Center, Huntsville, AL, United States)
Nordlund, A.(NASA Marshall Space Flight Center, Huntsville, AL, United States)
Fredricksen, J.(NASA Marshall Space Flight Center, Huntsville, AL, United States)
Sol, H.(NASA Marshall Space Flight Center, Huntsville, AL, United States)
Niemiec, J.(NASA Marshall Space Flight Center, Huntsville, AL, United States)
Lyubarsky, Y.(NASA Marshall Space Flight Center, Huntsville, AL, United States) Show more authors
Abstract: 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.
Publication Date: Oct 05, 2008
Document ID:
20090014784
(Acquired Apr 16, 2009)
Subject Category: ASTROPHYSICS
Report/Patent Number: MSFC-2129
Document Type: Conference Paper
Meeting Information: Kinetic Modeling of Astrophysical Plasmas; 5-9 Oct. 2008; Cracow; Poland
Financial Sponsor: NASA Marshall Space Flight Center; Huntsville, AL, United States
Organization Source: NASA Marshall Space Flight Center; Huntsville, AL, United States
Description: 1p; In English
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: Copyright
NASA Terms: RELATIVISTIC PLASMAS; PLASMA JETS; ELECTROMAGNETIC RADIATION; ASTROPHYSICS; ELECTRON-POSITRON PLASMAS; PARTICLE ACCELERATION; EMISSION SPECTRA; POWER SPECTRA; MAGNETOHYDRODYNAMIC STABILITY; PLASMA WAVES; MAGNETIC FIELDS; GAMMA RAY BURSTS; ACTIVE GALACTIC NUCLEI; QUASARS; PARTICLE IN CELL TECHNIQUE
Availability Source: Other Sources
Availability Notes: Abstract Only
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