Physics
Scientific paper
Feb 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sgrb.confe..46n&link_type=abstract
Presented at the KITP Conference: Supernova and Gamma-Ray Burst Remnants, Feb 10, 2006, Kavli Institute for Theoretical Physics,
Physics
Scientific paper
Nonthermal radiation observed from astrophysical systems containing(relativistic) jets and shocks, e.g., supernova remnants, active galacticnuclei (AGNs), gamma-ray bursts (GRBs), and Galactic microquasar systemsusually have power-law emission spectra. Fermi acceleration is themechanism usually assumed for the acceleration of particles inastrophysical environments. Recent PIC simulations using injectedrelativistic electron-ion (electro-positron) jets show that accelerationoccurs within the downstream jet, rather than by the scattering ofparticles back and forth across the shock as in Fermi acceleration. Shockacceleration is a ubiquitous phenomenon in astrophysical plasmas. Plasmawaves and their associated instabilities (e.g., the Bunemaninstability, other two-streaming instability, and the Weibelinstability) created in the shocks are responsible for particle(electron, positron, and ion) acceleration. The simulation results showthat the Weibel instability is responsible for generating and amplifyinghighly nonuniform, small-scalemagnetic fields. These magnetic fields contribute to the electron'stransverse deflection behind the jet head. The "jitter' radiation fromdeflected electrons has different properties than synchrotron radiationwhich is calculated in a uniform magnetic field. This jitter radiation maybe important tounderstanding the complex time evolution and/or spectral structure ingamma-ray bursts, relativistic jets, and supernova remnants. We willreview recent PIC simulations which show particle acceleration in jets.
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