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K.-I. Nishikawa (NSSTC), P. Hardee (Univ. of Alabama, Tuscaloosa), R. Preece, G. Richardson, G. Fishman (NSSTC)
Shock accelerations are ubiquitous phenomena in astrophysical plasmas. Recently several particle simulations have been performed to investigate electron acceleration in shocks. Electromagnetic waves (e.g., Buneman instability, two-streaming, Weibel instabilities) created in the shock transition regions are responsible for electron acceleration. The simulations of relativistic jets using a 3-D relativistic electromagnetic particle (REMP) code have shown particle acceleration in the shock transition regions. Simulations show that the electromagnetic waves (Weibel instability) created at the shock front propagate backward with increasing magnitude. The resulting enhanced waves accelerate particles perpendicular to the jet propagation direction. The acceleration rates depend on the size and composition of the jets, and the strength and direction of ambient magnetic fields. We will present simulation results with thin and thick jets with electron-positron and electron-ion composition.
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The author(s) of this abstract have provided an email address for comments about the abstract: Ken-Ichi.Nishikawa@nsstc.nasa.gov
Bulletin of the American Astronomical Society,
© 2003. The American Astronomical Soceity.