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K.-I. Nishikawa, G. Richardson, R. Preece (NSSTC), P. Hardee (Univ. Alabama, Tuscaloosa), J. Fishman (NSSTC)
Shock accelerations are ubiquitous phenomena in magnetospheric, solar, and astrophysical plasmas. Recently several 1-D particle simulations have been performed to investigate shock surfing acceleration of electrons. Electrostatic waves (e.g., Buneman instability, two-streaming instability) created in the shock transition regions are responsible for electron acceleration. New simulations of relativistic jets using a 3-d relativistic electromagnetic particle (REMP) code have shown particle acceleration in the shock transition regions and internal shocks. Simulations show that the electrostatic waves 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.
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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
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.