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Shock acceleration is an ubiquitous phenomenon in astrophysical plasmas.Plasma waves and their associated instabilities (e.g., the Buneman instability,two-streaming instability, and the Weibel instability) created in the shocksare responsible for particle (electron, positron, and ion) acceleration. Usinga 3-D relativistic electromagnetic particle (REMP) code, we have investigatedparticle acceleration associated with a relativistic jet front propagatingthrough an ambient plasma with and without initial magnetic fields. We findonly small differences in the results between no ambient and weak ambientmagnetic fields. Simulations show that the Weibel instability created in thecollisionless shock front accelerates particles perpendicular and parallel tothe jet propagation direction. The simulation results show that thisinstability is responsible for generating and amplifying highly nonuniform,small-scale magnetic fields, which contribute to the electron's transversedeflection behind the jet head. The ``jitter'' radiation from deflectedelectrons has different properties than synchrotron radiation which iscalculated in a uniform magnetic field. This jitter radiation may be importantto understanding the complex time evolution and/or spectral structure ingamma-ray bursts, relativistic jets, and supernova remnants.Comment: 4 pages, 1 figure, submitted to Proceedings of 2003 Gamma Ray Burst  Conferenc

Particle Acceleration and Radiation Associated with Magnetic Field Generation from Relativistic Collisionless Shocks