Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.1324l&link_type=abstract
American Astronomical Society, HEAD meeting #9, #13.24; Bulletin of the American Astronomical Society, Vol. 38, p.370
Astronomy and Astrophysics
Astronomy
Scientific paper
Using a new Particle-in-Cell code that includes self-consistent radiation processes, we have simulated the radiation output from electrons accelerated by Poynting flux, and by magnetized and nonmagnetic relativistic collisionless shocks. We discover that the radiation mechanism is different in each case, but none of which resembles classical synchrotron radiation. In pure Poynting flux acceleration the power output and critical frequency depend only on the electron momentum along the transverse electric field, and are many orders of magnitude below those of synchrotron radiation. In nonmagnetic shocks electrons are mainly accelerated by longitudinal electric fields and radiation is negligible. The radiation power is strongest in the case of strongly magnetized shocks, as the electrons are accelerated by the ponderomotive force. We apply these results to the interpretation of both prompt and afterglow data of GRBs.
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