Electron Acceleration In Relativistic GRB Shocks

Details Electron Acceleration In Relativistic GRB Shocks Electron Acceleration In Relativistic GRB Shocks

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.1321m&link_type=abstract

American Astronomical Society, HEAD meeting #9, #13.21; Bulletin of the American Astronomical Society, Vol. 38, p.369

Astronomy and Astrophysics

Astronomy

Scientific paper

The shock model of gamma-ray bursts (GRBs) contains two equipartition parameters: the magnetic energy density and the kinetic energy density of the electrons relative to the total energy density of the shock, ɛB and ɛe, respectively. These are free parameters within the model. Whereas the Weibel shock theory and numerical simulations fix ɛB at the level of few x(10-3...10-4), no understanding of ɛe exists so far. Here we demonstrate that is inevitably follows from the Weibel shock theory that ɛe (ɛB)1/2. The GRB afteglow data fully agree with this theoretical prediction. Our result explains why the electrons are close to equipartition in GRBs. The ɛe--ɛB relation can be used to reduce the number of free parameters in afterglow models.

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