On Fermi vs. Non-fermi Electron Acceleration at Relativistic Shocks of GRBs

Details On Fermi vs. Non-fermi Electron Acceleration at Relativistic Shocks of GRBs On Fermi vs. Non-fermi Electron Acceleration at Relativistic Shocks of GRBs

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.4103m&link_type=abstract

American Astronomical Society Meeting 210, #41.03; Bulletin of the American Astronomical Society, Vol. 39, p.155

Astronomy and Astrophysics

Astronomy

Scientific paper

The shock model of gamma-ray bursts (GRBs) contains epsilone parameter which describes the fraction of the total shock energy (essentially, the proton energy density) is carried by the electrons. Both fits to GRB afterglows and numerical simulations of relativistic shocks indicate that epsilone is substantially larger than me/mp, --- the value one would expect if no energy transfer exists between protons and electrons. Here we consider several models of the electron acceleration, including electrostatic and induction electric fields, pinch effect and wave-particle interactions. We argue that one can expect that epsilone (epsilonB)1/2 for the bulk electrons, based on energy arguments. The GRB afteglow data agree with this theoretical prediction. We suggest that the epsilone-epsilonB relation can be used to reduce the number of free parameters in afterglow models.

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