The principal paradigm for gamma-ray bursts (GRBs) suggests that the prompt
transient gamma-ray signal arises from multiple shocks internal to the
relativistic expansion. Since this signal is most probably electromagnetic
in origin, a major issue concerns how the electrons get energized and
accelerated in burst environments. This paper explores this issue of
electron heating/acceleration at relativistic shocks that pertain to GRB
models. Spectral fits to BATSE/EGRET burst data indicate that the
preponderance of electrons that are responsible for the prompt emission
reside in an intrinsically non-thermal population. Thisdiffers markedly from typical populations generated in acceleration
simulations; potential resolutions of this conflict such as the action of
self-absorption are discussed. In addition, the spectral analysissuggests that the synchrotron mechanism is favored over synchrotron
self-Compton scenarios due to the latter$apos;s characteristically broad
curvature near the spectral \"peak.\" The merits of other emission
processes are also touched upon. A connection of this data interpretation
to heating in the shock layer is then made. Expectations for heating of
electrons from cross shock electrostatic potentials are
presented, exploring the capability of relativistic shocks to generate
predominantly non-thermal electron distributions from thermal poolsupstream. Constraints that the EGRET power-law indices provide on the
shock parameters will also be discussed.
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