Shock Emission Model for Gamma-Ray Bursts

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Abstract
We discuss an emission model for classical gamma-ray bursts (GRBs) based on impulsively driven MHD relativistic winds shocked by interactions in optically thin environments. We show that GRB spectra can be modeled by synchrotron radiation of relativistic particles accelerated by a very efficient shock mechanism from a preshock Maxwellian distribution. In its simplest realization, the model predicts a quasiuniversal spectrum consistent with recently determined broadband spectra of bright GRBs. The emission model is applicable to both cosmological and galactic interpretations of GRBs. We discuss future tests aimed at clarifying the nature of the acceleration process in GRBs.