MG14 - Talk detail

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Abstract

We propose a model of Gamma-Ray Burst (GRB) prompt emission based on interaction of the GRB ejecta with a clumpy baryonic material, located outside the photospheric radius of the ejecta. The role of the material is to convert a small fraction of kinetic energy of GRB ejecta into seed thermal emission in the extreme UV - soft X-ray band. This thermal radiation field efficiently decelerates the GRB ejecta, while upscattered off the ejecta electrons. We discuss how this model naturally predicts the peak energy in the 10 keV – 1 MeV range. We also discuss the spectral shape of the prompt emission as well as its variability. We found that stellar winds from massive stars prior to their explosions may very likely produce such baryonic material. The proposed model leads to the identification of the prompt emission mechanism with inverse Compton scattering.

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