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We examine the prompt and afterglow emission within the context of theSupercritical Pile model for GRBs. For this we have performed self-consistentcalculations, by solving three time-dependent kinetic equations for protons,electrons and photons in addition to the usual mass and energy conservationequations. We follow the evolution of the RBW as it sweeps up circumstellarmatter and assume that the swept-up electrons and protons have energies equalto the Lorentz factor of the flow. While the electrons radiate their energiesthrough synchrotron and inverse Compton radiation on short timescales, theprotons, at least initially, start accumulating without any dissipation. As theaccumulated mass of relativistic protons increases, however, they can becomesupercritical to the `proton-photon pair-production - synchrotron radiation'network, and, as a consequence, they transfer explosively their stored energyto secondary electron-positron pairs and radiation. This results in a burstwhich has many features similar to the ones observed in GRB prompt emission. Wehave included in our calculations the radiation drag force exerted on the flowfrom the scattered radiation of the prompt emission on the circumstellarmaterial. We find that this can decelerate the flow on timescales which aremuch faster than the ones related to the usual adiabatic/radiative ones. As aresult the emission exhibits a steep drop just after the prompt phase, inagreement with the Swift afterglow observations.

Compton dragged supercritical piles: The GRB prompt and afterglow scenario