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D. Kazanas (NASA/GSFC), A. Mastichiadis (University of Athens, Greece), M. Georganopoulos (UMBC)
We present the spectral and temporal signatures of the prompt Gamma Ray Burst (GRB) emission expected within the ``Supercritical Pile" GRB model. This model is motivated by the need for a process that provides the dissipation necessary in GRB and presents a well defined scheme for converting the energy stored in the (relativistically) thermal protons of the Relativistic Blast Wave (RBW) associated with GRB into radiation; at the same time it leads to spectra which exhibit a peak in the burst luminosity at an energy approximately 1 MeV in the observer's frame, in agreement with observation and largely independent of the Lorentz factor \Gamma of the associated relativistic outflow. Futhermore, this scheme does not require (but does not preclude either) acceleration of particles at the shock other than that provided by the isotropization of the flow bulk kinetic energy on the RBW frame. We model in detail the evolution of protons, electrons and photons from a RBW to produce detailed spectra of the prompt GRB phase as a function of time across a very broad range spanning roughly 4 Log10 \Gamma decades in frequency. The model spectra are in general agreement with observations and provide a means for the delineating of the model parameters through direct comparison with trends observed in GRB properties.
The author(s) of this abstract have provided an email address for comments about the abstract: Demos.Kazanasemail@example.com
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.