Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aipc..836..137k&link_type=abstract
GAMMA-RAY BURSTS IN THE SWIFT ERA: Sixteenth Maryland Astrophysics Conference. AIP Conference Proceedings, Volume 836, pp. 137-
Astronomy and Astrophysics
Astrophysics
1
Gamma-Ray Sources, Gamma-Ray Bursts, Elementary Particle Processes
Scientific paper
The essence of the ``Supercritical Pile'' GRB model is a process for converting the energy stored in the relativistic protons of a Relativistic Blast Wave (RBW) of Lorentz factor Γ into electron - positron pairs of similar Lorentz factor. This is achieved by scattering the synchrotron radiation emitted by the RBW in an upstream located ``mirror'' and then re-intercepting it by the RBW. The repeated scatterings of radiation between the RBW and the ``mirror'', along with the threshold of the pair production reaction pγ --> pe-e+, lead to a maximum in the GRB spectral luminosity at an energy Ep ~= 1 MeV, in general agreement with observation, independent of the value of Γ. Furthermore, the same threshold implies that the prompt γ-ray emission is only possible for Γ larger than a minimum value, thereby providing a ``natural'' account for the termination of this stage of the GRB as the RBW slows down. Within this model the γ-ray (E ~ 100 keV - 1 MeV) emission process is due to bulk Inverse Compton scattering and it is thus expected to be highly polarized if viewed at angles θ ~= 1/Γ to the direction of the RBW. We have simulated the process of spectral formation by following the time development of the proton, electron and photon distribution functions. We present the results these calculations.
Georganopoulos Markos
Kazanas Demosthenes
Mastichiadis Apostolos
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