Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.1326k&link_type=abstract
American Astronomical Society, HEAD meeting #9, #13.26; Bulletin of the American Astronomical Society, Vol. 38, p.370
Astronomy and Astrophysics
Astronomy
Scientific paper
A recent model that details the dissipation of the energy stored in the protons of the Relativistic Blast Waves (RBW) of GRB, while at the same time provides a characteristic peak in their $\nu F_{\nu}$ spectra, is extended to include their transition into the afterglow. The model still employs the $p \gamma \rightarrow p e^+e^-$ reaction to convert the proton energy into electrons, however, in addition to its earlier version that considered only a (relativistic) Maxwellian proton distribution behind the RBW, it includes also a non-thermal, power-paw population of such protons. The transition from the prompt to the afterglow emission takes place when, due to the decrease in the RBW Lorentz factor $\Gamma(t)$, the protons in the Maxwellian part of the distribution function of energy $\sim \Gamma(t) m_pc^2$ cannot fulfill the threshold for $p \gamma \rightarrow p e^+e^-$ reaction, which however is still fulfilled by the protons of the power-law tail. It can be easily shown that the energy of peak $\nu F_{\nu}$ emission, $E_p$, shifts then from $E_p \sim 1$ MeV to a lower energy that decreases like $\sim \Gamma^2(t)$, marking the onset of the afterglow. GRB of sufficiently low initial $\Gamma$ for which the threshold condition is fulfilled at all times only by the protons of the power law distribution have $E_p \ll 1$ MeV and they would be called XRR or XRF. In addition, because of their lower values of $\Gamma$ their apparent luminosities and isotropic energy $E_{\rm iso}$ would be smaller than the normal GRB in general agreement with observation.
Georganopoulos Markos
Kazanas Demosthenes
Mastichiadis Apostolos
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