<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Mastichiadis, A.</style></author><author><style face="normal" font="default" size="100%">Kazanas, D.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">The supercritical pile model for GRBs</style></title><short-title><style face="normal" font="default" size="100%">Advances in Space Research</style></short-title></titles><dates><year><style  face="normal" font="default" size="100%">2007</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2007/01/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2007AdSpR..40.1250M</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">40</style></volume><pages><style face="normal" font="default" size="100%">1250 - 1254</style></pages><isbn><style face="normal" font="default" size="100%">0273-1177</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We present the basic notions of the &quot;Supercritical Pile&quot; model of Gamma Ray Bursts (GRBs). This model is motivated by the need for a process that provides the dissipation necessary in GRBs and presents a well defined scheme for converting the energy stored in the relativistic protons of the Relativistic Blast Waves (RBW) associated with GRB into radiation; at the same time it leads to spectra which exhibit a peak in the burst νF&lt;SUB&gt;ν&lt;/SUB&gt; distribution at an energy E&lt;SUB&gt;p&lt;/SUB&gt; ≃ 1 MeV in the observer's frame, in agreement with observation and largely independent of the Lorentz factor Γ of the associated relativistic outflow.</style></abstract></record></records></xml>