<?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%">Moraitis, K.</style></author><author><style face="normal" font="default" size="100%">Mastichiadis, A.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A two-zone model for the emission from &lt;ASTROBJ&gt;RX J1713.7-3946&lt;/ASTROBJ&gt;</style></title><short-title><style face="normal" font="default" size="100%">Astronomy and Astrophysics</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">acceleration of particles</style></keyword><keyword><style  face="normal" font="default" size="100%">Astrophysics</style></keyword><keyword><style  face="normal" font="default" size="100%">cosmic rays</style></keyword><keyword><style  face="normal" font="default" size="100%">ISM: supernova remnants</style></keyword><keyword><style  face="normal" font="default" size="100%">radiation mechanisms: non-thermal</style></keyword></keywords><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/2007A&amp;A...462..173M</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">462</style></volume><pages><style face="normal" font="default" size="100%">173 - 177</style></pages><isbn><style face="normal" font="default" size="100%">0004-6361</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">Aims:We study the acceleration and radiation of charged particles in the shock waves of supernova remnants using a recent version of the &quot;box model&quot;. According to this, particles are accelerated in an energy-dependent region around the shock by the first order Fermi mechanism and lose energy through radiation. &lt;BR /&gt;Methods: The particle distribution function is obtained from a spatially averaged kinetic equation that treats the energy losses self-consistently. There exists also a second population that consists of those particles that escape behind the shock where they also radiate. The energy distribution of this population is calculated in a similar manner. &lt;BR /&gt;Results: The application of the model to the supernova remnant &lt;ASTROBJ&gt;RX J1713.7-3946&lt;/ASTROBJ&gt;, which was recently confirmed as a TeV source by HESS, shows that the X-ray emission can be attributed to electron synchrotron radiation while in γ-rays there are contributions from both electrons and protons, with protons playing the dominant role. Additionally, there are strong indications that particles diffuse in turbulence that has a Kolmogorov spectrum.</style></abstract></record></records></xml>