Volume 462, Number 1, January IV 2007
|Page(s)||173 - 177|
|Section||Interstellar and circumstellar matter|
|Published online||24 October 2006|
A two-zone model for the emission from RX J1713.7-3946
Department of Physics, University of Athens, Panepistimiopolis, 15783 Zografos, Athens, Greece e-mail: firstname.lastname@example.org
Accepted: 29 September 2006
Aims.We study the acceleration and radiation of charged particles in the shock waves of supernova remnants using a recent version of the “box model”. 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.
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.
Results.The application of the model to the supernova remnant RX J1713.7-3946, 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.
Key words: acceleration of particles / cosmic rays / radiation mechanisms: non-thermal / ISM: supernova remnants
© ESO, 2007
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