A two-zone model for the emission from RX J1713.7-3946

Free access article

Issue		A&A Volume 462, Number 1, January IV 2007


Page(s)		173 - 177
Section		Interstellar and circumstellar matter
DOI		http://dx.doi.org/10.1051/0004-6361:20065725

A&A 462, 173-177 (2007)
DOI: 10.1051/0004-6361:20065725

A two-zone model for the emission from RX J1713.7-3946

K. Moraitis and A. Mastichiadis

Department of Physics, University of Athens, Panepistimiopolis, 15783 Zografos, Athens, Greece
e-mail: kmorait@phys.uoa.gr

(Received 30 May 2006 / Accepted 29 September 2006)

Abstract
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 $\gamma$ -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

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