Journal Article

Hadronic γ-ray images of Sedov supernova remnants

V. Beshley and O. Petruk

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 419, issue 2, pages 1421-1430
Published in print January 2012 | ISSN: 0035-8711
Published online December 2011 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2011.19799.x
Hadronic γ-ray images of Sedov supernova remnants

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A number of modern experiments in high-energy astrophysics produce images of supernova remnants (SNRs) in the TeV and GeV γ-rays. Either relativistic electrons (due to the inverse-Compton scattering) or protons (due to the pion decays) may be responsible for this emission. In particular, the broad-band spectra of SNRs may be explained in both leptonic and hadronic scenarios. Another kind of observational data, namely, images of SNRs, is an important part of experimental information. We present a method to model γ-ray images of Sedov SNRs in uniform media and magnetic field due to hadronic emission. These γ-rays are assumed to appear as a consequence of meson decays produced in inelastic collisions of accelerated protons with thermal protons downstream of the shock – a model would be relevant for SNRs without firm confirmations of the shock–cloud interaction, as e.g. SN 1006. Distribution of surface brightness of the shell-like SNR is synthesized numerically for a number of configurations. An approximate analytical formula for azimuthal and radial variation of hadronic γ-ray brightness close to the shock is derived. The properties of images as well as the main factors determining the surface brightness distribution are determined. Some conclusions that would be relevant to SN 1006 are discussed.

Keywords: acceleration of particles; radiation mechanisms: non-thermal; shock waves; ISM: supernova remnants

Journal Article.  5766 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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