Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 435, Issue 2, Pages 1174-1185Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stt1371
Keywords
acceleration of particles; instabilities; MHD; cosmic rays; ISM: supernova remnants
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Funding
- UK Science Technology and Facilities Council [ST/H001948/1]
- European Research Council under the European Community [247039]
- Science and Technology Facilities Council [ST/K00106X/1, ST/H001948/1] Funding Source: researchfish
- STFC [ST/H001948/1, ST/K00106X/1] Funding Source: UKRI
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We investigate the appearance of magnetic field amplification resulting from a cosmic ray escape current in the context of supernova remnant shock waves. The current is inversely proportional to the maximum energy of cosmic rays, and is a strong function of the shock velocity. Depending on the evolution of the shock wave, which is drastically different for different circumstellar environments, the maximum energy of cosmic rays as required to generate enough current to trigger the non-resonant hybrid instability that confines the cosmic rays follows a different evolution and reaches different values. We find that the best candidates to accelerate cosmic rays to similar to few PeV energies are young remnants in a dense environment, such as a red supergiant wind, as may be applicable to Cassiopeia A. We also find that for a typical background magnetic field strength of 5 mu G the instability is quenched in about 1000 years, making SN1006 just at the border of candidates for cosmic ray acceleration to high energies.
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