Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 353, Issue 2, Pages 550-558Publisher
BLACKWELL PUBLISHING LTD
DOI: 10.1111/j.1365-2966.2004.08097.x
Keywords
acceleration of particles; magnetic fields; plasmas; shock waves; turbulence; cosmic rays
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The diffusive shock acceleration of cosmic rays by supernova remnants depends upon the generation of magnetic fluctuations by cosmic rays upstream of the shock. Strongly driven, non-resonant, nearly purely growing modes grow more rapidly than the resonant Alfven waves usually considered. Non-linear simulation shows that the magnetic field can be amplified from its seed value by orders of magnitude. The consequences for the maximum attainable cosmic ray energy in supernova remnants are explored.
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