Turbulent amplification of magnetic field and diffusive shock acceleration of cosmic rays
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In this paper, it was shown that the magnetic field can be amplified from its seed value by orders of magnitude and the consequences for the maximum attainable cosmic ray energy in supernova remnants are explored.Abstract:
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.read more
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References
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The acceleration of cosmic rays in shock fronts – I
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Principles of Plasma Physics
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Particle Acceleration by Astrophysical Shocks
TL;DR: In this article, a new mechanism is proposed for acceleration of a power-law distribution of cosmic rays with approximately the observed slope, where high-energy particles in the vicinity of a shock are scattered by Alfven waves carried by the converging fluid flow leading to a first-order acceleration process in which the escape time is automatically comparable to the acceleration time.
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An introduction to the theory of diffusive shock acceleration of energetic particles in tenuous plasmas
TL;DR: In this article, the central idea of diffusive shock acceleration is presented from microscopic and macroscopic viewpoints; applied to reactionless test particles in a steady plane shock, the mechanism is shown to produce a power law spectrum in momentum with a slope which, to lowest order in the ratio of plasma to particle speed, depends only on the compression in the shock.