Turbulent amplification of magnetic field and diffusive shock acceleration of cosmic rays

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ID: 298162
2004
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Ranked #199 of 900 articles by views in monthly notices of the royal astronomical society

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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 Alfvén 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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Authors A. R. Bell
Journal monthly notices of the royal astronomical society
Year 2004
DOI
10.1111/j.1365-2966.2004.08097.x
URL
https://academic.oup.com/mnras/article-pdf/353/2/550/3869038/353-2-550.pdf
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