Open AccessTurbulent amplification of magnetic field and diffusive shock acceleration of cosmic rays
Author(s) -
Bell A. R.
Publication year - 2004
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2004.08097.x
Subject(s) - physics , cosmic ray , supernova , astrophysics , magnetic field , acceleration , shock wave , shock (circulatory) , shock waves in astrophysics , particle acceleration , turbulence , computational physics , astronomy , classical mechanics , mechanics , quantum mechanics , medicine
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.