Cosmic-ray propagation in strongly turbulent magnetized plasmas

Details Cosmic-ray propagation in strongly turbulent magnetized plasmas Cosmic-ray propagation in strongly turbulent magnetized plasmas

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..dpphm2005c&link_type=abstract

American Physical Society, 46th Annual Meeting of the Division of Plasma Physics, 15-19 November, 2004, Savannah, GA. MEETING I

Physics

Plasma Physics

Scientific paper

There exists a range of scales in many turbulent astrophysical plasmas that can usefully be described within the framework of magnetohydrodynamics (MHD). Strong MHD turbulence affects cosmic ray propagation in two distinct ways. First, magnetic fluctuations lead to pitch-angle scattering, which controls cosmic-ray diffusion along field lines. Second, MHD turbulence leads to field-line wandering, which in many cases controls cosmic ray diffusion perpendicular to any mean magnetic field in the system. This presentation will describe recent work on MHD turbulence, and its consequences for the phenomena described above.

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