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A&A 397, 777-788 (2003)
DOI: 10.1051/0004-6361:20021548
Cosmic ray transport in anisotropic magnetohydrodynamic turbulence
II. Shear Alfvèn waves
A. Teufel1, I. Lerche2 and R. Schlickeiser11 Institut für Theoretische Physik, Lehrstuhl IV: Weltraum- und Astrophysik, Ruhr-Universität Bochum, 44780 Bochum, Germany
e-mail: andreasm4@yahoo.com
2 Department of Geological Sciences, University of South Carolina, Columbia, SC 29208, USA
e-mail: black@geol.sc.edu
(Received 31 May 2002 / Accepted 23 October 2002 )
Abstract
Observations of interstellar turbulence imply that
the power spectrum of the wave turbulence must
be highly anisotropic. This anisotropy has to be included
when transport of high energy cosmic rays in
the Galaxy is discussed. Here we evaluate the relevant cosmic ray
transport parameters in the presence of anisotropic shear Alfvèn wave turbulence,
which have no contribution from the transit-time damping interaction and are
entirely due to gyroresonant interactions.
By averaging the respective Fokker-Planck coefficient over the particle
pitch-angle we calculate the momentum and spatial diffusion coefficients for
different anisotropy parameters.
For strongly perpendicular turbulence (
) we obtain that the momentum
diffusion coefficient is proportional to
, whereas for
strongly parallel turbulence (
) the momentum diffusion
coefficient is a constant.
We also calculate the anisotropy dependence of the spatial diffusion coefficient and
the mean free path for pure Alfvèn turbulence.
For all coefficients we discuss the rigidity dependence for
different cosmic ray particles and compare with earlier calculations of transport parameters
for slab-type Alfvèn turbulence.
Key words: magnetohydrodynamics (MHD) -- plasmas -- turbulence -- cosmic rays -- ISM: magnetic fields
Offprint request: A. Teufel, ate@tp4.ruhr-uni-bochum.de
© ESO 2003
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