Cosmic Ray Transport: Nonlinear Diffusion Parallel and Perpendicular to Magnetic Field

Details Cosmic Ray Transport: Nonlinear Diffusion Parallel and Perpendicular to Magnetic Field Cosmic Ray Transport: Nonlinear Diffusion Parallel and Perpendicular to Magnetic Field

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21113914y&link_type=abstract

American Astronomical Society, AAS Meeting #211, #139.14; Bulletin of the American Astronomical Society, Vol. 39, p.987

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We consider the propagation of cosmic rays in turbulent magnetic fields. We use the models of magnetohydrodynamic turbulence that were tested in numerical simulations, in which the turbulence is injected on large scale. To describe the interaction of cosmic rays with magnetic perturbations we develop a non-linear formalism that extends the ordinary Quasi-Linear Theory (QLT) that is routinely used for the purpose. This allows us to avoid the usual problem of 90 degree scattering and enable our computation of the mean free path of cosmic rays. We apply the formalism to the cosmic ray propagation in the galactic halo and in the Warm Ionized medium (WIM). In addition, we address the issue of the transport of cosmic rays perpendicular to the mean magnetic field and show that the issue of cosmic ray subdiffusion is only important for restricted cases when the ambient turbulence is far from what numerical simulations suggest to us. This work provides formalism that can be applied for calculating cosmic ray transport in a wide variety of circumstances. Various implications, including solar flare particle acceleration, are discussed.

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