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Cosmic ray transport in non-resonant current driven MHD turbulence

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Reville,  Brian
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Kirk,  John G.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Reville, B., O'Sullivan, S., Duffy, P., & Kirk, J. G. (2007). Cosmic ray transport in non-resonant current driven MHD turbulence. Talk presented at Seventh European Workshop on Collisionless Shocks. Paris, France. 2007-11-07 - 2007-11-09.


Cite as: https://hdl.handle.net/11858/00-001M-0000-0011-7BB2-4
Abstract
Both resonant and non-resonant instabilities are responsible for the self-generation of hydromagnetic waves in the precursor of collisionless shock waves. These waves facilitate the scattering of relativistic particles necessary for the diffusive acceleration of cosmic rays. We perform high-resolution magnetohydrodynamic simulations of the non-resonant cosmic-ray driven instability, in which the unstable waves are excited beyond the linear regime, and calculate the transport properties of test-particles in a snapshot of the resultant field. It is shown that even for modest field amplification that sub-Bohm diffusion can be achieved for a range of energies. This provides the first explicit demonstration that self-excited turbulence reduces the diffusion coefficient and has important implications for cosmic ray transport and acceleration in supernova remnants.