Scattering of Cosmic Rays by Magnetohydrodynamic Interstellar Turbulence

Abstract

Recent advances in understanding of magnetohydrodynamic (MHD) turbulence call for substantial revisions in our understanding of cosmic ray transport. In this paper we use gyroresonance recently obtained scaling laws for MHD modes to calculate the scattering frequency for cosmic rays in the ISM. We consider gyroresonance with MHD modes (Alfvenic, slow and fast) and transit-time damping (TTD) by fast modes. We conclude that the gyroresonance with fast modes is the dominant contribution to cosmic ray scattering for the typical interstellar conditions. In contrast to earlier studies, we find that Alfvenic and slow modes are inefficient because they are far from isotropy usually assumed.

4 pages, 2 figures, Phys. Rev. Lett. in press, minor changes

References in corpus (4)

• Simulations of MHD Turbulence in a Strongly Magnetized Medium
• Compressible MHD Turbulence in Interstellar Plasmas
• Galactic and extragalactic magnetic fields
• Velocity and density spectra of the Small Magellanic Cloud

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