Scattering of Cosmic Rays by Magnetohydrodynamic Interstellar Turbulence

Details Scattering of Cosmic Rays by Magnetohydrodynamic Interstellar Turbulence Scattering of Cosmic Rays by Magnetohydrodynamic Interstellar Turbulence

2002-05-17

arxiv.org/abs/astro-ph/0205285v2

Phys.Rev.Lett. 89 (2002) 281102

Astronomy and Astrophysics

Astrophysics

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

Scientific paper

10.1103/PhysRevLett.89.281102

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.

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