Quasi-linear perpendicular diffusion coefficients of charged cosmic rays calculated directly from the Newton-Lorentz equation

Details Quasi-linear perpendicular diffusion coefficients of charged cosmic rays calculated directly from the Newton-Lorentz equation Quasi-linear perpendicular diffusion coefficients of charged cosmic rays calculated directly from the Newton-Lorentz equation

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009mnras.394.2089d&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 394, Issue 4, pp. 2089-2097.

Astronomy and Astrophysics

Astronomy

4

Diffusion, Turbulence, Cosmic Rays

Scientific paper

It is the subject of this article to determine diffusion coefficients of charged test particles perpendicular to a mean magnetic field analytically by starting directly from the Newton-Lorentz equation. We employ the so-called standard quasi-linear theory to test the well-known field line random walk limit. It is demonstrated in this article that there is an additional gyroresonant contribution which describes the scattering of the particle away from a single field line. For certain situations, this additional contribution is small and can be neglected. For other cases, we obtain new results such as a rigidity-dependent quasi-linear perpendicular mean free path. The results of this article are relevant for particles in the solar wind which move scatter free or nearly scatter free in the direction parallel to the magnetic field of the Sun.

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