A two-component description of energetic particle scattering in a turbulent magnetoactive plasma

Details A two-component description of energetic particle scattering in a turbulent magnetoactive plasma A two-component description of energetic particle scattering in a turbulent magnetoactive plasma

May 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975jgr....80.1783m&link_type=abstract

Journal of Geophysical Research, vol. 80, May 1, 1975, p. 1783-1794.

Mathematics

7

Cosmic Rays, Interplanetary Medium, Magnetohydrodynamic Waves, Ecliptic, Mathematical Models, Momentum Transfer, Series (Mathematics), Solar Wind, Weighting Functions

Scientific paper

A method is developed for calculating the diffusion coefficient of energetic particles due to resonant interactions with an arbitrary distribution of Alfven waves. Resonant scattering is analyzed in terms of a simplified diffusion coefficient which allows a good quantitative measurement to be made of the pitch-angle and spatial diffusion coefficients for the general case of a wave vector distribution which is anisotropic and not necessarily field-aligned. The full wave vector distribution is represented as the sum of two weighted delta-function approximations, one parallel to the average magnetic field and the other parallel to the direction of the maximum wave vector density. This two-component model is used to calculate the pitch-angle and spatial diffusion coefficients of cosmic rays in the solar equatorial plane, and the results are compared with two other estimates where a radial diffusion is assumed. It is shown that the spatial coefficient in interplanetary space is considerably modified beyond approximately 1 AU when isotropic wave distribution is assumed.

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