Pitch angle scattering of solar particles - Comparison of 'particle' and 'field' approach. I - Strong scattering

Details Pitch angle scattering of solar particles - Comparison of 'particle' and 'field' approach. I - Strong scattering Pitch angle scattering of solar particles - Comparison of 'particle' and 'field' approach. I - Strong scattering

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988soph..117..135v&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 117, no. 1, 1988, p. 135-156. BMFT-supported research.

Physics

21

Angular Distribution, Energetic Particles, Particle Trajectories, Solar Magnetic Field, Diffusion Coefficient, Interplanetary Magnetic Fields, Power Spectra

Scientific paper

In the quasi-linear theory of pitch angle scattering the power spectrum of magnetic field fluctuations is related to the shape of the pitch angle diffusion coefficient D(μ), the absolute value of the mean free path λ, and the rigidity dependence of the mean free path λ(R). The authors discuss these relations in detail during the solar particle event of 11 April, 1978 which was observed on HELIOS-2 at a distance of 0.49 AU from the Sun. The values of D(μ) and λ based on the trajectory simulation for 100 MeV protons ("field" approach) are compared with results obtained from solar proton data ("particle" approach) and with predictions from quasi-linear theory based on the additional assumption of the slab model for magnetic field fluctuations ("QLT" approach). Results from the "field" and "particle" approaches agree surprisingly well.

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