Mean free paths of energetic particles at very large heliodistances (Pioneer 11 at 20 AU)

Details Mean free paths of energetic particles at very large heliodistances (Pioneer 11 at 20 AU) Mean free paths of energetic particles at very large heliodistances (Pioneer 11 at 20 AU)

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..140..161m&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 140, no. 1, July 1992, p. 161-170. Research supported by SERC.

Physics

11

Electromagnetic Interactions, Energetic Particles, Heliosphere, Interplanetary Magnetic Fields, Wave-Particle Interactions, Cosmic Rays, Diffusion Coefficient

Scientific paper

The parallel mean free path and the diffusion coefficient parallel to the magnetic field line are derived from magnetic field data at 20 AU to characterize heliospheric modulation and energetic-particle/magnetic-field interaction. The computational method of Moussas et al. (1975, 1982) is employed, and the values of the parallel mean free path are shown to be significantly larger than the values estimated in studies of up to 6 AU. The distance dependence of the parallel diffusion mean free path is found to follow a power law, and the diffusion coefficient dependence upon energy is determined by a constant mean free path and the velocity of the particle. The contribution of the diffusion coefficient perpendicular to the magnetic field is expected to dominate the radial diffusion coefficient of cosmic rays, although the contribution of the diffusion parallel to the field is important with respect to the small-scale structure of intensity gradients.

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