Compound and Perpendicular Diffusion of Solar Energetic Particles and Field Line Random Walk

Details Compound and Perpendicular Diffusion of Solar Energetic Particles and Field Line Random Walk Compound and Perpendicular Diffusion of Solar Energetic Particles and Field Line Random Walk

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh21c0435w&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH21C-0435

Physics

2118 Energetic Particles, Solar

Scientific paper

Simulations of energetic charged particle transport in random magnetic fields by Giacalone and Jokipii (1999), Mace et al. (2000) and Qin et al. (2002,2003) demonstrate that the quasilinear theory of diffusion of cosmic rays normal to the magnetic field is somewhat unsatisfactory. A more satisfactory theory for perpendicular diffusion, which better fits the simulations is the nonlinear guiding center theory of Matthaeus et al. (2003); Zank et al. (2004) and Shalchi et al. (2004), but this theory does not account for compound diffusion of particles perpendicular to the field observed in near slab turbulence. In this paper, we use a model for particle transport normal to the random walking mean magnetic field, based on a Chapman Kolmogorov equation, in which the particle is transported relative to the random walking field line. The model indicates that the particle can undergo both compound diffusion and ordinary diffusion perpendicular to the mean magnetic field. If the particle propagates in a ballistic fashion along the field at early times (as described by the telegrapher equation), then the particle diffuses perpendicular to the field at essentially the classical field line random walk (FLRW) value given by Jokipii (1966). We discuss the relation between this model, and the work of Chuvilgin and Ptuskin (1993) on perpendicular and compound diffusion.

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