Kinetics of Ions in the Solar Corona With Wave-Particle Interaction and Coulomb Collisions

Details Kinetics of Ions in the Solar Corona With Wave-Particle Interaction and Coulomb Collisions Kinetics of Ions in the Solar Corona With Wave-Particle Interaction and Coulomb Collisions

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh42b..04v&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH42B-04

Physics

2169 Sources Of The Solar Wind, 7511 Coronal Holes, 7827 Kinetic And Mhd Theory, 7843 Numerical Simulation Studies, 7867 Wave/Particle Interactions

Scientific paper

A kinetic model for the ions in the solar corona is presented. The model describes the wave-particle interaction within the framework of quasilinear theory and guarantees conservation of energy between waves and ions. The Coulomb collisions are evaluated using the Landau collision integral. Integration of the ion velocity distribution functions (VDFs) over the velocity components perpendicular to the background magnetic field introduces "reduced VDFs". Since the coupled Vlasov equations for these reduced VDFs depend only on the spatial coordinate, s, and speed component, v&|slash, parallel to the background magnetic field, they can be solved with reasonable numerical effort. Results for ions in a coronal funnel are presented. It is found that the heavy ions are heated preferredly and form strong temperature anisotropies, consistent with observations of the solar coronal plasma. The anisotropies increase with height, as the density and thus the efficiency of the Coulomb collisions decreases. The reduced VDFs develop pronounced deviations from a Maxwellian. Calculating the wave growth rate γ shows that the VDFs can reach the limit of marginal stability over a wide range of resonance speeds. The effects of the choice of the heavy ion species in the model plasma on the simulation results are also studied.

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