A Kinetic Shell Description of the Ion Cyclotron Anisotropy Instability

Details A Kinetic Shell Description of the Ion Cyclotron Anisotropy Instability A Kinetic Shell Description of the Ion Cyclotron Anisotropy Instability

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..493i&link_type=abstract

SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 493-4

Computer Science

1

Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind

Scientific paper

We consider the simulation investigations of the electromagnetic ion cyclotron anisotropy instability which have been undertaken by Gary and co-workers, in particular their claim that an unstable bi-Maxwellian ion distribution will retain its bi-Maxwellian character when it reaches the asymptotic stable state. Quasilinear theory predicts that the time-asymptotic ion distribution will be given by a form of the kinetic shell distribution, with no density gradients along surfaces of constant energy in the wave frame. These constant energy surfaces are not ellipses, as would be required for contours of a bi-Maxwellian distribution. We derive an expression for this asymptotic distribution predicted by quasilinear theory. We then present an example, and compare it with a published simulation result by Gary et al. We find some aspects of our results in agreement with the simulation, but discrepancies appear at small υ∥. Further comparative studies could provide useful information on the applicability of quasilinear theory and/or hybrid simulations to wave-particle interactions in space plasmas.

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