Influence of non-bi-Maxwellian distribution function of solar wind protons on the ion cyclotron instability

Details Influence of non-bi-Maxwellian distribution function of solar wind protons on the ion cyclotron instability Influence of non-bi-Maxwellian distribution function of solar wind protons on the ion cyclotron instability

Aug 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978jgr....83.3900l&link_type=abstract

Journal of Geophysical Research, vol. 83, Aug. 1, 1978, p. 3900-3902. Oesterreichischer Ford zur Foerderung der wissenschaftlic

Physics

3

Distribution Functions, Ion Cyclotron Radiation, Solar Protons, Solar Wind, Anisotropic Media, Maxwell-Boltzmann Density Function, Velocity Distribution

Scientific paper

The study is concerned with the field-aligned case, an ion cyclotron wave in a non-Maxwellian one-ion component solar wind plasma with isotropic electron background. A modified axisymmetric distribution function for solar wind protons is used to calculate the stability and growth rate of the ion cyclotron instability in a warm slow speed solar plasma at 1 AU. The calculations were performed because satellite measurements of the thermal anisotropy of solar wind protons have shown that the particle velocity distributions at 1 AU are not adequately described by a bi-Maxwellian distribution function. The calculations show that a solar wind proton velocity distribution slightly different from a bi-Maxwellian distribution causes the ion cyclotron wave to be unstable for observed temperature anisotropies, that is, when the ion temperature parallel to the magnetic field is larger than the ion temperature perpendicular to the magnetic field.

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