Ion-acoustic-like instabilities in the solar wind

Details Ion-acoustic-like instabilities in the solar wind Ion-acoustic-like instabilities in the solar wind

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978jgr....83.2504g&link_type=abstract

Journal of Geophysical Research, vol. 83, June 1, 1978, p. 2504-2510. Research sponsored by the U.S. Department of Energy.

Physics

19

Acoustic Instability, Distribution Functions, Solar Physics, Solar Wind, Drift Rate, Heat Flux, Ion Beams, Maxwell-Boltzmann Density Function, Phase Velocity, Solar Corona, Whistlers

Scientific paper

The linear dispersion properties of k parallel to B electrostatic instabilities driven by an electron heat flux or an ion beam are studied by use of parameters appropriate to average values in the solar wind near 1 AU. These modes are also compared with field-aligned electromagnetic instabilities driven by the same sources of free energy. The ion acoustic heat flux instability has a high threshold relative to the whistler heat flux instability, so the latter mode is the more likely cause of the heat flux limitation near 1 AU. However, at sufficiently large Te/T sub t the electrostatic ion beam instability threshold is of the same order as that of the magnetosonic ion beam instability, implying that the former is the more likely source of ion-acoustic-like fluctuations observed near 1 AU.

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