Electromagnetic instabilities driven by unequal proton beams in the solar wind

Details Electromagnetic instabilities driven by unequal proton beams in the solar wind Electromagnetic instabilities driven by unequal proton beams in the solar wind

Jun 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976jgr....81.2743m&link_type=abstract

Journal of Geophysical Research, vol. 81, June 1, 1976, p. 2743-2749. ERDA-NASA-sponsored research.

Physics

22

Electromagnetic Properties, Magnetohydrodynamic Stability, Proton Beams, Solar Wind, Angular Distribution, Electron Energy, Electron Flux Density, Magnetohydrodynamic Waves, Propagation Modes, Wave Dispersion

Scientific paper

The paper sets forth a numerical investigation of the linear dispersion relation for typical solar wind conditions at 1 AU during those times (high-speed streams) when a secondary beam of protons drifting relative to the main proton component is present. Three beam-driven instabilities were found to occur as the beam drift velocity approaches the Alfven speed: (1) a pure, field-aligned magnetosonic wave that is most important at relatively high beta and/or high beam drift speeds; (2) an oblique magnetosonic wave having highest growth rates 15-30 deg from the magnetic field; and (3) an oblique Alfven wave having maximum growth rates at increasing angle to the magnetic field. The linear growth rates for the field-aligned magnetosonic and the Alfven oblique modes are investigated as a function of relative beam density, varying anisotropic pitch angle distributions for the various components, electron temperature, and electron heat flux.

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