Proton-driven electromagnetic instabilities in high-speed solar wind streams

Details Proton-driven electromagnetic instabilities in high-speed solar wind streams Proton-driven electromagnetic instabilities in high-speed solar wind streams

Feb 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979jgr....84..553a&link_type=abstract

Journal of Geophysical Research, vol. 84, Feb. 1, 1979, p. 553-559. Research sponsored by the U.S. Department of Energy and NAS

Physics

22

High Speed, Magnetohydrodynamic Stability, Magnetohydrodynamic Waves, Magnetosonic Resonance, Solar Protons, Solar Wind Velocity, Alpha Particles, Cyclotron Frequency, Electromagnetic Radiation, Electron Distribution, Maxwell-Boltzmann Density Function, Polarization (Waves), Solar Spectra, Velocity Distribution

Scientific paper

Electromagnetic instabilities of the field-aligned, right-hand circularly polarized magnetosonic wave and the left-hand circularly polarized Alfven wave driven by two drifted proton components are analyzed for model parameters determined from Imp 7 solar wind proton data measured during high-speed flow conditions. Growth rates calculated using bi-Lorentzian forms for the main and beam proton as well as core and halo electron velocity distributions do not differ significantly from those calculated using bi-Maxwellian forms. Using distribution parameters determined from 17 measured proton spectra, we show that considering the uncertainties the magnetosonic wave may be linearly stable and the Alfven wave is linearly unstable. Because proton velocity distribution function shapes are observed to persist for times long compared to the proton gyroperiod, the latter result suggests that linear stability theory fails for proton-driven ion cyclotron waves in the high-speed solar wind.

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