Enhanced scintillations associated with high speed streams in the solar winds

Details Enhanced scintillations associated with high speed streams in the solar winds Enhanced scintillations associated with high speed streams in the solar winds

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982jgr....87.1688b&link_type=abstract

Journal of Geophysical Research, vol. 87, Mar. 1, 1982, p. 1688-1690.

Physics

2

Scintillation, Solar Wind Velocity, Stellar Radiation, Magnetohydrodynamic Waves, Plasma Dynamics, Proton Density (Concentration)

Scientific paper

The long wavelength (lambda greater than the ion-gyro radius) density homogeneities in the solar wind that raise the stellar radio scintillation index during the onset of a high-velocity stream, may be generated by a low-frequency compressional electromagnetic mode such as the magnetosonic (MS) wave. The present investigation shows that obliquely propagating MS waves are driven unstable by the double-peaked proton distributions observed in the solar wind. This is proposed as a reason for the correlation of high speed streams with enhanced scintillation. The stability at 1 AU of the observed nonequilibrium, double-peaked particle distributions emerges as a natural consequence of the suggested mechanism.

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