Alfven wave refraction in high-speed solar wind streams

Details Alfven wave refraction in high-speed solar wind streams Alfven wave refraction in high-speed solar wind streams

Mar 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975jgr....80..908h&link_type=abstract

Journal of Geophysical Research, vol. 80, Mar. 1, 1975, p. 908-916.

Astronomy and Astrophysics

Astronomy

12

Astronomical Models, Magnetohydrodynamic Waves, Refracted Waves, Solar Wind Velocity, Amplitude Distribution Analysis, Gas Streams, Interplanetary Magnetic Fields, Plane Waves, Rarefied Plasmas, Velocity Distribution

Scientific paper

A high-speed solar wind stream model, in which the parameters vary with heliocentric distance, is used to determine the gross average features of Alfven wave propagation and refraction in the compression and rarefaction regions without regard to the detailed variation of the wave properties across those regions. The configurations of the magnetic field lines associated with the velocity maximum and the frontmost and rearmost edges of the stream are calculated. The results show that the wave amplitudes are larger in the compression region, the relative amplitudes are larger in the rarefaction region, and the waves are refracted in the direction of the magnetic field in the rarefaction region and away from it in the compression region. The last result is shown to agree with on site observations at 1 AU.

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