Cosmic-ray anisotropy near the boundary of a high-speed solar-wind stream

Details Cosmic-ray anisotropy near the boundary of a high-speed solar-wind stream Cosmic-ray anisotropy near the boundary of a high-speed solar-wind stream

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981ge%26ae..21..424k&link_type=abstract

Geomagnetizm i Aeronomiia, vol. 21, May-June 1981, p. 424-427. In Russian.

Computer Science

8

Anisotropy, Cosmic Rays, Geomagnetism, Interplanetary Magnetic Fields, Solar Wind Velocity, Forbush Decreases, Lines Of Force, Neutron Scattering

Scientific paper

Experimental data obtained with neutron monitors at various stations are used to investigate the galactic-cosmic-ray anisotropy that was observed before and after the earth entered a high-speed solar-wind stream. The results show that a cosmic-ray anisotropy directed along the IMF lines of force toward the sun was observed in the region ahead of the high-speed stream where the IMF is compressed and that a Forbush decrease that may have also been anisotropic occurred within the high-speed stream. It is concluded that the magnetic field in a high-speed solar-wind stream is more regular than the field in the quiet solar wind and that, consequently, the cosmic-ray current along the IMF lines of force is amplified.

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