High-speed solar wind streams and galactic cosmic ray modulation

Details High-speed solar wind streams and galactic cosmic ray modulation High-speed solar wind streams and galactic cosmic ray modulation

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979stin...8029226i&link_type=abstract

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Computer Science

Cosmic Rays, High Speed, Solar Wind, Coronal Holes, Forbush Decreases, Interplanetary Magnetic Fields, Neutron Counters, Solar Activity Effects, Solar Corona, Solar Flares

Scientific paper

Two classes of fast solar wind streams are identified: quiet streams, coming from near equatorial holes, the stream interface is in the initial phase followed by low proton density, quiet interplanetary magnetic field with constant polarity and proton temperature following the wind speed time profile; perturbed streams, coming from active regions producing type 4 solar flares, for which the previous requirements are not satisfied. Superposed epoch analyses applied to solar wind speed and neutron monitor intensity show that during the highspeed streams presumably coming from coronal holes the cosmic ray intensity is depressed; the time behavior of this depression follows the time profile of the wind speed to be determined. The perturbed streams are accompanied by Forbush decreases whose amplitude and time behavior are not directly related to the speed increase.

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