Computer Science
Scientific paper
Aug 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979ncimc...2..421i&link_type=abstract
Nuovo Cimento C, Serie 1, vol. 2C, July-Aug. 1979, p. 421-438. Research supported by the Consiglio Nazionale delle Ricerche.
Computer Science
43
Cosmic Rays, Galactic Radiation, Solar Activity Effects, Solar Wind Velocity, Coronal Holes, Equatorial Atmosphere, High Speed, Interplanetary Magnetic Fields, Proton Density (Concentration), Radio Emission, Solar Flares, Velocity Distribution
Scientific paper
Two classes of fast solar-wind streams are identified: (1) quiet streams, coming from near equatorial holes; stream interface 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; and (2) perturbed streams, coming from active regions producing type-IV solar flares, for which the previous requirements are not satisfied. Superposed epoch analyses applied on solar-wind speed and neutron monitor intensity show that during the high-speed 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. The perturbed streams are accompanied by Forbush decreases whose amplitude and time behavior are not directly related to the speed increase.
Iucci N.
Parisi Mario
Storini Marisa
Villoresi G.
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