Mathematics
Scientific paper
Mar 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976izssr..40..634b&link_type=abstract
(Vsesoiuznaia Konferentsiia po Fizike Kosmicheskikh Luchei, Samarkand, Uzbek SSR, Oct. 29-31, 1975.) Akademiia Nauk SSSR, Izvest
Mathematics
Cosmic Rays, Forbush Decreases, Interplanetary Magnetic Fields, Magnetic Disturbances, Shock Fronts, Earth Magnetosphere, Mathematical Models, Solar Flares, Solar Wind
Scientific paper
Data on cosmic-ray intensity anisotropy are used to investigate the structure of strong interplanetary magnetic disturbances. The shape of the shock front associated with the chromospheric flare of Dec. 23, 1966, is deduced by comparing the observed longitudinal distribution of the intensity rise of cosmic rays generated by that flare with a theoretically calculated distribution. It is suggested that the main phase of a typical Forbush decrease occurs in three stages, with the first beginning after passage of the shock front, the second beginning when earth enters a 'magnetic region', and the third taking place in the relatively weak magnetic field of the central part of the flare plasma.
Belov Anatoly V.
Dorman Lev I.
Eroshenko Eugenia A.
Inozemtseva O. I.
Kaminer N. S.
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