An observation of a heliospheric magnetic cycle dependence for the integral radial gradient of E above 60 MeV cosmic rays

Details An observation of a heliospheric magnetic cycle dependence for the integral radial gradient of E above 60 MeV cosmic rays An observation of a heliospheric magnetic cycle dependence for the integral radial gradient of E above 60 MeV cosmic rays

Sep 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991jgr....9615899w&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 96, Sept. 1, 1991, p. 15,899-15,905. Research supported by University of

Physics

10

Galactic Cosmic Rays, Heliosphere, Radiation Distribution, Solar Cycles, Solar Magnetic Field, Radial Distribution, Radiation Transport, Solar Wind Velocity

Scientific paper

The dependence of the integral radial gradient of the cosmic radiation upon the cosmic ray intensity level and heliocentric radial distance is investigated. The magnitude of the integral radial gradient (IRG) from 1982-1990, during a period of negative polarity, is a strong function of the cosmic ray intensity changing from about 1.5 percent/AU at the time of the peak intensity in 1987 to about 3 percent/AU at times of minimum intensity in 1982 and 1990. In the early period studied from 1977 to 1982, during a period of positive polarity, practically no dependence of the magnitude of the IRG on the cosmic ray intensity was found. The gradient remained at about 3 percent/AU during the entire period. It is argued that these specific changes in the behavior of the gradient in opposite polarity cycles are not predicted by either the drift-wavy current sheet or simple diffusion-convection models of the solar modulation. The results are discussed in the context of the present understanding of the causes of the asymmetry in the 11-year modulation cycles.

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