Cosmic-ray gradients perpendicular to the ecliptic plane

Details Cosmic-ray gradients perpendicular to the ecliptic plane Cosmic-ray gradients perpendicular to the ecliptic plane

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985ge%26ae..25..184z&link_type=abstract

Geomagnetizm i Aeronomiia (ISSN 0016-7940), vol. 25, Mar.-Apr. 1985, p. 184-188. In Russian.

Computer Science

Cosmic Rays, Density Distribution, Interplanetary Space, Milky Way Galaxy, Radiation Distribution, Solar Cycles, Anisotropy, Magnetic Field Inversions, Solar Magnetic Field

Scientific paper

Anisotropy data are used to determine the solar-cycle-averaged symmetric and asymmetric components of the cosmic-ray-density gradient perpendicular to the ecliptic plane. The symmetric part of the gradient is found to vary only slightly with the solar cycle. The asymmetric part is equal to zero at the solar maximum (during the polarity reversal of the solar magnetic field), reaches its highest value at the solar minimum, and changes in sign after polarity reversal. Gradient values determined on the basis of numerical calculations from the equation for the distribution of galactic cosmic rays in interplanetary space agree well with experimental data.

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