Spatial distribution of cosmic rays in magnetic cycles of the Sun

Details Spatial distribution of cosmic rays in magnetic cycles of the Sun Spatial distribution of cosmic rays in magnetic cycles of the Sun

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....4..485a&link_type=abstract

In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 4 p 485-488 (SEE N85-34729 23-92)

Other

Charged Particles, Diffusion Coefficient, Galactic Cosmic Rays, Models, Modulation, Scattering, Solar Cycles, Solar Magnetic Field, Spatial Distribution, Anisotropy, Cosmic Ray Showers, Neutron Counters

Scientific paper

The space-time distribution of cosmic ray (CR) density is determined from the solution of the anisotropic diffusion equation. The boundary problem is solved in a quasistationary axisymmetric case, taking into account the delay of cosmic rays relative to the cyclic variations of solar activity. The specificty of the modulation model is the use of the empirical dependence of the free path of particles for scattering on the observed latitudinal distribution of solar activity. Another specific feature of the model is an account of an additional effect due to the drift of charged particles towards the helio-equator plane or backward, depending on the direction of the total magnetic field of the Sun.

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