Two-dimensional numerical modeling of the cosmic ray storm

Details Two-dimensional numerical modeling of the cosmic ray storm Two-dimensional numerical modeling of the cosmic ray storm

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986jgr....91...13k&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 91, Jan. 1, 1986, p. 13-29.

Astronomy and Astrophysics

Astronomy

31

Forbush Decreases, Galactic Cosmic Rays, Heliosphere, Interplanetary Medium, Solar Wind, Two Dimensional Models, Astronomical Models, Density Distribution, Solar Flares, Storms, Temporal Distribution

Scientific paper

A numerical model of a cosmic ray storm in the two-dimensional heliosphere is constructed incorporating the drift effect. The effects of a flare-associated interplanetary shock and the disturbed region behind it (characterized by enhancement in velocity and magnetic field, and decrease in mean free path) on the density and anisotropy of cosmic rays in the heliosphere are estimated. As the disturbance propagates outward, a density enhancement appears on the front side, and a density depression region is produced on the rear side. The effect of drift on the cosmic ray strom appears most clearly in the higher-latitude region. For the parallel (antiparallel) state of the solar magnetic field which corresponds to the pre(post-) 1980 period, the density in the higher-latitude region decreases (increases) before the shock arrival. The maximum density depression near the earth for the parallel state is greater than for the antiparallel state, and the energy spectrum of the density depression in percentage is softer for the parallel state than for the antiparallel state. Prior to the arrival of the shock, the phase of solar diurnal anisotropy begins to shift to the earlier hours, and its amplitude becomes greater for both polarity states. North-south anisotropy also becomes greater because of the enhanced drift for both polarity states.

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