The effect of solar wind latitudinal dependence on the cosmic-ray propagation in the heliosphere

Details The effect of solar wind latitudinal dependence on the cosmic-ray propagation in the heliosphere The effect of solar wind latitudinal dependence on the cosmic-ray propagation in the heliosphere

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991ap%26ss.175..173g&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 175, no. 2, Jan. 1991, p. 173-189.

Astronomy and Astrophysics

Astrophysics

1

Heliosphere, Solar Cosmic Rays, Solar Wind, Energy Spectra, Interplanetary Magnetic Fields, Transport Theory, Two Dimensional Models, Voyager Project

Scientific paper

The influence of the latitude dependence of the solar wind velocity (SWV) on the cosmic-ray (CR) modulation and distribution in the heliosphere was investigated. The dependence proposed by Fry and Akasofu (1987) is used. An estimation of the diffusion and drift terms in the transport equation is made, which shows that, toward the poles, the effects of the drift transfer decrease, while the diffusion terms in the equation increase due to the change of the interplanetary magnetic field (IMF) geometry. The numerical solutions of the two-dimensional transport equation show that, when the SWV changes with latitude, the CR intensities away from the neutral sheet are larger for both IMF polarity periods in comparison with the case when the SWV does not change with the latitude and the latitude gradients are negative during negative magnetic polarity periods. The Voyager 1 and Voyager 2 long-time observations showing greater galactic CR intensities nearer the sun at greater distances, could be explained by the proposed model.

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