On the heliolatitudinal variation of the galactic cosmic-ray intensity. Comparison with Ulysses measurements

Details On the heliolatitudinal variation of the galactic cosmic-ray intensity. Comparison with Ulysses measurements On the heliolatitudinal variation of the galactic cosmic-ray intensity. Comparison with Ulysses measurements

Jun 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003angeo..21.1341e&link_type=abstract

Annales Geophysicae, vol. 21, Issue 6, pp.1341-1345

Physics

Scientific paper

We study the dependence of cosmic rays with heliolatitude using a simple method and compare the results with the actual data from Ulysses and IMP spacecraft. We reproduce the galactic cosmic-ray heliographic latitudinal intensity variations, applying a semi-empirical, 2-D diffusion-convection model for the cosmic-ray transport in the interplanetary space. This model is a modification of our previous 1-D model (Exarhos and Moussas, 2001) and includes not only the radial diffusion of the cosmic-ray particles but also the latitudinal diffusion. Dividing the interplanetary region into spherical magnetic sectors (a small heliolatitudinal extension of a spherical magnetized solar wind plasma shell) that travel into the interplanetary space at the solar wind velocity, we calculate the cosmic-ray intensity for different heliographic latitudes as a series of successive intensity drops that all these spherical magnetic sectors between the Sun and the heliospheric termination shock cause the unmodulated galactic cosmic-ray intensity. Our results are compared with the Ulysses cosmic-ray measurements obtained during the first pole-to-pole passage from mid-1994 to mid-1995.

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