Radial Intensity Gradients and Diffusion Coefficients of Cosmic Rays in the Outer Heliosphere at Solar Maximum

Details Radial Intensity Gradients and Diffusion Coefficients of Cosmic Rays in the Outer Heliosphere at Solar Maximum Radial Intensity Gradients and Diffusion Coefficients of Cosmic Rays in the Outer Heliosphere at Solar Maximum

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....7.3831f&link_type=abstract

Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I

Physics

1

Scientific paper

The IMP-8, Voyager and Pioneer cosmic ray observations now cover the solar maximum of cycles 21, 22, and 23 and out to a heliocentric distance of 88 AU. In an accompanying paper we showed that the radial dependences of intensities J are different in the inner and outer heliosphere with a transition over the radial distance of 10 to 15 AU, and that those intensity gradients are well described as dJ/Jdr= G0 /r where r is heliocentric radial distance and G0 is constant with a different value in the inner and outer heliosphere. Using the obtained gradients and a simple one-dimensional modulation model we determined the diffusion coefficients as a function of radial distance and rigidity in the outer heliosphere at solar maximum. It is found that the diffusion coefficient, K, depends on radial distance r as r˜1.2 and on rigidity R as β R˜1.0 respectively in the outer heliosphere beyond 10 AU, where β is particle velocity over light velocity. K is determined on the assumption that K is a separable function of r and R.

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