Spatial Intensity Profiles of Galactic Cosmic Rays in the Heliosphere

Details Spatial Intensity Profiles of Galactic Cosmic Rays in the Heliosphere Spatial Intensity Profiles of Galactic Cosmic Rays in the Heliosphere

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..719..237m&link_type=abstract

PHYSICS OF THE OUTER HELIOSPHERE. AIP Conference Proceedings, Volume 719, pp. 237-242 (2004).

Physics

Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind, Planetary Bow Shocks, Interplanetary Shocks

Scientific paper

We study the spatial intensity profiles of galactic cosmic ray protons (H) and α-particles (He) during the solar minimum periods of 1987 (the so-called negative drift state) and 1977/1997 (both positive drift states) of the heliosphere. These intensities were measured with the Pioneer, Voyager and IMP spacecraft. The 1997 intensities were so low that one cannot readily explain them, even with the acceleration at the solar wind termination shock (SWTS) and modulation in the heliosheath included. Our heliospheric model is azimuthally symmetric with a spherical shock and heliopause, however, and we infer from its results that more realistic geometries may produce modulation effects that will explain the observations better.

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