Heliospheric Magnetic Field Configuration at Solar Maximum Conditions: Consequences for Galactic Cosmic Rays

Details Heliospheric Magnetic Field Configuration at Solar Maximum Conditions: Consequences for Galactic Cosmic Rays Heliospheric Magnetic Field Configuration at Solar Maximum Conditions: Consequences for Galactic Cosmic Rays

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..719...70z&link_type=abstract

PHYSICS OF THE OUTER HELIOSPHERE. AIP Conference Proceedings, Volume 719, pp. 70-80 (2004).

Physics

Particle Emission, Solar Wind, Interplanetary Magnetic Fields, Solar Wind Plasma, Sources Of Solar Wind

Scientific paper

During solar maximum conditions, the heliosphere is highly structured on all spatial scales. It is the purpose of this paper to summarize our current understanding of these structures from global scales to mesoscale, a fraction of 1 AU. We use theoretical considerations, in situ observations near Earth and the Ulysses spacecraft, and global heliosphere calculations to discuss the effects on both global and mesoscales on the three-dimensional structure of the heliospheric magnetic field and their effects on galactic cosmic rays. These conclusions are in contrast to near-solar-minimum-like heliospheric conditions that are currently assumed in modulation and transport calculations even during solar maximum. The expected complex heliospheric properties should be of major importance for the interpretation of the heliospheric boundary events observed by Voyager 1 since 2002. A companion paper by L. A. Fisk will explore the effects of the mesoscale structures on particle acceleration in the heliospheric boundary region.

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