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Heliospheric Magnetic Field Configuration and its Coronal Sources

Published online by Cambridge University Press:  13 May 2016

T. H. Zurbuchen
T. H. Zurbuchen*
Affiliation:
University of Michigan, Department of Atmospheric, Oceanic and Space Sciences, 2455 Hayward Street, Ann Arbor, MI 48109-2143, USA

Abstract

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The heliospheric magnetic field configuration is largely determined in the solar atmosphere. The interplanetary magnetic field is therefore intimately linked with the coronal structure and evolution during the solar cycle. We summarize recent experimental results from active satellite experiments on Ulysses and the Advanced Composition Explorer (ACE). These results provide constraints on the sources of the solar wind and also the magnetic structure of the heliosphere and the corona. These results suggest the relevance of reconnection processes and differential rotation effects close to the Sun. This leads to large perturbations from a standard Archimedean spiral configuration which cannot be successfully modeled using coronal models which assume a potential magnetic field.

Type
Session VII: Energetic Particles and the Local Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 203: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from Soho and Other Space Missions , 2001 , pp. 585 - 594
Copyright
Copyright © Astronomical Society of the Pacific 2001 

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