The heliospheric magnetic field at solar maximum

Details The heliospheric magnetic field at solar maximum The heliospheric magnetic field at solar maximum

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh52b..01z&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH52B-01

Physics

2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma

Scientific paper

The heliospheric magnetic field configuration close to solar maximum reflects the development of the underlying solar magnetic field. During the entire time of the heliospheric polarity change, the magnetic field of the Sun can be considered having two distinct components: open magnetic flux that constitutes the majority of the heliospheric magnetic field, and closed magnetic flux which remains attached to the Sun. In a paper in 2001, Fisk and Schwadron demonstrated how the evolution of the open heliospheric magnetic field can be described using a diffusive transport mechanism that depends on the closed magnetic field configuration. We use this model to calculate the average heliospheric magnetic field configuration during solar maximum. The heliospheric magnetic field lines show large, non-random deviations from the average Parker field configuration. We discuss this large-scale geometry, and make predictions for particle propagation in the heliosphere during solar maximum.

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