The Evolution of the Heliospheric Magnetic Field During the Solar Cycle

Details The Evolution of the Heliospheric Magnetic Field During the Solar Cycle The Evolution of the Heliospheric Magnetic Field During the Solar Cycle

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusm.a21b..04f&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #A21B-04

Physics

2134 Interplanetary Magnetic Fields, 2162 Solar Cycle Variations (7536)

Scientific paper

During previous solar cycles the heliospheric magnetic field, often referred to as the open magnetic flux of the Sun, appeared to evolve in a very simple manner. There was a single current sheet separating two regions of opposite polarity that appeared to rotate over during the solar cycle, accomplishing the field reversal. There was a background level of open magnetic flux that remains relatively constant, indicating little disconnection of open flux at the current sheet. Superimposed on this background level is the magnetic flux of CMEs, which is most evident at solar maximum. During the current solar minimum, the background level of open magnetic flux appears to have decreased relative to its level in previous minima. The implications of this observation for our understanding of the evolution of the heliospheric magnetic field and for the solar dynamo will be discussed.

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