Magnetic field configurations associated with fast solar wind

Details Magnetic field configurations associated with fast solar wind Magnetic field configurations associated with fast solar wind

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..131..165s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 131, Jan. 1991, p. 165-186. Research supported by U.S. Navy.

Physics

21

Magnetic Field Configurations, Photosphere, Solar Corona, Solar Terrestrial Interactions, Solar Wind Velocity, Astronomical Models, Coronal Holes, Solar Magnetic Field, Sunspots, Ulysses Mission

Scientific paper

The implications are considered of the observed inverse correlation between solar wind speed at earth and the expansion rate of the sun-earth flux tube as it passes through the corona. It is found that the coronal expansion rate depends critically on the large-scale photospheric field distribution around the footpoint of the flux tube. The smallest expansions occur in tubes that are rooted near a local minimum in the field. This suggests that the fastest wind streams originate from regions where large coronal holes are about to break apart and from the facing edges of adjacent like-polarity holes, whose field lines converge as they transit the corona. Predictions are made which follow from the above ideas.

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