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Detailed Reference Information
Guhathakurta et al. 1999
Guhathakurta, M., Sittler, E., Fisher, R., McComas, D. and Thompson, B. (1999). Coronal magnetic field topology and source of fast solar wind. Geophysical Research Letters 26: doi: 10.1029/1999GL010662. issn: 0094-8276.

We have developed a steady state, 2D semiempirical MHD model of the solar corona and the solar wind with many surprising results. This model for the first time shows, that the boundary between the fast and the slow solar wind as observed by Ulysses beyond 1 AU, is established in the low corona. The fastest wind observed by Ulysses (680--780 km/s) originates from the polar coronal holes at 70¿--90¿ latitude at the Sun. Rapidly diverging magnetic field geometry accounts for the fast wind reaching down to a latitude of ¿30¿ at the orbit of Earth. The gradual increase in the fast wind observed by Ulysses, with latitude, can be explained by an increasing field strength towards the poles, which causes Alfv¿n wave energy flux to increase towards the poles. Empirically, there is a direct relationship between this gradual increase in wind speed and the expansion factor, f, computed at r>20R. This relationship is inverse if f is computed very close to the Sun. ¿ 1999 American Geophysical Union

BACKGROUND DATA FILES

Abstract

Keywords
Solar Physics, Astrophysics, and Astronomy, Coronal holes, Solar Physics, Astrophysics, and Astronomy, Magnetic fields, Interplanetary Physics, Sources of the solar wind, Interplanetary Physics, Interplanetary magnetic fields
Journal
Geophysical Research Letters
http://www.agu.org/journals/gl/
Publisher
American Geophysical Union
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