Coronal magnetic field topology and source of fast solar wind

Details Coronal magnetic field topology and source of fast solar wind Coronal magnetic field topology and source of fast solar wind

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999georl..26.2901g&link_type=abstract

Geophysical Research Letters, Volume 26, Issue 19, p. 2901-2904

Astronomy and Astrophysics

Astrophysics

7

Solar Physics, Astrophysics, And Astronomy: Coronal Holes, And Astronomy: Magnetic Fields, Interplanetary Physics: Sources Of The Solar Wind, Interplanetary Physics: Interplanetary Magnetic Fields

Scientific paper

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 Alfvén 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>20Rsolar. This relationship is inverse if f is computed very close to the Sun.

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