Evidence for Nonradial Solar Wind Acceleration in Magnetostatic Coronal Holes

Details Evidence for Nonradial Solar Wind Acceleration in Magnetostatic Coronal Holes Evidence for Nonradial Solar Wind Acceleration in Magnetostatic Coronal Holes

Apr 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997eostr..78..258c&link_type=abstract

Eos Trans. AGU, 78(17), Spring Mtg. Suppl., 258

Astronomy and Astrophysics

Astrophysics

1

Solar Corona, Solar Wind

Scientific paper

We compare UVCS/SOHO observations of densities and outflow velocities in polar coronal holes with theoretical mass-conservation models of an idealized force-free magnetostatic geometry. Open flux tubes bordering the closed-field streamer belt initially expand much more rapidly than flux tubes over the poles, then turn nearly radial and expandless rapidly. In the past, this variation in the super radial expansion factor has been inversely correlated with solar wind velocity at 1 AU, but we find an even stronger inverse correlation in the acceleration region of the solar wind (1 to 10 solar radii). A considerable reduction in the wind speed of low-latitude flux tubes, compared with those over the poles, results in a geometry-dependent variation in the Doppler dimming of UV resonance lines such as H I Lyman alpha. Thus, we are able to use these emission diagnostics not only to infer the magnitude of the solar wind velocity, but also to map out the geometry of the solar wind emerging from large polar coronal holes. This work is supported by NASA under Grant NAG5-3192 to the Smithsonian Astrophysical Observatory, by the Italian Space Agency, and by Switzerland.

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