A Magnetohydrodynamic Test of the Wang-Sheeley Model

Details A Magnetohydrodynamic Test of the Wang-Sheeley Model A Magnetohydrodynamic Test of the Wang-Sheeley Model

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.5714l&link_type=abstract

American Astronomical Society, 200th AAS Meeting, #57.14; Bulletin of the American Astronomical Society, Vol. 34, p.739

Astronomy and Astrophysics

Astronomy

Scientific paper

The Wang-Sheeley empirical model enables the calculation of the solar wind speed at Earth from the divergence of magnetic flux tubes in a synoptic map-based potential field source surface model of the coronal magnetic field. The formula used for this purpose was derived from observations of the solar wind speed at 1 AU. According to the model, fast solar wind emanates from regions of small magnetic field divergence, while slow solar wind comes from high divergence regions. Arge and Pizzo (2000) recently improved the Wang-Sheeley formula by taking the stream interaction effects between the Sun and 1 AU into account. We use a three-dimensional MHD model of the solar corona to test the assumptions of the Wang- Sheeley model and the improvements made by Arge and Pizzo for various magnetic configurations. These results provide insight into what additional coronal heating may be implied for different flux tube geometries in order to obtain the observed relationship with solar wind speed.

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