An MHD Model of the Solar Corona and Solar Wind

Details An MHD Model of the Solar Corona and Solar Wind An MHD Model of the Solar Corona and Solar Wind

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...188.3307m&link_type=abstract

American Astronomical Society, 188th AAS Meeting, #33.07; Bulletin of the American Astronomical Society, Vol. 28, p.868

Astronomy and Astrophysics

Astronomy

5

Scientific paper

The structure of the heliosphere, especially the regions of fast and slow solar wind, are strongly influenced by coronal magnetic structure near the Sun. Favorable comparisons between three-dimensional MHD models of the solar corona and eclipse observations have shown that it is possible to model the structure of the large-scale solar corona. However, these models use a simplified energy equation, in which the plasma is assumed to obey an adiabatic energy equation with a reduced polytropic index. As a consequence, even though the predicted streamer structure in the corona agrees fairly well with eclipse observations, the predicted solar wind speed is not realistic. We have improved this model by adding important dynamic and thermodynamic effects, including the presence of a transition region, thermal conduction, radiation, coronal heating, and Alfven wave acceleration. We will present results obtained with this improved model on the structure of the solar corona and solar wind.

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