Physics
Scientific paper
Jan 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....81..161p&link_type=abstract
Astronomy and Astrophysics, vol. 81, no. 1-2, Jan. 1980, p. 161-166.
Physics
18
Coronal Holes, Mathematical Models, Solar Corona, Solar Magnetic Field, Solar Physics, Solar Flux Density, Solar Temperature, Solar Wind Velocity
Scientific paper
Theoretical modeling of the solar wind expansion in magnetic field geometries considering the polar coronal hole modeled by Munro and Jackson (1977) is discussed, as is the physical temperature and density structure resulting from such expansion. A model based on the potential field approximation is computed, and the solar wind is examined through integration of the solar wind equations along individual field lines. In particular, the temperature, density and magnetic field strength necessary at the base of the hole to reproduce the observed density structure in the 2-4 solar radii region are determined. The influence of coronal heating on the solar wind is also investigated by introducing a crude exponentially damped heating function similar to that of Kopp and Orral (1976) into the solar wind equations. Although higher temperatures are produced in the inner corona, there was little effect on the temperature at 1 AU, and the solar wind velocity is actually decreased by heating in the inner corona.
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