Modeling the large-scale structure of the solar corona

Details Modeling the large-scale structure of the solar corona Modeling the large-scale structure of the solar corona

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991jgr....9617663b&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 96, Oct. 1, 1991, p. 17,663-17,674.

Physics

24

Coronagraphs, Solar Corona, Stellar Models, Solar Magnetic Field, Solar Rotation, Space Plasmas

Scientific paper

The aim of this study is to find a quantitative description of both the magnetic field and the distribution of plasma in the lower corona that matches the white light images of the K-corona. The magnetostatic model of Bogdan and Low (1986) and data obtained by the High Altitude Observatory Mark III K-Coronameter stationed at Mauna Loa, Hawaii is used. To start with, the simplest, solar minimum case when the corona is approximately longitudinally symmetric is taken. By varying parameters in the Bogdan and Low model it is possible to quantitatively match the general characteristics of the lower corona at solar minimum: power law radial profiles of coronal brightness; enhanced brightness at the equator; uniform density depletion at the pole.

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