Modelling the Large Scale Structure of the Solar Corona

Details Modelling the Large Scale Structure of the Solar Corona Modelling the Large Scale Structure of the Solar Corona

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.1207g&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #12.07; Bulletin of the American Astronomical Society, Vol. 24, p.748

Astronomy and Astrophysics

Astronomy

Scientific paper

We report on recent attempts 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. We use the magnetostatic model of Bogdan and Low and data obtained by the High Altitude Observatory K-Coronameter (1.2 - 2.3 Rsun) and the Solar Maximum Mission Coronameter/Polarimeter (1.5 - 4 Rsun). By varying parameters in the Bogdan and Low model we are able 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. Further, we use the best fit model to determine a temperature distribution in the corona and investigate the implications this has for solar wind theory.

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