Predicting the Structure of the Solar Corona During the 21 June 2001 Total Solar Eclipse

Details Predicting the Structure of the Solar Corona During the 21 June 2001 Total Solar Eclipse Predicting the Structure of the Solar Corona During the 21 June 2001 Total Solar Eclipse

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh41b24m&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH41B-24

Physics

2164 Solar Wind Plasma, 7509 Corona, 7524 Magnetic Fields

Scientific paper

We describe the application of a three-dimensional magnetohydrodynamic (MHD) model to the prediction of the structure of the corona during the total solar eclipse that is expected to occur on 21 June 2001. The calculation uses the observed photospheric radial magnetic field as a boundary condition. This model makes it possible to determine the large-scale structure of the magnetic field in the corona, as well as the distribution of the solar wind velocity, plasma density, and temperature. We will use magnetic fields observed on the solar disk prior to eclipse day to predict what the corona will look like during the eclipse. The estimated coronal density will be used to predict the plane-of-sky polarization brightness prior to the eclipse.

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