Comparing an MHD Model of the Corona During the July 11, 2010 Total Solar Eclipse with Observations (Invited)

Details Comparing an MHD Model of the Corona During the July 11, 2010 Total Solar Eclipse with Observations (Invited) Comparing an MHD Model of the Corona During the July 11, 2010 Total Solar Eclipse with Observations (Invited)

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh42a..09m&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH42A-09

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields

Scientific paper

Total solar eclipses offer a unique opportunity to study the white light and emission coronae at high resolution. Magnetohydrodynamic (MHD) models have been used to predict the structure of the corona prior to eclipses, using measurements of photospheric magnetic fields on the Sun. In particular, such an MHD model was used to predict the structure of the corona for the July 11, 2010 total solar eclipse, using SOHO/MDI photospheric magnetic field data. We will compare observed images of the total solar eclipse with features from the MHD model, including magnetic field line traces and simulated polarization brightness images. We will also compare images of simulated emission in EUV and X-rays with observations from SOHO/EIT, Hinode/XRT, STEREO/EUVI, and SDO/AIA. Such comparisons of observed emission with predictions from global coronal MHD models provide a very sensitive constraint on coronal heating models. Research supported by NASA's Heliophysics Theory and Living With a Star Programs, and NSF/CISM.

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