Comparing Eclipse Observations of the August 1, 2008 Solar Corona with an MHD Model Prediction

Details Comparing Eclipse Observations of the August 1, 2008 Solar Corona with an MHD Model Prediction Comparing Eclipse Observations of the August 1, 2008 Solar Corona with an MHD Model Prediction

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh13b1524r&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH13B-1524

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1

2129 Interplanetary Dust, 2164 Solar Wind Plasma, 2169 Solar Wind Sources, 7509 Corona

Scientific paper

Total solar eclipses offer a unique opportunity to study the white light and emission coronae at high resolution. Newly developed image-processing techniques allow us to combine many individual coronal images with different exposures to produce coronal images during an eclipse that resemble those taken with radially graded filters, but with a higher quality. In a separate effort, 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 August 1, 2008 total solar eclipse. The eclipse was observed from Altaj village, Mongolia, under perfect seeing conditions. The white-light corona was observed with 6 telescopes, with a focal lenses ranging from 200 mm to 1250 mm. The emission corona at 530.3 nm (Fe XIV) was imaged thorough a narrow passband filter with a transmission width of 0.03 nm. To separate out the 530.3 nm corona, the scattered background was substracted from a white-light coronal image taken at 529.1 nm, taken simultaneously with another narrow passband filter with a transmission width of 0.03 nm. This was the first time that the green emission corona was observed during an eclipse. We will compare the observed images with features from the predicted MHD model, including magnetic field line traces and simulated polarization brightness images. Research partially supported by NASA and NSF.

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