We compute emission of radiation from the corona by
integrating the emission kernels for extreme ultraviolet (EUV) and
X-ray radiation along a chosen line of sight. This intergation
requires knowledge of the plasma density and temperature in the corona,
which we predict using our model. The images below show the
predicted coronal emission at the time of the eclipse (02:35 UT on July
22, 2009). Click on
the images to see higher resolution versions.
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