Coronal Emission

    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 greatest eclipse (19:33 UT on July 11, 2010).  Click on the images to see higher resolution versions.

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EUV 171Å Emission (EIT)
Simulated EIT 171Å image
Simulated EIT 171 movie
Full-resolution QuickTime movie 800 kbytes)
Full-resolution GIF movie (19 Mbytes)
Half-resolution GIF movie (6 Mbytes)
EUV 195Å Emission (EIT)
Simulated EIT 195Å image
Simulated EIT 195 movie
Full-resolution QuickTime movie (600 kbytes)
Full-resolution GIF movie (17 Mbytes)
Half-resolution GIF movie (6 Mbytes)
EUV 284Å Emission (EIT)
Simulated EIT 284Å image
Simulated EIT 284 movie
Full-resolution QuickTime movie (700 kbytes)
Full-resolution GIF movie (17 Mbytes)
Half-resolution GIF movie (6 Mbytes)
X-Ray Emission (XRT Ti-poly Filter)
Simulated XRT Ti-poly image
Simulated XRT Ti-poly movie
Full-resolution QuickTime movie (400 kbytes)
Full-resolution GIF movie (15 Mbytes)
Half-resolution GIF movie (5 Mbytes)