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Predicting the Structure of the Solar Corona for the Total Solar Eclipse of March 29,2006We describe the use of a three-dimensional MHD model to predict the s tructure of the corona prior to the total solar eclipse of March 29, 2006. The calculation uses the observed photospheric radial magnetic f ield as a boundary condition. We use a new version of our model that has an improved description of energy transport in the corona. The mo del allows us to predict the emission of X-ray and EUV radiation in t he corona. We compare the predicted polarization brightness in the co rona with four observations of the eclipse from Greece, Egypt, and Li bya, and we demonstrate that the model accurately predicts the largescale structure of the corona. We also compare X-ray emission from the model with GOES/SXI images.
Document ID
20070025413
Acquisition Source
Goddard Space Flight Center
Document Type
Reprint (Version printed in journal)
Authors
Mikic, Z.
(Science Applications International Corp. San Diego, CA, United States)
Linker, J. a.
(Science Applications International Corp. San Diego, CA, United States)
Lionello, R.
(Science Applications International Corp. San Diego, CA, United States)
Riley, P.
(Science Applications International Corp. San Diego, CA, United States)
TItov, V.
(Science Applications International Corp. San Diego, CA, United States)
Date Acquired
August 23, 2013
Publication Date
January 1, 2007
Publication Information
Publication: Solar and Stellar Physics Through Eclipses. ASP Conference Series
Volume: 370
Subject Category
Solar Physics
Funding Number(s)
CONTRACT_GRANT: NNG05EE09C
Distribution Limits
Public
Copyright
Other

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