Predicting the Structure of the Solar Corona for the Total Solar Eclipse of March 29, 2006

摘要

We describe the use of a three-dimensional MHD model to predictthe structure of the corona prior to the total solar eclipse of March 29, 2006. Thecalculation uses the observed photospheric radial magnetic field as a boundarycondition. We use a new version of our model that has an improved descriptionof energy transport in the corona. The model allows us to predict the emission ofX-ray and EUV radiation in the corona. We compare the predicted polarizationbrightness in the corona with four observations of the eclipse from Greece, Egypt,and Libya, and we demonstrate that the model accurately predicts the large-scale structure of the corona. We also compare X-ray emission from the modelwith GOES/SXI images.