Predicting the structure of the solar corona for the total solar eclipse of March 29, 2006

We describe the use of a three-dimensional MHD model to predict the structure of the corona prior to the total solar eclipse of March 29, 2006. The calculation uses the observed photospheric radial magnetic field as a boundary condition. We use a new version of our model that has an improved description of energy, transport in the corona. The model allows us to predict the emission of X-ray and EUV radiation in the corona. We compare the predicted polarization brightness 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 model with GOES/SXI images.