We have developed a three-dimensional steady-state MHD model of the solar corona and solar wind. The model covers the region from the coronal base to 100 AU and accounts for the effects of pickup protons in the distant heliosphere. To attain these ends, the two-region model of Usmanov and Goldstein (2003) was modified to include a region Ⅲ that extends from 1-100 AU and incorporates a population of interstellar pickup protons and its interaction with the solar wind protons. We compute the global structure of the solar wind from the coronal base out to 100 AU and compare our results with Voyager 2 observations.
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