Abstract
A short review is given, first, of an extension of classical, continuum gasdynamics to solar system magnetohy-drodynamics (MHD) in both the steady and time-dependent contexts. A slightly longer review is given of two-and three-dimenslonal, numerical, MHD simulations of transient, solar-generated disturbances in the inner solar system. Validation of this approach is provided by making use of several examples wherein shock shapes and energetic particle fluxes (generated by shocks) are empirically confirmed. Although these studies are based on an ideal, one-fluid (proton) plasma, we suggest that a three-dimensional MHD model be employed to make use of presently available solar observations as approximate physical parameters for initialization conditions. Such a model may be useful, within the space weather national implementation plan, for geomagnetic storm forecasts.
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