TALK ABSTRACT:
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I review numerical approaches to modeling the solar wind and associated 
Heliospheric magnetic fields.  Much of the space plasma environment can 
be modeled under the MHD assumption and this is the focus of the 
methods described in this talk, although extended MHD and kinetic 
effects will be mentioned.  The primary constraint on MHD methods is the 
Div B = 0 constraint and this leads to methods that differ considerably 
in approach.  Other capabilities such as the ability to deal with 
shocks, adaptive mesh refinement and the practical difficulties of 
large-scale simulation on parallel super-computers introduce additional 
challenges.  One very promising approach using staggered meshes in which 
we have made advances will be presented.