Magnetohydrodynamic modeling of coronal structure and expansion

Details Magnetohydrodynamic modeling of coronal structure and expansion Magnetohydrodynamic modeling of coronal structure and expansion

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983nascp.2280.183s&link_type=abstract

In JPL Solar Wind Five p 183-198 (SEE N84-13067 03-92)

Physics

Flow Geometry, Magnetohydrodynamic Flow, Mathematical Models, Solar Corona, Boundary Value Problems, Magnetic Fields, Polytropic Processes, Radial Distribution, Transonic Flow

Scientific paper

The presence of a magnetic field in the corona adds structure to the solar wind and almost certainly plays an important role in the energetics of the flow. Analytical and numerical modeling of gas-magnetic field interactions as used to compute steady, global flow are discussed. The approach used in, and results from a recent global model (Steinolfson, Suess and Wu, 1982) are discussed. Ideas on the most effective ways to improve the physical content and numerical efficiency of these models are outlined. Solutions of the MHD equations are discussed only in order to find steady-state flows, even though this often entails solving time-dependent equations.

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