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Magnetohydrodynamic modeling of coronal structure and expansion (1983)

Suess, S. T.

In: CASI

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Publication Date: 2016-06-07

Description: 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.

Keywords: SOLAR PHYSICS

Type: JPL Solar Wind Five; p 183-198

Format: application/pdf

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