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Magnetohydrodynamic modeling of coronal structure and expansionThe 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.
Document ID
19840005013
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Suess, S. T.
(National Oceanic and Atmospheric Administration Boulder, CO, United States)
Date Acquired
August 12, 2013
Publication Date
November 1, 1983
Publication Information
Publication: JPL Solar Wind Five
Subject Category
Solar Physics
Accession Number
84N13081
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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