AbstractThe magnetic barrier is a significant fraction of the magnetosheath region where magnetic forces react back on the plasma flow. We use a magnetohydrodynamic approach to calculate the solar wind flow around the magnetosphere. The use of so-called frozen-in coordinates, where the flow lines and the magnetic field are coordinate axes, is found to be most appropriate. Numerical solutions are presented for the problem of the flow around a blunt body. The results near the magnetopause are used as input parameters for a model of the reconnection of magnetic field lines based on shock-type structures.
The solar wind flow along the subsolar line in the magnetic barrier and reconnection at the magnetopause
Advances in Space Research ; 14 , 7 ; 81-86
1994-01-01
6 pages
Article (Journal)
Electronic Resource
English
British Library Conference Proceedings | 1994
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