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The solar wind flow along the subsolar line in the magnetic barrier and reconnection at the magnetopauseThe 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.
Document ID
19950028703
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Erkaev, N. V.
(Russian Academy of Sciences Krasnoyarsk, Russia)
Mezentsev, A. V.
(Russian Academy of Sciences Krasnoyarsk, Russia)
Biernat, H. K.
(Austrian Academy of Sciences Graz, Austria)
Besser, B. P.
(Austrian Academy of Sciences Graz, Austria)
Bachmaier, G. A.
(Austrian Academy of Sciences Graz, Austria)
Semenov, V. S.
(State Univ. St. Petersburg, St. Petergof, Russia)
Rijnbeek, R. P.
(Univ. of St. Andrews Scotland, UK, United States)
Farrugia, C. J.
(NASA Goddard Space Flight Center Greenbelt, MD, US, United States)
Date Acquired
August 16, 2013
Publication Date
July 1, 1994
Publication Information
Publication: Advances in Space Research
Volume: 14
Issue: 7
ISSN: 0273-1177
Subject Category
Geophysics
Accession Number
95A60302
Funding Number(s)
CONTRACT_GRANT: NAS5-30442
CONTRACT_GRANT: P8046-GEO
Distribution Limits
Public
Copyright
Other

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