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Motion of the heliospheric termination shock - A gas dynamic modelA simple quantitative model is presented for the heliospheric termination shock's anticipated movement in response to upstream solar wind condition variations, under the assumption that the termination shock is initially a strong gasdynamic shock that is at rest relative to the sun, and that there is a discontinuous increase or decrease in the dynamical pressure upstream of the shock. The model suggests that the termination shock is constantly in motion, and that the mean position of the shock lies near the mean equilibrium position which corresponds to the balance between the mean solar wind dynamical pressure and the mean interstellar pressure.
Document ID
19940033498
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Barnes, Aaron
(NASA Ames Research Center Moffett Field, CA, United States)
Date Acquired
August 16, 2013
Publication Date
September 1, 1993
Publication Information
Publication: Journal of Geophysical Research
Volume: 98
Issue: A9
ISSN: 0148-0227
Subject Category
Astrophysics
Accession Number
94A10153
Distribution Limits
Public
Copyright
Other

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