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Momentum and energy transport by waves in the solar atmosphere and solar windThe fluid equations for the solar wind are presented in a form which includes the momentum and energy flux of waves in a general and consistent way. The concept of conservation of wave action is introduced and is used to derive expressions for the wave energy density as a function of heliocentric distance. The explicit form of the terms due to waves in both the momentum and energy equations are given for radially propagating acoustic, Alfven, and fast mode waves. The effect of waves as a source of momentum is explored by examining the critical points of the momentum equation for isothermal spherically symmetric flow. We find that the principal effect of waves on the solutions is to bring the critical point closer to the sun's surface and to increase the Mach number at the critical point. When a simple model of dissipation is included for acoustic waves, in some cases there are multiple critical points.
Document ID
19770059500
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Jacques, S. A.
(Colorado, University Boulder, Colo., United States)
Date Acquired
August 9, 2013
Publication Date
August 1, 1977
Publication Information
Publication: Astrophysical Journal
Subject Category
Solar Physics
Accession Number
77A42352
Funding Number(s)
CONTRACT_GRANT: NAS8-31378
Distribution Limits
Public
Copyright
Other

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