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Cosmic ray-modified stellar winds. I - Solution topologies and singularitiesIn the present two-fluid hydrodynamical model for stellar wind flow modification due to its interaction with Galactic cosmic rays, these rays are coupled to the stellar wind by either hydromagnetic wave scattering or background flow irregularity propagation. The background flow is modified by the cosmic rays via their pressure gradient. The system of equations used possesses a line of singularities in (r, u, P sub c)-space, or a two-dimensional hypersurface of singularities in (r, u, P sub c, dP sub c/dr)-space, where r, u, and P sub c are respectively the radial distance from the star, the radial wind flow speed, and the cosmic ray pressure. The singular points may be nodes, foci, or saddle points.
Document ID
19880036370
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Ko, C. M.
(Arizona Univ. Tucson, AZ, United States)
Webb, G. M.
(Arizona, University Tucson, United States)
Date Acquired
August 13, 2013
Publication Date
December 15, 1987
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 323
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
88A23597
Funding Number(s)
CONTRACT_GRANT: NSF ATM-83-17701
CONTRACT_GRANT: NSG-7101
Distribution Limits
Public
Copyright
Other

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