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A semiempirical model for the red supergiant's wind in Zeta Aurigae systemsA semiempirical model for the wind in four Zeta Aur binary systems is developed, basing the analyses on the velocity function, nonthermal velocities, and upper limits to Ne/N(H) inferred from observations of the winds from the cool supergiants. The model assumes that the energy fluxes needed to drive the wind are supplied by Alfven waves, since the acoustic wave flux estimated from line broadening is too low. The damping scale length of the waves, is found to change from very small values near the star to larger values of the order of the local radius further out in the wind. The temperature structure and hydrogen ionization are derived for these models. Limits to the stellar magnetic field are found, as well as a necessary constraint for the existence of cool massive winds, suggesting that the dividing line in the H-R diagram is where this constraint is violated.
Document ID
19890066490
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Kuin, N. P. M.
(NASA Goddard Space Flight Center; ST Systems Corp. Greenbelt, MD, United States)
Ahmad, I. A.
(Imad-ad-Dean, Inc. Bethesda, MD, United States)
Date Acquired
August 14, 2013
Publication Date
September 15, 1989
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 344
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
89A53861
Funding Number(s)
CONTRACT_GRANT: NAS5-28752
CONTRACT_GRANT: NAS5-29381
Distribution Limits
Public
Copyright
Other

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