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Absorption-line profiles in a companion spectrum of a mass-losing cool supergiantCool star winds can best be observed in resonance absorption lines seen in the spectrum of a hot companion, due to the wind passing in front of the blue star. We calculated absorption line profiles that would be seen in the ultraviolet part of the blue companion spectrum. Line profiles are derived for different radial dependences of the cool star wind and for different orbital phases of the binary. Bowen and Wilson find theoretically that stellar pulsations drive mass loss. We therefore apply our calculations to the Cepheid binary S Muscae which has a B5V companion. We find an upper limit for the Cepheid mass loss of M less than or equal to 7 x 10 (exp -10) solar mass per year provided that the stellar wind of the companion does not influence the Cepheid wind at large distances.
Document ID
19930037501
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Rodrigues, Liliya L.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Boehm-Vitense, Erika
(Washington Univ. Seattle, United States)
Date Acquired
August 16, 2013
Publication Date
December 20, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 401
Issue: 2
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
93A21498
Funding Number(s)
CONTRACT_GRANT: NSG-5398
Distribution Limits
Public
Copyright
Other

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