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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
19920024986
Acquisition Source
Legacy CDMS
Document Type
Contractor Report (CR)
Authors
Rodrigues, Liliya L. (Washington Univ. Seattle, WA, United States)
Boehm-Vitense, Erika (Washington Univ. Seattle, WA, United States)
Date Acquired
September 6, 2013
Publication Date
January 1, 1990
Subject Category
Astronomy
Report/Patent Number
NAS 1.26:190854
NASA-CR-190854
Accession Number
92N34230
Funding Number(s)
CONTRACT_GRANT: NSG-5398
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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