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Terminal velocities of the winds from rapidly rotating OB starsThis paper presents measurements of terminal velocities of OB stars which are rapid rotators, based on archival high-dispersion IUE spectra of the C IV resonance doublet. The terminal velocities of the most rapidly rotating stars appear to be systematically lower than those of the less rapidly rotating stars (at least for the cooler stars), although the number of very rapid rotators is only three. The modified line-radiation driven wind model of Friend and Abbott, which takes into account the finite size of the star as well as its rotation, predicts that the terminal velocity should drop with increasing rotational velocity. However, when a smaller but very homogeneous subset of the data is used (BO giants only), the correlation between terminal velocity and rotational velocity disappears.
Document ID
19900044377
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Friend, David B.
(Weber State College Ogden, UT, United States)
Date Acquired
August 14, 2013
Publication Date
April 20, 1990
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 353
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
90A31432
Funding Number(s)
CONTRACT_GRANT: NAG5-804
CONTRACT_GRANT: NAG5-1029
Distribution Limits
Public
Copyright
Other

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