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Carbon and nitrogen lines in the spectra of Wolf-Rayet starsThe one-representative-point radiative transfer theory of Castor and van Blerkom (1970) is used to predict the relative energies in emission lines of the ions of carbon and nitrogen in Wolf-Rayet atmospheres for a wide range of parameters. The predicted ratios are compared with observed relative energies of lines in the visible and ultraviolet spectral ranges of six Wolf-Rayet stars. It is found that the lower levels of C II, C III, N III, and N IV are strongly overpopulated relative to their populations in LTE. The differences between WC and WN spectra appear to be due chiefly to a difference in electron temperature in the line-emitting regions. The typical volume of stars studied is estimated to be in the range of 10 to the 41st to 10 to the 44th cu cm. Possible ways in which the line-emitting regions may be arranged around the star are discussed, noting that the high-temperature line-emitting plasma may lie in a thin annular disk approximately 10 to the 15th cm from the star.
Document ID
19880054422
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Bhatia, A. K.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Underhill, A. B.
(British Columbia, University Vancouver, Canada)
Date Acquired
August 13, 2013
Publication Date
June 1, 1988
Publication Information
Publication: Astrophysical Journal Supplement Series
Volume: 67
ISSN: 0067-0049
Subject Category
Astrophysics
Accession Number
88A41649
Distribution Limits
Public
Copyright
Other

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