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The oxygen emission lines in Wolf-Rayet spectraThe statistical equilibrium of oxygen in the line-emitting regions of WR stars is studied using the one-representative point theory of Castor and van Blerkom (1970) for a wider range of the radiation temperature, electron temperature, and electron density. Radiative processes, collisional processes, and electronic recombination are studied for a 59-level model atom. The level populations depart by large factors from those expected for LTE at the electron temperature and electron density. When the parameters have the values found previously by Bhatia and Underhill to be representative for WR stars, the oxygen atoms are strongly concentrated in the lower levels of O(2+), O(3+), and O(4+). The predicted relative energies in typical lines of O III, O IV, and O V for a solar abundance ratio of O to H are compatible with what is observed in WC and WN spectra.
Document ID
19900054793
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, Anne B.
(British Columbia, University Vancouver, Canada)
Date Acquired
August 14, 2013
Publication Date
July 20, 1990
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 358
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
90A41848
Distribution Limits
Public
Copyright
Other

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