Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...358..240b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 358, July 20, 1990, p. 240-250. Research supported by NSERC.
Astronomy and Astrophysics
Astrophysics
4
Abundance, Emission Spectra, Radiative Transfer, Stellar Atmospheres, Stellar Spectra, Wolf-Rayet Stars, Atomic Energy Levels, Ground State, Oxygen Atoms, Oxygen Ions, Populations
Scientific paper
The 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.
Bhatia Anand K.
Underhill Anne. B.
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