Observations and analyses of the S VI lambda 1975, lambda 1993 A lines in the IUE ultraviolet spectra of WN stars

Details Observations and analyses of the S VI lambda 1975, lambda 1993 A lines in the IUE ultraviolet spectra of WN stars Observations and analyses of the S VI lambda 1975, lambda 1993 A lines in the IUE ultraviolet spectra of WN stars

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...292..616n&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 292, no. 2, p. 616-630

Astronomy and Astrophysics

Astronomy

3

Abundance, Electron Transitions, Helium, Line Spectra, Stellar Atmospheres, Stellar Models, Sulfur, Ultraviolet Astronomy, Ultraviolet Spectra, Wolf-Rayet Stars, Computer Programs, Distance, Interstellar Extinction, Iron, Iue, Oao 2, Oao 3, Stellar Winds, Ultraviolet Spectroscopy

Scientific paper

From a detailed study of high resolution IUE ultraviolet spectra we identify strong emission lines near approximately lambda 1990 A as the S VI (4p2P0 - 4d2D) transitions at lambda 1975.21 A, lambda 1992.56, 1993.24 A in HD 187282 (WN4), HD 50896 (WN5), HD 191765 (WN6) and HD 192163 (WN6). These S VI emissions may also be weakly present in HD 151932 (WN7). Additional S VI (4s2S - 4p2P0 lambda 2587, lambda 2618 emission features are also evident in the WNE spectra. Theoretical S VI line intensities are calculated using empirical non-local thermodynamic equilibrium (nLTE) model atmosphere codes adopting both spherically-symmetric, homogeneous and clumped wind structures. The observed S VI line strengths compared to the model predictions yield an estimated abundance ratio of S/He approximated = (2-3) x 10-4 by number. Within the observational and modeling uncertainties, this value is consistent with an initial near-solar abundance ratio, slightly modified by helium enhancement via CNO-burning, although a S-overabundance of x2-3 cannot be ruled out.

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