Modelling the spectrum of WC-type Wolf-Rayet stars

Details Modelling the spectrum of WC-type Wolf-Rayet stars Modelling the spectrum of WC-type Wolf-Rayet stars

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...255..200h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 255, no. 1-2, p. 200-214.

Astronomy and Astrophysics

Astrophysics

53

Emission Spectra, Stellar Atmospheres, Stellar Spectra, Wolf-Rayet Stars, Carbon Stars, Electron Transitions, Helium, Ionization, Stellar Models

Scientific paper

Model calculations for carbon-rich Wolf-Rayet stars (WC) are presented which account for complex model atoms of helium and, especially, of carbon. The multilevel non-LTE radiation transfer in expanding atmospheres is simulated under the standard assumptions of spherical symmetry, homogeneity, and stationarity. A small set of models is presented, and the dependence of the resulting spectra on the basic stellar and atmospheric parameters is studied. The synthetic spectra are compared with the observed spectrum of WR111 (alias HD165763, subtype WC5), identifying the numerous lines and blends and discussing their significance for the purpose of spectral analyses. The models seem capable of reproducing the observation with reasonable accuracy. Thus we have prepared the tools for future quantitative analyses of WC spectra. The theoretical spectra are found to depend not on the stellar radius R* and the mass-loss rate M(dot) individually, but (in good approximation) only on the ratio R*/M(dot) exp 2/3. This 'transformation law' which is already known from pure-helium models is confirmed here for the carbon lines as well.

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