The eclipsing Wolf-Rayet binary V444 Cygni - Modelling the light curve and the helium spectrum consistently

Details The eclipsing Wolf-Rayet binary V444 Cygni - Modelling the light curve and the helium spectrum consistently The eclipsing Wolf-Rayet binary V444 Cygni - Modelling the light curve and the helium spectrum consistently

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...261..523h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 261, no. 2, p. 523-534.

Astronomy and Astrophysics

Astrophysics

30

Eclipsing Binary Stars, Helium, Light Curve, O Stars, Stellar Spectra, Wolf-Rayet Stars, Local Thermodynamic Equilibrium, Spectral Line Width, Stellar Atmospheres, Stellar Evolution, Stellar Models

Scientific paper

The eclipse light curve of the WR+O binary V444 Cygni (HD 193576, WR139) is modelled, describing the WR atmosphere by means of elaborate multilevel non-LTE calculations. It is demonstrated that the observed light curve can be reproduced by a manifold of parameter combinations. A unique solution is obtained from a simultaneous fit to the observed helium lines in the composite spectrum. The consistent reproduction of both the spectrum and the light curve is considered as a general confirmation of the applied model. The effective temperature of the WR component is derived as 35 kK. For the luminosities we obtain 10 exp 4.7 and 10 exp 4.3 solar luminosities for the WR star and the O star, respectively, but we discuss the possibility that these values might be underestimated by about 0.5 dex. The evolutionary status of the system can be explained by homogeneous evolution of the WR component, or alternatively by close-binary evolution with Roche-lobe overflow.

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