On the spectroscopic orbit of the bright WC binary Gamma(2) Velorum, with implications for the evolutionary scenario of Wolf-Rayet stars

Details On the spectroscopic orbit of the bright WC binary Gamma(2) Velorum, with implications for the evolutionary scenario of Wolf-Rayet stars On the spectroscopic orbit of the bright WC binary Gamma(2) Velorum, with implications for the evolutionary scenario of Wolf-Rayet stars

Jun 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986aj.....91.1386m&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 91, June 1986, p. 1386-1391. Research supported by the Universidad Catolica de Chile

Other

45

Binary Stars, Orbital Elements, Stellar Evolution, Stellar Luminosity, Stellar Spectrophotometry, Wolf-Rayet Stars, O Stars, Photographic Plates, Radial Velocity, Stellar Mass Ejection, Stellar Orbits, Stellar Winds

Scientific paper

A series of over 50 spectroscopic plates distributed over three orbital cycles confirm the radial-velocity (RV) orbit for this 78.5 day, WC 8 + O9 I binary, as determined recently by Niemela and Sahade (1980). On the basis of RV perturbations, no evidience is found for a third, low-mass body in the system, as proposed elsewhere in the literature. Comparison with other WC + O binaries reveals a trend of mass ratio with spectral subclass, such that the cooler, late-type, WCL stars are more massive relative to their O companions than the hotter, early-type, WCE stars. Therefore, the finite lifetime of the WC phase combined with the observed high mass-loss rate for W-R stars implies that WCL stars may evolve into WCE stars. This scenario goes in the right sense if the peeling-off process of the wind exposes a progressively hotter core.

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