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

Journal Article · Sun Jun 01 04:00:00 EDT 1986 · Astron. J.; (United States)

DOI:https://doi.org/10.1086/114115· OSTI ID:5266784

Moffat, A F.J.; Paquin, G; Lamontagne, R; Vogt, N; Barrera, L H

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. 24 references.

• Research Organization: Montreal Universite, Canada; Universidad Catolica de Chile, Santiago
• OSTI ID: 5266784
• Journal Information: Astron. J.; (United States), Journal Name: Astron. J.; (United States) Vol. 91; ISSN ANJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BINARY STARS
LUMINOSITY
MAIN SEQUENCE STARS
MASS TRANSFER
OPTICAL PROPERTIES
ORBITS
PHYSICAL PROPERTIES
RADIAL VELOCITY
STAR EVOLUTION
STARS
STELLAR ACTIVITY
STELLAR WINDS
VELOCITY
WOLF-RAYET STARS