The origin and evolution of the WR binary V 444 Cygni

Details The origin and evolution of the WR binary V 444 Cygni The origin and evolution of the WR binary V 444 Cygni

Jul 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...200...79d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 200, no. 1-2, July 1988, p. 79-84.

Astronomy and Astrophysics

Astrophysics

8

Cygnus Constellation, Eclipsing Binary Stars, Stellar Evolution, Stellar Mass, Wolf-Rayet Stars, Mass Transfer, Stellar Luminosity, Stellar Mass Ejection, Stellar Winds

Scientific paper

The authors present an explicit model for the formation and the evolution of the well known Wolf-Rayet binary V444 Cygni. Performing a series of evolutionary computations for massive star undergoing case A and case B of mass transfer, including overshooting from convective cores, it is found that a massive binary system with initial masses of 24 and 16 M_sun; and an initial period of 1.91 days reproduces the observed system after case A and B of mass transfer. Since the primary WR star of V444 Cyg is a WN 5 star, the range of allowed initial primary masses is restricted to 20 M_sun; < M1i < 28 M_sun;. The authors cannot reproduce the high luminosity for the WR component claimed by Pauldrach et al. (1985), but they confirm the small value for the radius of the WR star found by Cherepaschuk et al. (1984).

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