The Evolution of Massive Stars — The Production of Binary WR Stars

  • C. de Loore
Part of the International Astronomical Union/Union Astronomique Internationale book series (IAUS, volume 99)


A large part of the stars of the galactic disk are binaries. Abt and Levy (1976,1978) estimate that more than 50% of B type stars are members of binary or multiple systems, and about 50% are close binaries. According to Conti et al. (1980) the total fraction of certain or probable binaries among 0 stars is about 36 percent. This means that during the evolution their components can fill their Roche volumes, and consequently have to lose mass in order to keep the star within the allowed surface. Several review papers dealing with the evolution of binaries were published recently: Paczynski (1971,1980), van den Heuvel (1976), de Loore (1980,1981), Webbink (1979).


Neutron Star Massive Star Mass Loss Rate Stellar Wind Roche Lobe 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


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Copyright information

© IAU 1982

Authors and Affiliations

  • C. de Loore
    • 1
  1. 1.Astrophysical InstituteVrije Universiteit BrusselBelgium

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