The model and evolutionary status of the close binary system V 367 Cygni

Details The model and evolutionary status of the close binary system V 367 Cygni The model and evolutionary status of the close binary system V 367 Cygni

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990azh....67..653m&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 67, May-June 1990, p. 653-656. In Russian.

Astronomy and Astrophysics

Astronomy

4

Binary Stars, Stellar Evolution, Stellar Models, Abundance, Main Sequence Stars, Stellar Luminosity, Stellar Mass

Scientific paper

Observed parameters of the stellar components of V 367 Cygni have been compared with the theoretical ones for main sequence stars of the same mass, and considerable excesses in radii and luminosities of both components of the system were found. The whole set of observed characteristics of the bright, less massive component is well described by the existing theory of the evolution of close binary system of medium mass. It is also shown that the luminosity abundances of the secondary component cannot be explained within the framework of the disk accretion model.

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