The evolution status of contact close binaries of early spectral types

Details The evolution status of contact close binaries of early spectral types The evolution status of contact close binaries of early spectral types

Oct 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001kfnt...17..459e&link_type=abstract

Kinematika i Fizika Nebesnykh Tel, vol. 17, no. 5, p. 459-470

Physics

Scientific paper

Hertzsprung-Russel diagram is constructed for contact close binary stars of early spectral types (CE-systems) on the basis of the "Catalogue of approximate photometric and absolute elements of eclipsing variable stars" by Svechnikov M. A. and Kuznetsova E. F. The excess luminosity - mass, excess radius - mass, excess luminosity - mass ratio, and excess radius - mass ratio relations are obtained for these binary systems. All contact close binary stars of early spectral types are subdivided into 4 groups: 1) massive CE-systems of the pre-main sequence; 2) massive CE-systems of the post-main sequence; 3) low mass systems that have passed the "role exchange" phase (q<0.5); 4) low mass systems which have not passed the mass exchange phase (q≥0.5). Karetnikov's diagram is constructed for low-mass CE-systems with q<0.5, short-period detached main-sequence systems (DMS-systems) with P<2(d) and Sp1 from F2 to A5, and semi-detached systems of the R CMa type. The results prove that low-mass CE-systems with q<0.5 descended from short-period DMS-systems having passed the stage of semi-detached R CMa systems. The spatial density of stars in every CE-group is estimated taking into account the effect of observational selection. The low-mass stars which have experienced mass exchange are the most numerous among CE-systems.

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