The development of low-mass eclipsing binary systems of main-sequence stars

Details The development of low-mass eclipsing binary systems of main-sequence stars The development of low-mass eclipsing binary systems of main-sequence stars

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990azh....67..885k&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 67, July-Aug. 1990, p. 885-887. In Russian.

Astronomy and Astrophysics

Astronomy

2

Eclipsing Binary Stars, Main Sequence Stars, Stellar Mass, Astronomical Catalogs, Roche Limit, Stellar Evolution

Scientific paper

Data from the Svechnikov (1969) catalog were used to obtain the characteristics and examine the development of eclipsing binary systems of main-sequence (MS) stars. It is shown that, during the evolution of low-mass stars (of M not above 1.5 solar masses) of eclipsing binary systems with loss of angular momentum due to the magnetic stellar wind, the time of the transition from an MS system to a quasi-KW system is approximately (0.9-2.0) x 10 to the 9th yrs, while the time for a regular KW system is greater by 3.5 x 10 to the 7th. The filling-up of the Roche lobes by stars of these systems is determined not by the evolutionary increase of solar radii but by the decrease of Roche lobe size, due to the decrease of the distance between the components of the binary.

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