Other
Scientific paper
Mar 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aj....103..960r&link_type=abstract
Astronomical Journal (ISSN 0004-6256), vol. 103, March 1992, p. 960-966.
Other
36
Binary Stars, Dwarf Stars, Stellar Color, Stellar Orbits, Stellar Temperature, Hertzsprung-Russell Diagram, Main Sequence Stars, Stellar Models
Scientific paper
The phenonemon of the short-period limit of the W UMa-type binaries is explained by the fact that at low surface temperatures stars become fully convective. It is shown that the more massive component has a relatively thicker convective envelope and that at low temperatures it becomes fully convective first. Because of the energy transfer to the secondary, the full-convection point of the primary component is shifted to somewhat larger masses than for single stars. The full-convection limit for solar-abundance, main-sequence systems is located at about 1.5, almost independently of the total mass or mass ratio of a system. This point is some distance from the colors of the currently known shortest-period systems. Although the Hayashi line is a definite limit on parameters of contact binaries, other factors produce the observed cutoff in the period distribution.
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