Gravitational radiation and the evolution of cataclysmic binaries

Details Gravitational radiation and the evolution of cataclysmic binaries Gravitational radiation and the evolution of cataclysmic binaries

Aug 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...248l..27p&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 248, Aug. 15, 1981, p. L27-L30.

Statistics

Computation

202

Binary Stars, Gravitational Waves, Stellar Evolution, Stellar Gravitation, Stellar Mass, Stellar Radiation, Variable Stars, Angular Momentum, Chemical Composition, Roche Limit, Stellar Mass Accretion, Stellar Mass Ejection, Stellar Models

Scientific paper

Model evolutionary computations were done for a low-mass secondary component filling its Roche lobe. Mass transfer from the secondary onto a primary component was driven by angular momentum loss caused by gravitational radiation. The secondary was initially a lower-main-sequence star, and it gradually became degenerate as a result of mass loss. The orbital period initially decreased to a minimum value close to 80 minutes and then increased. The observed hydrogen-rich cataclysmic binaries have a short-period cutoff at 81 minutes. This indicates that gravitational radiation is the main driving force for the evolution of such short-period systems.

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