The evolution of highly compact binary stellar systems

Details The evolution of highly compact binary stellar systems The evolution of highly compact binary stellar systems

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...254..616r&link_type=abstract

Astrophysical Journal, Part 1, vol. 254, Mar. 15, 1982, p. 616-640.

Astronomy and Astrophysics

Astrophysics

281

Binary Stars, Stellar Evolution, Stellar Mass Accretion, Stellar Systems, X Ray Sources, Angular Momentum, Companion Stars, Gravitational Waves, Mass Transfer, Neutron Stars, Opacity, Orbit Decay, Variable Stars, X Ray Binaries

Scientific paper

A new theoretical treatment of the evolution of highly compact binary systems is presented. The evolution is calculated until almost the entire mass of the secondary has been transferred to the primary or lost from the system. It is assumed that gravitational radiation from the system is the cause of mass transfer. It is found that the structure of the mass-losing star can be approximated by an n = 3/2 polytrope, and as a result a relatively large number of different cases can be explored and some general conclusions drawn. An explanation is found for the existence of a cutoff in the orbital period distribution among the cataclysmic variables and light is shed upon the possible generic relationships among cataclysmic variables, the low-mass X-ray binaries, and the spectrally soft transient X-ray sources.

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