Evolution of low-mass close binary sytems with a compact mass accreting component

Details Evolution of low-mass close binary sytems with a compact mass accreting component Evolution of low-mass close binary sytems with a compact mass accreting component

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...191...57p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 191, no. 1, Feb. 1988, p. 57-70.

Mathematics

119

Binary Stars, Pulsars, Stellar Mass Accretion, Supernovae, X Ray Binaries, Angular Momentum, Branching (Mathematics), Hertzsprung-Russell Diagram, Stellar Mass Ejection

Scientific paper

Numerical calculations are presented that simulate the evolution of low-mass close binary systems in which a star of mass equal to 1.0 to 2.0 solar masses transfers mass to a compact object. It is shown that the mass transfer starts when the lobe-filling star is at a stage betwen the Zero Age Main Sequence and the ascent of the giant branch. Adopting the estimate of Verbunt and Zwaan (1981) for the efficiency of magnetic braking, the bifurcation periods which separate the converging binary sytems from the diverging binary systems, leading to wide detached binaries with a white dwarf remnant of the donor star, are determined. The possible initial system parameters and current evolutionary state of PSR 1831-00, A 0620-00, 4U 1626-67, G 16-29, 4U 1916-05, Sco X-1, Cen X-4, and GK Per are discussed.

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