The evolution of highly compact binary stellar systems in globular clusters

Details The evolution of highly compact binary stellar systems in globular clusters The evolution of highly compact binary stellar systems in globular clusters

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...282..466k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 282, July 15, 1984, p. 466-480. Research supported by the University of Cal

Astronomy and Astrophysics

Astrophysics

43

Binary Stars, Globular Clusters, Gravitational Collapse, Stellar Evolution, Stellar Mass Accretion, Stellar Systems, Dwarf Novae, Stellar Models, Stellar Motions, Three Body Problem, X Ray Sources

Scientific paper

The authors have calculated the secular evolution of a highly compact binary stellar system, composed of a collapsed object and a low-mass secondary star, in the core of a globular cluster. The binary evolves under the combined influences of (1) gravitational radiation losses from the system, (2) the evolution of the secondary star, (3) the resultant gradual mass transfer, if any, from the secondary to the collapsed object, and (4) occasional encounters with passing field stars. The times of encounters with field stars, and the initial parameters specifying those encounters, were chosen by use of a Monte Carlo technique; the subsequent gravitational interactions were calculated utilizing a three-body integrator. It is found that occasional close encounters with field stars strongly dominate the evolution of highly compact binaries in dense globular cluster cores. The authors display the distributions of fractional changes in semimajor axis and changes in eccentricity per encounter, and they discuss the frequency both of catastrophic encounters and of encounters which expel binaries from the cluster by superelastic recoil.

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