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Binaries in Globular Clusters

Published online by Cambridge University Press:  14 August 2015

S. L. W. Mcmillan,
C. Pryor and
E. S. Phinney
S. L. W. Mcmillan
Affiliation:
Drexel University Department of Physics, Philadelphia, PA 19104, U.S.A.
C. Pryor
Affiliation:
Rutgers, the State University of New Jersey Dept. of Physics and Astronomy, 136 Frelinghuysen Rd., Piscataway, NJ 08854, U.S.A.
E. S. Phinney
Affiliation:
California Institute of Technology Theoretical Astrophysics, 130-33 Caltech, Pasadena, CA 91125, U.S.A.

Extract

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Binary stars in a globular cluster (hereafter, GC) may be primordial (i.e. formed along with the cluster), or the result of cluster dynamics. “Dynamical” binaries can result from conservative three-body encounters (e.g. Spitzer, 1987) if a third star can carry away enough kinetic energy to leave two others bound, or from dissipative two-body encounters, if two stars happen to pass within a few stellar radii of one other (Fabian, Pringle, & Rees, 1975). Such non-primordial systems are likely to be found primarily in evolved GC cores, both because conditions are more favorable for making them there, and because of mass segregation. Knowledge of the formation process allows reasonable estimates to be made of their mass and energy distributions. The initial spatial, mass, and energy distributions of primordial binaries, on the other hand, are largely unknown.

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