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Binaries in Globular Clusters

McMillan, S. L. W. and Pryor, C. and Phinney, E. S. (1998) Binaries in Globular Clusters. In: Highlights of Astronomy. International Astronomical Union Symposium (IAUS). No.11B. Springer , Dordrecht, pp. 616-621. ISBN 978-0-7923-5556-4.

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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.

Item Type:Book Section
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Additional Information:© 1998 Springer Science+Business Media Dordrecht. SLWM's research has been supported by NASA grant NAGW-2559 and NSF grant AST 93-08005. CP's research on GCs is supported by NSF grant AST 96-19510. ESP's research has been supported by NASA grant NAG 5-2756 and NSF grant AST 96-18537.
Funding AgencyGrant Number
NSFAST 93-08005
NSFAST 96-19510
NASANAG 5-2756
NSFAST 96-18537
Subject Keywords:Black Hole; Neutron Star; Globular Cluster; Binary Star; Binary Frequency
Series Name:International Astronomical Union Symposium (IAUS)
Issue or Number:11B
Record Number:CaltechAUTHORS:20190605-152527586
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:96168
Deposited By: Tony Diaz
Deposited On:06 Jun 2019 03:11
Last Modified:16 Nov 2021 17:18

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