Figure 15

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"Relativistic Binaries in Globular Clusters"

Matthew J. Benacquista and Jonathan M. B. Downing

	Abstract
1	Introduction
2	Globular Clusters
	2.1	Stellar populations in globular clusters
	2.2	The structure of globular clusters
	2.3	The dynamical evolution of globular clusters
3	Observations
	3.1	Cataclysmic variables
	3.2	Low-mass X-ray binaries
	3.3	Millisecond pulsars
	3.4	Black holes
	3.5	Extragalactic globular clusters
4	Relativistic Binaries
	4.1	Binary evolution
	4.2	Mass transfer
	4.3	Globular cluster processes
5	Dynamical Evolution
	5.1	Star cluster simulation methods
	5.2	Results from models of globular clusters
	5.3	Intermediate-mass black holes
6	Prospects of Gravitational Radiation
7	Summary
	Acknowledgements
	References
	Updates
	Figures
	Tables

Figure 15: Contours of constant number of X-ray binaries as a function of the “Verbunt parameters”. Here $Γ = ρ2r3c∕vc$ , $γ = ρ∕vc$ , $ρ$ is the average stellar density, $rc$ is the core radius and $vc$ the core velocity dispersion. $Γ$ describes the two-body stellar encounter rate and $γ$ describes the rate of encounters between a single binary with the stellar background. The squares represent the location of various Galactic globular clusters in the $γ − Γ$ plane and the number in parentheses is the number of X-ray binaries observed in the cluster. Plot reproduced by permission from Banerjee and Ghosh [30], copyright by IOP.