Figure 17

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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 17: The effect of stellar wind mass-loss on the evolution of a runaway merger product during core hydrogen and core helium burning. The blue curve corresponds to the mass-loss used by Portegies Zwart et al. (2004) [385]. The black curve corresponds to the mass-loss used by Belkus et al. (2007) [49] with Z = 0.02 while the red line is for the same models but Z = 0.001 Image reproduced by permission from Vanbeveren et al. [468], copyright by Springer.