Figure 13

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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 13: Statistical properties of eccentric DWDs ( $e > 0.01$ ) in the LISA band ( $P < 5000 s$ ) for three different cluster models. Hatched histograms are for the entire eccentric DWD population while shaded histograms arefore the DWDs with at least two harmonics individually resolvable by LISA with an $S∕N > 8$ (5 year mission, 10 kpc distance). The PDFs are normalized to unity. From left to right: frequency, eccentricity, total mass, mass ratio and lifetime before merger. Plot reproduced by permission from Willems et al. 2007 [487], copyright by IOP.