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We estimate the population of eccentric gravitational wave (GW) binary blackhole (BBH) mergers forming during binary-single interactions in globularclusters (GCs), using ~ 800 GC models that were evolved using the MOCCA codefor star cluster simulations as part of the MOCCA-Survey Database I project. Byre-simulating binary-single interactions (only involving 3 BHs) extracted fromthis set of GC models using an N-body code that includes GW emission at the 2.5post-Newtonian level, we find that ~ 10% of all the BBHs assembled in our GCmodels that merge at present time form during chaotic binary-singleinteractions, and that about half of this sample have an eccentricity > 0.1 at10 Hz. We explicitly show that this derived rate of eccentric mergers is ~ 100times higher than one would find with a purely Newtonian N-body code.Furthermore, we demonstrate that the eccentric fraction can be accuratelyestimated using a simple analytical formalism when the interacting BHs are ofsimilar mass; a result that serves as the first successful analyticaldescription of eccentric GW mergers forming during three-body interactions inrealistic GCs.

MOCCA-SURVEY Database I: Eccentric Black Hole Mergers During Binary-Single Interactions In Globular Clusters