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Coalescing black hole (BH) binaries forming in the dense core of globularclusters (GCs) are expected to be one the brightest sources of gravitationalwave (GW) radiation for the next generation of ground-based laserinterferometers. Favorable conditions for merger are initiated by the Kozairesonance in which the gravitational interaction with a third distant object,typically another BH, induces quasi-periodic variations of the inner BH binaryeccentricity. In this paper we perform high precision N-body simulations of thelong term evolution of hierarchical BH triples and investigate the conditionsthat lead to the merging of the BH binary and the way it might become anobservable source of GW radiation. We find that the secular orbit averagetreatment, adopted in previous works, does not reliably describe the dynamicsof these systems if the binary is orbited by the outer BH on a highly inclinedorbit at a moderate distance. During the high eccentricity phase of a Kozaicycle the torque due to the outer BH can drive the binary to extremely largeeccentricities in a fraction of the binary's orbital period. This occurs beforerelativistic terms become important to the evolution and allows the binary GWsignal to reach large GW frequencies (>~10 Hz) at high eccentricities. We showthat ~50 % of coalescing BH binaries driven by the Kozai mechanism in GCs willhave eccentricities larger than 0.1, with 10 % of them being extremelyeccentric, (1-e)<~10^-5, when they first chirp in the frequency band of groundbased laser interferometers. This implies that a large fraction of such GWsources could be missed if conventional quasi-circular templates are used foranalysis of GW detectors data. The efficient detection of all coalescing BHbinaries in GCs will therefore require template banks of eccentric inspiralwaveforms for matched-filtering and dedicated search strategies.

Black hole triple dynamics: breakdown of the orbit average approximation and implications for gravitational wave detections