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We consider the formation of binary black hole mergers through the evolutionof field massive triple stars. In this scenario, favorable conditions for theinspiral of a black hole binary are initiated by its gravitational interactionwith a distant companion, rather than by a common-envelope phase invoked instandard binary evolution models. We use a code that follows self-consistentlythe evolution of massive triple stars, combining the secular triple dynamics(Lidov-Kozai cycles) with stellar evolution. After a black hole triple isformed, its dynamical evolution is computed using either the orbit-averagedequations of motion, or a high-precision direct integrator for triples withweaker hierarchies for which the secular perturbation theory breaks down. Mostblack hole mergers in our models are produced in the latter non-seculardynamical regime. We derive the properties of the merging binaries and computea black hole merger rate in the range (0.3- 1.3) Gpc^{-3}yr^{-1}, or up to~2.5Gpc^{-3}yr^{-1} if the black hole orbital planes have initially randomorientation. Finally, we show that black hole mergers from the triple channelhave significantly higher eccentricities than those formed through theevolution of massive binaries or in dense star clusters. Measuredeccentricities could therefore be used to uniquely identify binary mergersformed through the evolution of triple stars. While our results suggest up to~10 detections per year with Advanced-LIGO, the high eccentricities couldrender the merging binaries harder to detect with planned space basedinterferometers such as LISA.

Binary black hole mergers from field triples: properties, rates and the impact of stellar evolution