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Stellar-remnant black holes (BH) in dense stellar clusters comprise a naturalsetup to trigger general-relativistic (GR) inspiral and merger of binary blackholes (BBH), detectable by the LISA and the LIGO-Virgo, through dynamicalencounters inside such environments. In this work, the intricacies of suchdynamical interactions are probed utilizing realistic, self-consistent,post-Newtonian, direct N-body evolutionary models of young massive and openstellar clusters. Particularly, the configurations of the compact subsystems,that drive the in-cluster GR BBH coalescences, are tracked on the fly. Such anapproach reveals that the GR coalescences within the open clusters take placeprimarily via chaotic interactions involving triple BH systems. Although lessfrequently, such mergers are found to happen also in higher-order subsystemssuch as quadruples and in subsystems involving non-BH members; the mergers canthemselves be BH---non-BH, which events would leave electromagnetic signatures.Close, fly-by encounters inside the clusters can also make BBHs and other typesof double-compact binaries temporarily post-Newtonian; such binaries wouldpotentially contribute to the GW background for the LISA and the PTA. Thesecalculations, furthermore, suggest that open clusters are potential hosts fornot only detached BH---main-sequence binaries, as recently identified in theglobular cluster NGC 3201, but also a wide variety of other types ofremnant---non-remnant binaries, which are assembled via dynamical interactionsinside the clusters and which have the prospects of being discovered inradial-velocity surveys.

monthly notices of the royal astronomical society

Stellar-mass black holes in young massive and open stellar clusters and  their role in gravitational-wave generation III: dissecting black hole  dynamics