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Several scenarios were suggested for the origins of gravitational-wave (GW)sources from mergers of stellar binary black holes (BBHs). Here we propose anovel origin through catalyzed formation of GW-sources from ultra-wide binariesin the field. Such binaries experience perturbations from random stellarfly-bys which excite their eccentricities. Once a wide-binary is driven to asufficiently small peri-center approach, GW-emission becomes significant, andthe binary inspirals and merges. We derive an analytic model and verify it withnumerical calculation to compute the merger rate to be $\sim10{\rm \timesf_{wide}\,{\rm Gpc}^{-3}yr^{-1}}$ ($f_{{\rm wide}}$ is the fraction of wideBH-binaries), which is comparable to the observationally inferred rate. Theobservational signatures from this channel include spin-orbit misalignment;preference for high mass-ratio BBH; preference for high velocity-dispersionhost-galaxies; and a uniform delay-time distribution.

Gravitational-wave sources from mergers of binary black-holes catalyzed by fly-bys interactions in the field