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Wide black hole binaries (wide-BBHs; $\geqslant 10^3$ AU) in the field can beperturbed by random stellar flybys that excite their eccentricities. Once awide binary is driven to a sufficiently small pericenter approach,gravitational wave (GW) emission becomes significant, and the binary inspiralsand merges. In our previous study, using simplified models for wide-BBHs, wefound that successive flybys lead to significant merger fractions of wide-BBHsin less than Hubble time, making the flyby perturbation mechanism a relevantcontributor to the production rate of GW-sources. However, the exact rates anddetailed properties of the resulting GW sources depend on the wide binaryprogenitors. In this paper we use detailed population synthesis models for theinitial wide-BBH population, considering several populations corresponding todifferent natal-kick models and metallicities, and then follow the wide-BBHsevolution due to flyby perturbations and GW-emission. We show that thecumulative effect of flybys is conductive for the production of GW sources innon-negligible rates of $1-20$ Gpc$^{-3}$ yr$^{-1}$, which are sensitive to thenatal kicks model. Such rates are relevant to the observationally inferredrate. Our models, now derived from detailed population of binaries, provide thedetailed properties of the produced GW-sources, including mass-functions anddelay times. The GW mergers are circularized when enter the aLIGO band; have apreference for high velocity dispersion host galaxies (in particularellipticals); have a relatively uniform delay-time distribution; and likelyhave mildly correlated (less than isolated evolution channels and more thandynamical channels) prograde spin-spin and spin-orbits.

Detailed properties of gravitational-wave mergers from flyby perturbations of wide binary black holes in the field