Detailed properties of gravitational-wave mergers from flyby
  perturbations of wide binary black holes in the field
  Wide black hole binaries (wide-BBHs; $\geqslant 10^3$ AU) in the field can be
perturbed by random stellar flybys that excite their eccentricities. Once a
wide binary is driven to a sufficiently small pericenter approach,
gravitational wave (GW) emission becomes significant, and the binary inspirals
and merges. In our previous study, using simplified models for wide-BBHs, we
found that successive flybys lead to significant merger fractions of wide-BBHs
in less than Hubble time, making the flyby perturbation mechanism a relevant
contributor to the production rate of GW-sources. However, the exact rates and
detailed properties of the resulting GW sources depend on the wide binary
progenitors. In this paper we use detailed population synthesis models for the
initial wide-BBH population, considering several populations corresponding to
different natal-kick models and metallicities, and then follow the wide-BBHs
evolution due to flyby perturbations and GW-emission. We show that the
cumulative effect of flybys is conductive for the production of GW sources in
non-negligible rates of $1-20$ Gpc$^{-3}$ yr$^{-1}$, which are sensitive to the
natal kicks model. Such rates are relevant to the observationally inferred
rate. Our models, now derived from detailed population of binaries, provide the
detailed properties of the produced GW-sources, including mass-functions and
delay times. The GW mergers are circularized when enter the aLIGO band; have a
preference for high velocity dispersion host galaxies (in particular
ellipticals); have a relatively uniform delay-time distribution; and likely
have mildly correlated (less than isolated evolution channels and more than
dynamical channels) prograde spin-spin and spin-orbits.
