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Many astrophysical environments, from star clusters and globular clusters tothe disks of Active Galactic Nuclei, are characterized by frequent interactionsbetween stars and the compact objects that they leave behind. Here, using asuite of $3-D$ hydrodynamics simulations, we explore the outcome of closeinteractions between $1M_{\odot}$ stars and binary black holes (BBHs) in thegravitational wave regime, resulting in a tidal disruption event (TDE) or apure scattering, focusing on the accretion rates, the back reaction on the BHbinary orbital parameters and the increase in the binary BH effective spin. Wefind that TDEs can make a significant impact on the binary orbit, which isoften different from that of pure scattering. Binaries experiencing a prograde(retrograde) TDE tend to be widened (hardened) by up to $\simeq 20\%$.Initially circular binaries become more eccentric by $\lesssim 10\%$ by aprograde or retrograde TDE, whereas the eccentricity of initially eccentricbinaries increases (decreases) by a retrograde (prograde) TDE by $\lesssim5\%$. Overall a single TDE can generally result in changes of the gravitationalwave-driven merger time scale by order unity. The accretion rates of both blackholes are very highly super-Eddington, showing modulations (preferentially forretrograde TDEs) on a time scale of the orbital period, which can be acharacteristic feature of BBH-driven TDEs. Prograde TDEs result in theeffective spin parameter $\chi$ to vary by $\lesssim 0.02$ while $\chi\gtrsim-0.005$ for retrograde TDEs.

Close Encounters of Stars with Stellar-mass Black Hole Binaries