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Tidal stellar disruptions have traditionally been discussed as a probe of thesingle, massive black holes (MBHs) that are dormant in the nuclei of galaxies.In Chen et al. (2009), we used numerical scattering experiments to show thatthree-body interactions between bound stars in a stellar cusp and anon-evolving "hard" MBH binary will also produce a burst of tidal disruptions,caused by a combination of the secular "Kozai effect" and by close resonantencounters with the secondary hole. Here we derive basic analytical scalings ofthe stellar disruption rates with the system parameters, assess the relativeimportance of the Kozai and resonant encounter mechanisms as a function oftime, discuss the impact of general relativistic (GR) and extended stellar cuspeffects, and develop a hybrid model to self-consistently follow the shrinkingof an MBH binary in a stellar background, including slingshot ejections andtidal disruptions. In the case of a fiducial binary with primary hole massM_1=10^7\msun and mass ratio q=M_2/M_1=1/81, embedded in an isothermal cusp, wederive a stellar disruption rate \dot{N_*} ~ 0.2/yr lasting ~ 3X10^5 yr. Thisrate is 3 orders of magnitude larger than the corresponding value for a singleMBH fed by two-body relaxation, confirming our previous findings. For q<<0.01,the Kozai/chaotic effect could be quenched due to GR/cusp effects by an orderof magnitude, but even in this case the stellar-disruption rate is still twoorders of magnitude larger than that given by standard relaxation processesaround a single MBH. Our results suggest that >~10% of the tidal-disruptionevents may originate in MBH binaries.

Tidal stellar disruptions by massive black hole pairs: II. Decaying binaries