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We study the orbital evolution of black hole (BH) binaries in quadruple systems, where the tertiary binary excites large eccentricity in the BH binary through Lidov–Kozai (LK) oscillations, causing the binary BHs to merge via gravitational radiation. For typical BH binaries with masses |m₁, ₂ 20\!-\!30\, M_| and initial semimajor axis a0 ∼ 100 au (such that the binaries have no chance of merging by themselves within ∼1010 yr), we show that binary–binary interactions can significantly increase the LK window for mergers (the range of companion inclinations that allows the BH binary to merge within 10 Gyr). This increase arises from a secular resonance between the LK oscillation of the BH binary and the nodal precession of the outer (binary–binary) orbit driven by the tertiary binary. Therefore, in the presence of tertiary binary, the BH merger fraction is increased to |10\!-\!30{\ per\ cent}|, an order of magnitude larger than the merger fraction found in similar triple systems. Our analysis (with appropriate scalings) can be easily adapted to other configurations of systems, such as relatively compact BH binaries and moderately hierarchical triples, which may generate even higher merger fractions. Since the occurrence rate of stellar quadruples in the galactic fields is not much smaller than that of stellar triples, our result suggests that dynamically induced BH mergers in quadruple systems may be an important channel of producing BH mergers observed by LIGO/VIRGO.
Liu et al. (Mon,) studied this question.