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Recently several gravitational wave detections have shown evidence forcompact object mergers. However, the astrophysical origin of merging binariesis not well understood. Stellar binaries are typically at much largerseparations than what is needed for the binaries to merge due to gravitationalwave emission, which leads to the so-called final AU problem. In this letter wepropose a new channel for mergers of compact object binaries which solves thefinal AU problem. We examine the binary evolution following gas expansion dueto a weak failed supernova explosion, neutrino mass loss, core disturbance, orenvelope instability. In such situations the binary is possibly hardened byambient gas. We investigate the evolution of the binary system after a shockhas propagated by performing smoothed particle hydrodynamics simulations. Wefind that significant binary hardening occurs when the gas mass bound to thebinary exceeds that of the compact objects. This mechanism represents a newpossibility for the pathway to mergers for gravitational wave events.

Compact object mergers driven by gas fallback