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We model explosions driven by the coalescence of a black hole or neutron starwith the core of its massive-star companion. Upon entering a common envelopephase, a compact object may spiral all the way to the core. The concurrentrelease of energy is likely to be deposited into the surrounding commonenvelope, powering a merger-driven explosion. We use hydrodynamic models ofbinary coalescence to model the common envelope density distribution at thetime of coalescence. We find toroidal profiles of material, concentrated in thebinary's equatorial plane and extending to many times the massive star'soriginal radius. We use the spherically-averaged properties of thiscircumstellar material (CSM) to estimate the emergent light curves that resultfrom the interaction between the blast wave and the CSM. We find that typicalmerger-driven explosions are brightened by up to three magnitudes by CSMinteraction. From population synthesis models we discover that the brightestmerger-driven explosions, $M_V \sim -18$ to $-19$, are those involving blackholes because they have the most massive and extended CSM. Black holecoalescence events are also common; they represent about 50% of allmerger-driven explosions and approximately 0.3% of the core-collapse rate.Merger-driven explosions offer a window into the highly-uncertain physics ofcommon envelope interactions in binary systems by probing the properties ofsystems that merge rather than eject their envelopes.

astrophysical journal/the astrophysical journal

Explosions Driven by the Coalescence of a Compact Object with the Core  of a Massive-Star Companion Inside a Common Envelope: Circumstellar  Properties, Light Curves, and Population Statistics