Binary Stars Approaching Supermassive Black Holes: Tidal Breakup, Double Stellar Disruptions, and Stellar Collision

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In galactic centers, stars and binaries can be injected into low-angular-momentum orbits, resulting in close encounters with the central supermassive black hole (SMBH). Previous works have shown that under different conditions, such close encounters can lead to the breakup of the binary, disruptions of both stars, and collision between the stars. We use three-body scattering experiments to characterize these different outcomes for a range of system parameters, such as β b , the ratio of the binary tidal radius to the pericenter distance r p to the SMBH, and the compactness of the binary. We focus on stellar collisions, which occur for a range of β b s, with a few to tens of percent probabilities (depending on the compactness of the binary). In gentle encounters (β b ≲ 1), stellar collisions occur after the pericenter passage, and the merger remnants are typically ejected from the SMBH at a small velocity. In deep encounters (β b ≳ 1), collisions occur near the pericenter, with the impact velocity a few times the escape velocity of the star, and the merger remnants are typically bound to the SMBH. We suggest that stellar collisions induced by binary–SMBH encounters may produce exotic stars in galactic centers, trigger accretion flares onto the SMBH due to the mass loss, and result in bound merger remnants causing repeated partial tidal disruption events.