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The tidal breakup of binary star systems by the supermassive black hole(SMBH) in the center of the galaxy has been suggested as the source of both theobserved sample of hypervelocity stars (HVSs) in the halo of the Galaxy and theS-stars that remain in tight orbits around Sgr A*. Here, we use apost-Newtonian N-body code to study the dynamics of main-sequence binaries onhighly elliptical bound orbits whose periapses lie close to the SMBH,determining the properties of ejected and bound stars as well as collisionproducts. Unlike previous studies, we follow binaries that remain bound forseveral revolutions around the SMBH, finding that in the case of relativelylarge periapses and highly inclined binaries the Kozai resonance can lead tolarge periodic oscillations in the internal binary eccentricity andinclination. Collisions and mergers of the binary elements are found toincrease significantly for multiple orbits around the SMBH, while HVSs areprimarily produced during a binary's first passage. This process can lead tostellar coalescence and eventually serve as an important source of young starsat the galactic center.

Tidal break-up of binary stars at the Galactic center and its consequences