Up to 50% of wide binaries in the empty loss-cone regime around massive black holes harden into close binaries via repeated MBH perturbations and chaotic stellar tides rather than undergoing Hills breakup.
Here we consider the tidal damping from inertial waves, with the correspondingQ ′ (Barker 2020): Q′ =Q ′ IW ≈10 7 Prot 10 d 2 ,(E2) whereP rot is the rotation period of the star
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Formation of Close Binaries through Massive Black Hole Perturbations and Chaotic Tides
Up to 50% of wide binaries in the empty loss-cone regime around massive black holes harden into close binaries via repeated MBH perturbations and chaotic stellar tides rather than undergoing Hills breakup.