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.
Define a new variableA f,k to represent the amplitude of the oscillation modes: Af,k = √ 2ωf cf,k e−iωf Pk/2,(B6) whereP k =t k+1/2 −t k−1/2 is the period of thek-th inner orbit
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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.