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The massive stars in the Galactic center inner arcsecond share analogousproperties with the so-called Hot Jupiters. Most of these young stars havehighly eccentric orbits, and were probably not formed in-situ. It has beenproposed that these stars acquired their current orbits from the tidaldisruption of compact massive binaries scattered toward the proximity of thecentral supermassive black hole. Assuming a binary star formed in a thingaseous disk beyond 0.1 pc from the central object, we investigate therelevance of disk-satellite interactions to harden the binding energy of thebinary, and to drive its inward migration. A massive, equal-mass binary star isfound to become more tightly wound as it migrates inwards toward the centralblack hole. The migration timescale is very similar to that of a single-starsatellite of the same mass. The binary's hardening is caused by the formationof spiral tails lagging the stars inside the binary's Hill radius. We show thatthe hardening timescale is mostly determined by the mass of gas inside thebinary's Hill radius, and that it is much shorter than the migration timescale.We discuss some implications of the binary's hardening process. When the moremassive (primary) components of close binaries eject most their mass throughsupernova explosion, their secondary stars may attain a range of eccentricitiesand inclinations. Such processes may provide an alternative unified scenariofor the origin of the kinematic properties of the central cluster and S-starsin the Galactic center as well as the high velocity stars in the Galactic halo.

Binaries migrating in a gaseous disk: Where are the Galactic center binaries?