Secular Evolution Of Binaries Near Massive Black Holes: Formation of
  compact binaries, merger/collision products and G2-like objects
  Here we discuss the evolution of binaries around MBH in nuclear stellar
clusters. We focus on their secular evolution due to the perturbation by the
MBH, while simplistically accounting for their collisional evolution. Binaries
with highly inclined orbits in respect to their orbit around the MBH are
strongly affected by secular processes, which periodically change their
eccentricities and inclinations (e.g. Kozai--Lidov cycles). During periapsis
approach, dissipative processes such as tidal friction may become highly
efficient, and may lead to shrinkage of a binary orbit and even to its merger.
Binaries in this environment can therefore significantly change their orbital
evolution due to the MBH third-body perturbative effects. Such orbital
evolution may impinge on their later stellar evolution. Here we follow the
secular dynamics of such binaries and its coupling to tidal evolution, as well
as the stellar evolution of such binaries on longer time-scales. We find that
stellar binaries in the central parts of NSCs are highly likely to evolve into
eccentric and/or short period binaries, and become strongly interacting
binaries either on the main sequence (at which point they may even merge), or
through their later binary stellar evolution. The central parts of NSCs
therefore catalyze the formation and evolution of strongly interacting
binaries, and lead to the enhanced formation of blue stragglers, X-ray
binaries, gravitational wave sources and possible supernova progenitors.
Induced mergers/collisions may also lead to the formation of G2-like cloud-like
objects such as the one recently observed in the Galactic center.
