Presentation #404.01 in the session Dynamics near supermassive Black Holes.
The central parsec of our Galaxy contains young stars orbiting Sgr A*, a supermassive black hole. These include the isotropic S star cluster of B stars within ~0.04 pc of Sgr A*, as well as a larger disc containing O and Wolf–Rayet stars. I will discuss how the disc can form from the tidal disruption of a molecular cloud. Subsequent dynamical evolution can produce a secular gravitational instability in the disc that will put some of its stars on nearly radial orbits. Sgr A* will tidally disrupt binaries on such orbits, producing S and hypervelocity stars.