  Over the last 15 years, around a hundred very young stars have been observed
in the central parsec of our Galaxy. While the presence of young stars forming
one or two stellar disks at approx. 0.1 pc from the supermassive black hole
(SMBH) can be understood through star formation in accretion disks, the origin
of the S stars observed a factor of 10 closer to the SMBH has remained a major
puzzle. Here we show the S stars to be a natural consequence of dynamical
interaction of two stellar disks at larger radii. Due to precession and Kozai
interaction, individual stars achieve extremely high eccentricities at random
orientation. Stellar binaries on such eccentric orbits are disrupted due to
close passages near the SMBH, leaving behind a single S star on a much tighter
orbit. The remaining star may be ejected from the vicinity of the SMBH, thus
simultaneously providing an explanation for the observed hypervelocity stars in
the Milky Way halo.
