  Hypervelocity stars (HVSs) that are observed in the Galactic halo, are
believed to be accelerated to large velocities by a process of tidal disruption
of binary stars passing close to a supermassive black hole (SMBH) which resides
in the center of the Galaxy. It is, however, still unclear, where these
relatively young stars were born and which dynamical process pushed them to
nearly radial orbits around the SMBH. In this paper we investigate the
possibility that the young binaries originated from a thin eccentric disc,
similar to the one observed in the Galactic center nowadays. By means of direct
N-body simulations, we follow the dynamical evolution of an initially thin and
eccentric disc of stars with a 100% binary fraction orbiting around the SMBH.
Such a configuration leads to Kozai-Lidov oscillations of orbital elements,
bringing considerable amount of binaries to close vicinity of the black hole.
Subsequent tidal disruption of these binaries accelerates one of their
component to velocities well above the escape velocity from the SMBH while the
second component becomes tightly bound to the SMBH. We describe the main
kinematic properties of the escaping and tightly bound stars within our model
and compare them qualitatively to the properties of the observed HVSs and
S-stars, respectively. The most prominent feature is a strong anisotropy in the
directions of the escaping stars which is observed for the Galactic HVSs but
not explained yet.
