  Within the central parsec of the Galaxy, several tens of young stars orbiting
a central supermassive black hole are observed. A subset of these stars forms a
coherently rotating disc. Other observations reveal a massive molecular torus
which lies at a radius ~1.5pc from the centre. In this paper we consider the
gravitational influence of the molecular torus upon the stars of the stellar
disc. We derive an analytical formula for the rate of precession of individual
stellar orbits and we show that it is highly sensitive upon the orbital
semi-major axis and inclination with respect to the plane of the torus as well
as on the mass of the torus. Assuming that both the stellar disc and the
molecular torus are stable on the time-scale >6Myr, we constrain the mass of
the torus and its inclination with respect to the young stellar disc. We
further suggest that all young stars observed in the Galactic Centre may have a
common origin in a single coherently rotating structure with an opening angle
<5deg, which was partially destroyed (warped) during its lifetime by the
gravitational influence of the molecular torus.
