On the possibility of a warped disc origin of the inclined stellar discs
  at the Galactic Centre
  (Abridged) The Galactic Center (GC) hosts a population of young stars some of
which seem to form mutually inclined discs of clockwise and counter clockwise
rotating stars. We present a warped disc origin scenario for these stars
assuming that an initially flat accretion disc becomes warped due to the
Pringle instability, or due to Bardeen-Petterson effect, before it fragments to
stars. We show that this is plausible if the star formation efficiency
$\epsilon_{SF} \lesssim 1$, and the viscosity parameter $\alpha \sim 0.1$.
After fragmentation, we model the disc as a collection of concentric, circular,
mutually tilted rings, and construct warped disc models for mass ratios and
other parameters relevant to the GC environment, but also for more massive
discs. We take into account the disc's self-gravity and the torques exerted by
a surrounding star cluster. We show that a self-gravitating low-mass disc ($M_d
/ M_{bh} \sim 0.001$) precesses in integrity in the life-time of the stars, but
precesses freely when the torques from a non-spherical cluster are included. An
intermediate-mass disc ($M_d / M_{bh} \sim 0.01$) breaks into pieces which
precess independently in the self-gravity-only case, and become disrupted in
the presence of the star cluster torques. For a high-mass disc ($M_d / M_{bh}
\sim 0.1$) the evolution is dominated by self-gravity and the disc is broken
but not dissolved. The time-scale after which the disc breaks scales almost
linearly with ($M_d / M_{bh}$) for self-gravitating models. Typical values are
longer than the age of the stars for a low mass disc, and are in the range
$\sim 8 \times 10^4-10^5$ yr for high and intermediate-mass discs respectively.
None of these models explain the rotation properties of the two GC discs, but a
comparison of them with the clockwise disc shows that the lowest mass model in
a spherical star cluster matches the data best.
