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(Abridged) The Galactic Center (GC) hosts a population of young stars some ofwhich seem to form mutually inclined discs of clockwise and counter clockwiserotating stars. We present a warped disc origin scenario for these starsassuming that an initially flat accretion disc becomes warped due to thePringle instability, or due to Bardeen-Petterson effect, before it fragments tostars. 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 andother parameters relevant to the GC environment, but also for more massivediscs. We take into account the disc's self-gravity and the torques exerted bya 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, butprecesses freely when the torques from a non-spherical cluster are included. Anintermediate-mass disc ($M_d / M_{bh} \sim 0.01$) breaks into pieces whichprecess independently in the self-gravity-only case, and become disrupted inthe 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 brokenbut not dissolved. The time-scale after which the disc breaks scales almostlinearly with ($M_d / M_{bh}$) for self-gravitating models. Typical values arelonger 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 acomparison of them with the clockwise disc shows that the lowest mass model ina spherical star cluster matches the data best.

On the possibility of a warped disc origin of the inclined stellar discs at the Galactic Centre