Abstract. About one hundred young stars orbiting a central supermassive black hole are observed in the innermost parsec of our Galaxy. Roughly one half of them forms a coherently rotating disk. Other observations reveal a massive molecular torus with characteristic radius of ≈ 2 pc. In this work we attempt to model the orbital evolution of the self-gravitating disk of young stars numerically, considering the gravitational influence of the torus. The results show precession of stellar orbits in the disk, which strongly depends on the inclination of the orbit with respect to the plane of the torus. This inclination is affected by the two-body relaxation of the stellar disk which, therefore, accelerates the precession. Moreover, the dependence of the precession rate upon the semi-major axis of the orbit leads to warping of the disk. Considering these results, we suggest that all of the observed young stars may have been formed in a single disk, which was partially destroyed during its lifetime by the precession
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