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The Galactic center hosts several hundred early-type stars, about 20% ofwhich lie in the so-called clockwise disk, while the remaining 80% do notbelong to any disks. The circumnuclear ring (CNR), a ring of molecular gas thatorbits the supermassive black hole (SMBH) with a radius of 1.5 pc, has beenclaimed to induce precession and Kozai-Lidov oscillations onto the orbits ofstars in the innermost parsec. We investigate the perturbations exerted by agas ring on a nearly-Keplerian stellar disk orbiting a SMBH by means ofcombined direct N-body and smoothed particle hydrodynamics simulations. Wesimulate the formation of gas rings through the infall and disruption of amolecular gas cloud, adopting different inclinations between the infalling gascloud and the stellar disk. We find that a CNR-like ring is not efficient inaffecting the stellar disk on a timescale of 3 Myr. In contrast, a gas ring inthe innermost 0.5 pc induces precession of the longitude of the ascending nodeOmega, significantly affecting the stellar disk inclination. Furthermore, thecombined effect of two-body relaxation and Omega-precession drives the stellardisk dismembering, displacing the stars from the disk. The impact of precessionon the star orbits is stronger when the stellar disk and the inner gas ring arenearly coplanar. We speculate that the warm gas in the inner cavity might haveplayed a major role in the evolution of the clockwise disk.

The influence of dense gas rings on the dynamics of a stellar disk in the Galactic center