Modeling the Circumnuclear Disk and the Young Stellar Disks at the Galactic Center The Galactic Centre harbors a super massive black hole with a mass of 4x106 Msun. The black hole is surrounded by a group of young stars, as well as by a molecular disk, the so-called Circumnunclear Disk (CND). Roughly one half of the young stars appear to form a coherent disk, rotating clockwise on the plane of the sky. Both the clockwise young stellar disk, and the CND exhibit warping to different degrees. In this work, we investigated the long term evolution of the young stellar disk and the CND by use of numerical simulations taking into account the radial extent of the CND for the first time. We constrained the physical parameters for these systems for which they sustain their orbital stability. We investigated which radial extent values for the CND existing in the literature are consistent with the observed structure of CND. Adopting various surface density profiles for our disks in our simulations and making comparisons with previous work, we concluded that the surface density profile of the CND can not be constant along radius. We also determined the radial extents and the surface density profiles for which the effects of the CND on the evolution of the young stellar disk become nonnegligible.
