We studied the dynamical evolution of the central parsec of the Milky Way, where stars have aspecific structure orbiting the Central Massive Black Hole. We consider that the central parsec consist of a very dense central cluster within the inner-most Arcsec, which is referred as the S-cluster, and two outer orbiting disks. By presenting a series of N-body simulations the evolution of the this active central region is compared to the observational data. The simulations were deployed on different software, such as NBODY4 and SyMBA, trying to reach the most accurate result. With the use of this Newtonian N-body simulation we study the evolution of the orbital eccentricity and inclination of the stars inside the central parsec of the Massive Black Hole(MBH), beginning from Boily’s initial conditions to making our own initial conditions and comparing them with each other and with the observed data. In the final simulation we find out that the smaller mass stars get more excited, whereas the massive stars have more balanced orbits which could lead to the conclusion that the initial mass function for the disk may be higher than what we expected it to be.