We present results of N-body simulations aimed at understanding the dynamics of young stars near the Galactic center .
Specifically , we model the inspiral of a cluster core containing an intermediate mass black hole and N \sim 50 cluster stars in the gravitational potential of a supermassive black hole .
We first study the elliptic three-body problem to isolate issues of tidal stripping and subsequent scattering , followed by full N-body simulations to treat the internal dynamics consistently .
We find that our simulations reproduce several dynamical features of the observed population .
These include the observed inner edge of the claimed clockwise disk , as well as the thickness of said disk .
We find that high density clumps , such as that claimed for IRS13E , also result generically from our simulations .
However , not all features of the observations are reproduced .
In particular , the surface density profile of the simulated disk scales as \Sigma \propto r ^ { -0.75 } , which is considerably shallower than that observed .
Further , at no point is any significant counter-rotating population formed .