  Recent observations of the Galactic center revealed a nuclear disk of young
OB stars near the massive black hole (MBH), in addition to many similar
outlying stars with higher eccentricities and/or high inclinations relative to
the disk (some of them possibly belonging to a second disk). In addition,
observations show the existence of young B stars (the 'S-cluster') in an
isotropic distribution in the close vicinity of the MBH ($<0.04$ pc). We use
extended N-body simulations to probe the dynamical evolution of these two
populations. We show that the stellar disk could have evolved to its currently
observed state from a thin disk of stars formed in a gaseous disk, and that the
dominant component in its evolution is the interaction with stars in the cusp
around the MBH. We also show that the currently observed distribution of the
S-stars could be consistent with a capture origin through 3-body binary-MBH
interactions. In this scenario the stars are captured at highly eccentric
orbits, but scattering by stellar black holes could change their eccentricity
distribution to be consistent with current observations.
