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There is a dense group of OB and Wolf-Rayet stars within a fraction of aparsec from the super-massive black hole (SMBH) at the Galactic Center. Thesestars appear to be coeval and relatively massive. A subgroup of these starsorbits on the same plane. If they emerged with low to modest eccentricityorbits from a common gaseous disk around the central super-massive black hole,their inferred lifespan would not be sufficiently long to account for theexcitation of their high orbital eccentricity through dynamical relaxation.Here we analyze the secular perturbation on Galactic Center stars by anintermediate-mass companion (IMC) as a potential mechanism to account for theseyoung disk stars' high eccentricity. This IMC may be either anintermediate-mass black hole (IMBH) or a compact cluster such as IRS-13E. Ifits orbital angular momentum vector is anti-parallel to that of the disk stars,this perturbation would be effective in exciting the eccentricity of stars withorbital precession rates which resonate with IMC's precession rate. If itorbits around the SMBH in the same direction as the disk stars, theeccentricity of the young stars can still be highly excited by the IMC duringthe depletion of their natal disk, possible associated with the launch of theFermi bubble. In this scenario, IMC's precession rate decreases and its secularresonance sweeps through the proximity of the young stars. We carry outnumerical simulations with various inclination angles between the orbits of IMCand the disk stars and show this secular interaction is a robust mechanism toexcite the eccentricity and inclination of some disk stars.

The influence of the secular perturbation of an intermediate-mass companion: I. Eccentricity excitation of disk stars at the Galactic center