  The presence of young stars, aged around several million years and situated
within the range of $\sim 0.04-1$ pc from our Galactic center raises a question
about their origins and dynamical evolutions. Their kinematics provide an
opportunity to explore their formation or possible subsequent dynamical
evolution. If Sagittarius A* was active in the past as suggested by several
observations, the accretion disk may have a significant impact on the dynamics
of stars in the Galactic center. The drag force exerted on stars during
star-disk interaction could lead some of them to sink into the accretion disk,
and these embedded stars will rapidly migrate inward and eventually be
disrupted within $\sim10^5$ yr. This could roughly explain the absence of stars
within $2.5 \times 10^4 R_{\rm g}$ ($\sim$ 1000 au). Additionally, Kozai-Lidov
oscillations, induced by the gravitational perturbation of the disk, could
contribute to the bimodal distribution of S-star inclinations and drive a
majority of stars into high eccentricity orbits.
