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Within the distance of 1 pc from the Galactic center (GC), more than 100young massive stars have been found. The massive stars at 0.1-1 pc from the GCare located in one or two disks, while those within 0.1 pc from the GC,S-stars, have an isotropic distribution. How these stars are formed is not wellunderstood, especially for S-stars. Here we propose that a young star clusterwith an intermediate-mass black hole (IMBH) can form both the disks andS-stars. We performed a fully self-consistent $N$-body simulation of a starcluster near the GC. Stars escaped from the tidally disrupted star cluster werecarried to the GC due to an 1:1 mean motion resonance with the IMBH formed inthe cluster. In the final phase of the evolution, the eccentricity of the IMBHbecomes very high. In this phase, stars carried by the 1:1 resonance with theIMBH were dropped from the resonance and their orbits are randomized by achaotic Kozai mechanism. The mass function of these carried stars is extremelytop-heavy within 10". The surface density distributions of young massive starshas a slope of -1.5 within 10" from the GC. The distribution of stars in themost central region is isotropic. These characteristics agree well with thoseof stars observed within 10" from the GC.

The origin of S-stars and a young stellar disk: distribution of debris stars of a sinking star cluster