The central bulge of M31 is observed to have two distinct brightness peaks with the separation of \sim 2 pc .
Tremaine ( 1995 ) recently proposed a new idea that the M31 ’ s nucleus is actually a single thick eccentric disk surrounding the central super-massive black hole .
In order to explore the origin of the proposed eccentric disk , we numerically investigate the dynamical evolution of a merger between a central massive black hole with the mass of \sim 10 ^ { 7 } M _ { \odot } and a compact stellar system with the mass of \sim 10 ^ { 6 } M _ { \odot } and the size of a few pc in the central 10 pc of a galactic bulge .
We found that the stellar system is destroyed by strong tidal field of the massive black hole and consequently forms a rotating nuclear thick stellar disk .
The orbit of each stellar component in the developed disk is rather eccentric with the mean eccentricity of \sim 0.5 .
These results imply that the M31 ’ s nuclear eccentric disk proposed by Tremaine ( 1995 ) can be formed by merging between a central massive black hole and a compact stellar system .
We furthermore discuss when and how a compact stellar system is transferred into the nuclear region around a massive black hole .