Direct N-body simulation of the Galactic centre.

We study the dynamics and evolution of the nuclear star cluster of the Milky Way galaxy performing a high resolution direct one-million-body simulation. We focus on the interaction of the stellar system with the supermassive black hole. We find that the 3D density distribution of stellar black holes after 5 Gyr is fully consistent with the Bahcall-Wolf slope of -1.75. We obtain the rate of tidal disruption events to be $4\times 10^{-6}$\yr$^{-1}$ and estimate the number of objects emitting gravitational waves during the accretion onto the supermassive black hole to be $\sim 230$ per Gyr with $\approx 100$ of them being possible extreme mass ratio inspirals. The examined binary fraction drops by less then a half from the initial value of 5\% with the final value of 3\% with 2.5\% inside the inner parsec. We discuss the contribution of binaries with compact objects in the presence of pulsars and of Supernovae Ia rates.