Dynamical interaction of supermassive black holes with the surrounding stellar system

Abstract

We use high resolution direct N-body simulation methods to study the stellar dynamics in the Galactic centre (GC) and in active galactic nuclei (AGN). We follow the evolution of the GC from the assumed in-situ formation of the nuclear star cluster (NSC) up to 5 Gyr using one million particles taking into account single and binary stellar evolution. We investigate 3D stellar density distributions, obtain rate of tidal disruption events, rate of hypervelocity star ejections and estimate the number of extreme mass-ratio inspirals. We examine the survivability of binary stars in the NSC and discuss the contribution of binaries with compact objects in presence of pulsars and Supernovae Ia rates in the GC. We use more simplified model to study the stellar dynamics in AGN. The analysis of two simulations with 128000 particles (with and without the accretion disk (AD)) shows that the interaction of the NSC with the AD leads to formation of a stellar disc in the central part of the NSC. We derive the mass and size of the formed stellar disc and discuss possible existence of such discs in some nearby galaxies.