Berczik P. Self-consistent modeling of chemical and dynamical evolution of galaxies

The thesis is devoted to the study of complex modeling of the formation and evolution of galaxies and galactic structures using multivariate methods of numerical simulation based on the methods of particles (N-body problem). Multi-dimensional gas-dynamic calculations were carried out in the work as a method based on the "particle", namely SPH - Smoothed Particle Hydrodynamics. It is found that such approach provides a realistic description of the process of formation, chemical and dynamical evolution of disk galaxies over a cosmological timescale. It follows the evolution of all components of a galaxy such as dark matter, stars, and molecular clouds and diffuses interstellar matter (ISM). Dark matter and stars are treated as collisionless N-body systems. The ISM is numerically described by a SPH approach for the diffuse (hot/warm) gas and a sticky particle scheme for the (cool) molecular clouds. The thesis also analyzes in detail the dynamic evolution of the galactic center with single and double black holes. Here, we follow the long-term evolution of a massive binary in more realistic, triaxial and rotating galaxy models. We find that the binary does not stall. The binary hardening rates that we observe are sufficient to allow complete coalescence of binary SBHs in 1 Gyr or less, even in the absence of collisional loss-cone refilling or gas-dynamical torques, thus providing a potential solution to the final parsec problem. The final chapter examines in detail the evolution of star clusters of the galactic disk in the gravitational field of the galaxy. Tidal tails of star clusters are not homogeneous but show well defined clumps in observations as well as in numerical simulations. For the numerical realization we use star-by-star N-body simulations. We find a very good agreement of theory and models. We show that the radial offset of the tidal arms scales with the tidal radius, which is a function of cluster mass and the rotation curve at the cluster orbit. We present a quantitative derivation of the angular momentum and energy distribution of escaping stars from a star cluster in the tidal field of the Milky Way and derive the connection to the position and width of the clumps.