The evolution of the Milky Way - A self-consistent chemodynamical model

A two-dimensional chemodynamical model of the Milky Way Galaxy is presented that can account for the structural, kinematical, and chemical pecularitie s of the galactic components in a self-consistent way. The dynamics of thre e stellar components and the multi-phase interstellar medium consisting of clouds and intercloud gas are followed in detail. Mass interchange and ener getic interaction processes between the stars and the gas phases are treate d simultaneously according to the astrophysical experience including star f ormation, supernovae type I and II, planetary nebulae, stellar winds, evapo ration and condensation, drag, cloud collisions, heating and cooling, and s tellar nucleosynthesis. These processes are coupling large ranges on tempor al and spatial scales, and allow for feedback and self-regulation mechanism s, which play a significant role in galactic evolution. In comparison with observations the capability of the chemodynamical treatment is convincingly proved by the excellent agreement with various observations. In addition, also well-known problems (G-dwarf problem, the discrepancy between local ef fective yields, etc.), which so far could be only explained by artificial c onstraints, are solved in the global scenario. Here we wish also to focus o n temporal behaviours of the radial abundance gradient and abundance ratios in order to stimulate further more specific observations and to make parti cular predictions which can test the validity of used model ingredients lik e stellar yields.