Chemodynamical Simulations of Galaxies

We predict the frequency distribution of elemental abundance ratios from carbon to zinc as a functions of time and location, which can be directly compared with the next generation of the galactic archeology project such as the HERMES. We perform the chemodynamical simulations of a Milky Way-type galaxy from a CDM initial condition, using a self-consistent hydrodynamical code with supernova feedback and chemical enrichment. In the simulated galaxy, the kinematical and chemical properties of the bulge, disk, and halo are consistent with the observations. The bulges have formed from the assembly of subgalaxies at z >= 2 and have higher [alpha/Fe] ratios because of the lack of contribution of Type Ia Supernovae. The disks have formed with a constant star formation over 13 Gyr and show a decreasing trend of [a/Fe] and increasing trends of [(Na,Al,Cu,Mn)/Fe]. However, the thick disk stars tend to have higher [alpha/Fe] and lower [Mn/Fe] than thin disk stars. About 60% of the thick disk stars have formed in the satellite galaxies before they accrete on the disk in this CDM-based simulation.