  Since stellar populations enhance particular element abundances according to
the yields and lifetimes of the stellar progenitors, the chemical evolution of
galaxies serves as one of the key tools that allows the tracing of galaxy
evolution. In order to deduce the evolution of separate galactic regions one
has to account for the dynamics of the interstellar medium, because distant
regions can interact by means of large-scale dynamics. To be able to interpret
the distributions and ratios of the characteristic elements and their relation
to e.g. the galactic gas content, an understanding of the dynamical effects
combined with small-scale transitions between the gas phases by evaporation and
condensation is essential. In this paper, we address various complex signatures
of chemical evolution and present in particular two problems of abundance
distributions in different types of galaxies: the discrepancies of metallicity
distributions and effective yields in the different regions of our Milky Way
and the N/O abundance ratio in dwarf galaxies. These can be solved properly, if
the chemodynamical prescription is applied to simulations of galaxy evolution.
