One-dimensional dynamical calculations of the evolution of galaxies are presented taking into account a detailed description of the stars and a multi-component interstellar medium (ISM) as well as their interactions. Since cooling and heating processes depend on the metal content and because the dynamical behaviour of galaxies is determined by the internal energetic processes, both dynamical and chemical evolution cannot be considered separately but are intimately coupled. The results demonstrate the self-regulation of star formation and the generation of galactic mass loss by means of stellar heating of the ISM. In addition, they show convincingly that star formation can still proceed though galaxies lose hot gas by means of supernova-driven winds. Reasonably, the evolution of galaxies is mainly determined by both their initial masses and densities so that different evolutionary scenarios lead to the disconnection in the structures of giant and dwarf galaxies. The galactic evolution can nearly always be generally divided into an initial stage of continuous star-formation rate that is followed by star-formation bursts. Both timescales depend on the initial conditions. By this, the variety of dwarf galaxy types can be understood as different evolutionary stages.