We present our recently developed 3-dimensional chemodynamical code for galaxy evolution .
This code follows the evolution of different galactic components like stars , dark matter and different components of the interstellar medium ( ISM ) , i.e .
a diffuse gaseous phase and the molecular clouds .
Stars and dark matter are treated as collisionless N-body systems .
The ISM is numerically described by a smoothed particle hydrodynamics ( SPH ) approach for the diffuse gas and a sticky particle scheme for the molecular clouds .
Additionally , the galactic components are coupled by several phase transitions like star formation , stellar death or condensation and evaporation processes within the ISM .

As an example we show the dynamical and chemical evolution of a star forming dwarf galaxy with a total baryonic mass of 2 \cdot 10 ^ { 9 } M _ { \odot } .
After a moderate collapse phase the stars and the molecular clouds follow an exponential radial distribution , whereas the diffuse gas shows a central depression as a result of stellar feedback .
The metallicities of the galactic components behave quite differently with respect to their temporal evolution as well as their radial distribution .
Especially , the ISM is at no stage well mixed .