Abstract
Calculations of the evolution of the interstellar medium (ISM) in a one-zone model are presented. The purpose is to study the influences of different processes on the evolution of the ISM and the star-formation rate by applying a detailed description of the stars and the ISM as well as their interactions. Different processes and time-scales are taken into account: stellar evolutionary time-scales and nucleosynthesis, stellar mass loss and energy release to the ISM by means of both supernovae and stellar winds, and a multi-component ISM with phase transitions by means of condensation, evaporation, and ionization as well as metal-dependent heating and cooling of the different phases. Moreover, we allow for intrinsic heating of the cool star-forming clouds. The results show that in addition to the heating by means of supernovae that represents the global star-formation regulation mechanism young stars act predominantly already locally within the star-forming sites. Open-box models allowing for inflow of all existing gas phases with similar physical states but restricting the outflow to the hot phase only are able to explain successfully the dilution of metallicity and large fluctuations of the star-formation rate, of the volume-filling factors, and of the amounts of different gas phases.
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