We investigate the criteria under which SN-feedback can be resolved in simulations of galaxy formation and evolution by pure thermal injection of a canonical SN-energy of 1e51 erg. The simulations are carried out with the multi-method code P-Gadget-3. We test the behavior of three different solvers for the equation of hydrodynamics (SPH, MFM and MFV) and determine the resolution that is needed to resolve the Sedov-Taylor phase for each solver. Further, we investigate the effects of non-equilibrium cooling and chemistry and thermal conduction on physical properties of the SN-bubble 
and the SN-shell. 
Moreover, we carried out simulations of small patches of the ISM and apply SN-driving to investigate the effects of chemistry and thermal conduction on the properties of the SN-driven ISM. While we fin dominating VFF with and without thermal conduction the VFF in the case with thermal conduction are lie between 70 and 80 per cent which is in very good agreement with both theoretical findings and observations.