Here results of numerical radiation hydrodynamical simulations arepresented which explore the energetic impact of massive stars on the interstellar medium. We study the evolution of the ambient gas around isolated massive stars in the mass range between 15 and 85 M๏ in order to analyze the formation of structures and further the transfer and deposit of the stellar wind and radiation energy into the circumstellar medium until the stars explode as a supernovae. The derived energy transfer efficiencies are much smaller thananalytically estimated and should be inserted into chemo-dynamicalevolutionary models of galaxies as appropriate parameter values. As an additional issue the element release in the Wolf-Rayet phases and its detectability have been investigated for comparison with observations.