self-consistent SFRs, a multi-phase inhomogeneous ISM, and further more.

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Also more detailed numerical simulations [@db99; @rec06a], show that galactic winds are not very effective in removing gas from a galaxy. Although galactic winds develop vertically, while the horizontal transport along the disk is very limited, their efficiency depends very sensitively on the galaxy structure and ISM properties, as e.g. on the disk shape [@rec09]. Fig. \[fig:wind\] reveals clearly that the more eccentric the disk is, the more pronounced does the superbubble expand. On the one hand, the hot SN gas has to act against the galactic ISM, exciting turbulence and mixing between the metal-rich hot gas with the surrounding . Not taken into account in present-day models is the porosity of the ISM, consisting of clouds and diffuse less dense gas. In particular, the presence of clouds can hamper the development of galactic winds through their evaporation. This so-called mass loading reduces the wind momentum and internal energy. Since the metallicity in those clouds are presumably lower than the hot SNII gas, also the abundances in the outflow are diminished as e.g. observed in the galactic X-ray outflow of NGC 1569 [@mar02] for which a mass-loading 