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Feedback from supernovae is an essential aspect of galaxy formation. In orderto improve subgrid models of feedback we perform a series of numericalexperiments to investigate how supernova explosions power galactic winds. Weuse the Flash hydrodynamic code to model a simplified ISM, including gravity,hydrodynamics, radiative cooling above 10,000 K, and star formation thatreproduces the Kennicutt-Schmidt relation. By simulating a small patch of theISM in a tall box perpendicular to the disk, we obtain sub-parsec resolutionallowing us to resolve individual supernova events and we investigate how thewind properties depend on those of the ISM and the galaxy. We find thatoutflows are more efficient in disks with lower surface densities or gasfractions. A simple model in which the warm cloudy medium is the barrier thatlimits the expansion of blast waves reproduces the scaling of outflowproperties with disk parameters at high star formation rates. The scaling wefind sets the investigation of galaxy winds on a new footing, providing aphysically motivated sub-grid description of winds that can be implemented incosmological hydrodynamic simulations and phenomenological models. [Abridged]

How supernova explosions power galactic winds