  We studied the effect of supernovae feedback on a disk galaxy, taking into
account the impact of infalling gas on both the star formation history and the
corresponding outflow structure, the apparition of a supernovae-driven wind
being highly sensitive to the halo mass, the galaxy spin and the star formation
efficiency. We model our galaxies as cooling and collapsing NFW spheres. The
dark matter component is modelled as a static external potential, while the
baryon component is described by the Euler equations using the AMR code RAMSES.
Metal-dependent cooling and supernovae-heating are also implemented using
state-of-the-art recipes coming from cosmological simulations. We allow for 3
parameters to vary: the halo circular velocity, the spin parameter and the star
formation efficiency. We found that the ram pressure of infalling material is
the key factor limiting the apparition of galactic winds. We obtain a very low
feedback efficiency, with supernovae to wind energy conversion factor around
one percent, so that only low cicrular velocity galaxies give rise to strong
winds. For massive galaxies, we obtain a galatic fountain, for which we discuss
the observational properties. We conclude that for quiescent isolated galaxies,
galactic winds appear only in very low mass systems. Although that can quite
efficiently enrich the IGM with metals, they don't carry away enough cold
material to solve the overcooling problem.
