  Observations give evidences of the presence of metals in the intergalactic
medium (IGM). The stars responsible for transforming hydrogen and helium into
more complex atoms do not form outside the galaxies in the standard scenario of
galaxy formation. Supernovae-driven winds and their associated feedback was
proposed as a possible solution to explain such enrichment of the IGM. It
turned out that a proper modelling of supernovae explosions within a turbulent
interstellar medium (ISM) is a difficult task. Recent advances have been
obtained using a multiphase approach to solve for the thermal state of the ISM,
plus some additional recipes to account for the kinetic effect of supernovae on
the galactic gas. We briefly describe here our implementation of supernovae
feedback within the RAMSES code, and apply it to the formation and evolution of
isolated galaxies of various masses and angular momenta. We have explored under
what conditions a galactic wind can develop, if one considers only a quiescent
mode of star formation. We have also characterized the distribution and
evolution of metallicity in the gas outflow spreading in the IGM.
