AUTHORS: C. Evoli (SISSA, Trieste, Italy) & A. Ferrara (SNS, Pisa,
Italy)

I will present new results concerning supernova-driven outflows as a
mechanism to pump and sustain turbulence in the IGM surrounding
high-redshift galaxies. The evolution of winds is investigated via a
semi-analytic approach following both galaxy evolution along its
hierarchical growth and the expansion of supernova driven superbubbles
as they escape from the halo potential well.  We investigate the
turbulence evolution within the bubble using a novel approach based on
the spectral transfer equation. In brief, this approach allows to
follow the turbulent energy density deposited by galactic winds in the
IGM, its spectral features, dissipation, and to predict the
corresponding thermal/kinetic properties of such
component. Preliminary results will be presented showing the
contribution of turbulent pressure to QSO line-of-sights passing
nearby UV-selected galaxies at redshift 1.8 < z < 3.3.