  Our three-dimensional hydro-dynamical simulations of starbursts examine the
formation of superbubbles over a range of driving luminosities and mass
loadings that determine superbubble growth and wind velocity. From this we
determine the relationship between the velocity of a galactic wind and the
power of the starburst. We find a threshold for the formation of a wind, above
which the speed of the wind is not affected by grid resolution or the
temperature floor of our radiative cooling. We investigate the effect two
different temperature floors in our radiative cooling prescription have on wind
kinematics and content. We find that cooling to $10$ K instead of to $10^4$ K
increases the mass fraction of cold neutral and hot X-ray gas in the galactic
wind while halving that in warm H$\alpha$. Our simulations show the mass of
cold gas transported into the lower halo does not depend on the starburst
strength. Optically bright filaments form at the edge of merging superbubbles,
or where a cold dense cloud has been disrupted by the wind. Filaments formed by
merging superbubbles will persist and grow to $>400$ pc in length if anchored
to a star forming complex. Filaments embedded in the hot galactic wind contain
warm and cold gas that moves $300-1200$ km s$^{-1}$ slower than the surrounding
wind, with the coldest gas hardly moving with respect to the galaxy. Warm and
cold matter in the galactic wind show asymmetric absorption profiles consistent
with observations, with a thin tail up to the wind velocity.
