  Both absorption and emission line studies show that cold gas around galaxies
is commonly outflowing at speeds of several hundred km$\,\textrm{s}^{-1}$. This
observational fact poses a severe challenge to our theoretical models of galaxy
evolution since most feedback mechanisms (e.g., supernovae feedback) accelerate
hot gas, and the timescale it takes to accelerate a blob of cold gas via a hot
wind is much larger than the time it takes to destroy the blob. We revisit this
long-standing problem using three-dimensional hydrodynamical simulations with
radiative cooling. Our results confirm previous findings, that cooling is often
not efficient enough to prevent the destruction of cold gas. However, we also
identify regions of parameter space where the cooling efficiency of the mixed,
`warm' gas is sufficiently large to contribute new comoving cold gas which can
significantly exceed the original cold gas mass. This happens whenever,
$t_{\mathrm{cool, mix}}/t_{\mathrm{cc}} < 1$, where $t_{\mathrm{cool,mix}}$ is
the cooling time of the mixed warm gas and $t_{\mathrm{cc}}$ is the
cloud-crushing time. This criterion is always satisfied for a large enough
cloud. Cooling `focuses' stripped material onto the tail where mixing takes
place and new cold gas forms. A sufficiently large simulation domain is crucial
to capturing this behavior.
