Evolution of Thermal Conducting Clouds Embedded in Galactic Winds

We performed high resolution hydrodynamical simulations of dense cool clouds embedded in supernova-driven galactic superwinds. Here we present preliminary results of our reference model in which the effect of heat conduction are taken into account. Significant dynamical differences occur between simulations with and without heat conduction. In absence of heat conduction the cloud fragments in few dynamical timescale. The inclusion of heat conduction has the effect to stabilize the cloud and inhibit the growth of Kelvin-Helmholtz and Reyleigh-Taylor instabilities. Furthermore in the conditions met in our simulations the strong heat flux at the cloud edge generates a converging shock which compresses the cloud. We also calculate the high energy emission (Ovi and soft X-ray) of the cloud and Ovi absorption line properties and compare the results with obvervations. Models in which heat conduction is taken into account seem to fit the observations much better. In general only a small fraction (0.1-0.4%) of the wind mechanical energy intersecting the cloud is radiated away. Finally some of our models are able to explain the low metallicity abundance seen in X-ray osservation of superwinds.