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We have performed a series of three-dimensional simulations of theinteraction of a supersonic wind with a non-spherical radiative cloud. Thesesimulations are motivated by our recent three-dimensional model of astarburst-driven galactic wind interacting with an inhomogeneous disk, whichshow that an optically emitting filament can be formed by the break-up andacceleration of a cloud into a supersonic wind. In this study we consider theevolution of a cloud with two different geometries (fractal and spherical) andinvestigate the importance of radiative cooling on the cloud's survival. Wehave also undertaken a comprehensive resolution study in order to ascertain theeffect of the assumed numerical resolution on the results. We find that theability of the cloud to radiate heat is crucial for its survival. While anadiabatic cloud is destroyed over a short period of time, a radiative cloud isbroken up via the Kelvin-Helmholtz instability into numerous small, densecloudlets, which are drawn into the flow to form a filamentary structure. Thedegree of fragmentation is highly dependent on the resolution of thesimulation, with the number of cloudlets formed increasing as theKelvin-Helmholtz instability is better resolved. Nevertheless, there is a clearqualitative trend, with the filamentary structure still persistent at highresolution. We confirm the mechanism behind the formation of the H-alphaemitting filaments found in our global simulations of a starburst-driven wind.Based on our resolution study, we conclude that bow shocks around acceleratedgas clouds, and their interaction, are the main source of the soft X-rayemission observed in these galactic-scale winds. [ABRIDGED]

Starburst-Driven Galactic Winds: Filament Formation and Emission Processes