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The starburst galaxy M82 shows a system of H$\alpha$-emitting filaments whichextend to each side of the galactic disk. We model these filaments as theresult of the interaction between the winds from a distribution of SuperStellar Clusters (SSCs). We first derive the condition necessary for producinga radiative interaction between the cluster winds (a condition which is met bythe SSC distribution of M82). We then compute 3D simulations for SSC winddistributions which satisfy the condition for a radiative interaction, and alsofor distributions which do not satisfy this condition. We find that the highlyradiative models, that result from the interaction of high metallicity clusterwinds, produce a structure of H$\alpha$ emitting filaments, which qualitativelyagrees with the observations of the M82, while the non-radiative SSC windinteraction models do not produce filamentary structures. Therefore, ourcriterion for radiative interactions (which depends on the mass loss rate andthe terminal velocity of the SSC winds, and the mean separation between SSCs)can be used to predict whether or not an observed galaxy should have associatedH$\alpha$ emitting filaments.

Filaments in Galactic Winds Driven by Young Stellar Clusters