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We perform hydrodynamical simulations of a young galactic disc embedded in ahot gaseous halo using parameters typical for Lyman break galaxies (LBGs). Wetake into account the (static) gravitational potentials due to a dark matterhalo, a stellar bulge and a disc of stars and gas. Star formation is treated bya local Kennicutt-Schmidt law. We simplify the structure of the interstellarmedium by restricting the computational domain to a 25th of the full azimuthalangle, effectively assuming large-scale axisymmetry and neglecting any effectsof spiral structure, and focus on the large-scale ISM drivers, thesuperbubbles. Supernovae are triggered randomly and have preset event sizes ofseveral tens to hundreds. We further investigate different halo gas pressuresand energy injection methods. Many of our simulated galaxies, but not all,develop bipolar outflows. We characterise the strength of the outflow by massand energy outflow rates, and investigate the effect of changes to the detailsof the model. We find that supernovae are more effective if comprised intolarger superbubbles. The weight and the pressure of the halo gas is able toquench galactic outflows. The wind emerges from a series of superbubbles inregions where a critical star formation density is exceeded. The superbubblesexpand into the gaseous halo at slightly supersonic speed, producing radiativeshock waves with similar characteristics as the absorptions systems observedaround LBGs.

Galactic winds - How to launch galactic outflows in typical Lyman-break galaxies