  Galactic superbubbles are triggered by stellar feedback in the discs of
star-forming galaxies. They are important in launching galactic winds, which
play a key role in regulating the mass and energy exchange in galaxies.
Observations can only reveal projected information and the 3D structure of such
winds is quite complex. Therefore, numerical simulations are required to
further our understanding of such structures. Here, we describe hydrodynamical
simulations targeting two spatial scales. Large-scale superbubble models reveal
supernova-driven outflows, and their subsequent merging, which leads to
galactic wind formation. Additionally, the turbulence parameter $\sigma_t$ not
only affects disc formation, but also influences mass and energy
characteristics, controlling gas distribution and the injection rate in the
simulated star formation zone. Small-scale wind-multicloud models indicate that
isolated clouds are susceptible to instabilities, leading to fragmentation and
dense gas destruction. In contrast, in closer cloud configurations, the
condensation mechanism becomes important owing to hydrodynamic shielding, which
helps to maintain the cold material throughout the evolution of the system.
These simulations provide a comprehensive picture of galactic winds, showing
how large-scale superbubble dynamics create the environment where small-scale
wind-multicloud interactions shape the interstellar and circumgalactic media,
ultimately regulating galaxy evolution.
