We study the impact of stellar winds and supernovae on the multi-phase interstellar medium using three-dimensional hydrodynamical simulations carried out with FLASH .
The selected galactic disc region has a size of ( 500 { pc } ) ^ { 2 } \times \pm 5 { kpc } and a gas surface density of 10 { M } _ { \odot } { pc } ^ { -2 } .
The simulations include an external stellar potential and gas self-gravity , radiative cooling and diffuse heating , sink particles representing star clusters , stellar winds from these clusters which combine the winds from individual massive stars by following their evolution tracks , and subsequent supernova explosions .
Dust and gas ( self- ) shielding is followed to compute the chemical state of the gas with a chemical network .
We find that stellar winds can regulate star ( cluster ) formation .
Since the winds suppress the accretion of fresh gas soon after the cluster has formed , they lead to clusters which have lower average masses ( 10 ^ { 2 } -10 ^ { 4.3 } { M } _ { \odot } ) and form on shorter timescales ( 10 ^ { -3 } -10 Myr ) .
In particular we find an anti-correlation of cluster mass and accretion time scale .
Without winds the star clusters easily grow to larger masses for \sim 5 Myr until the first supernova explodes .
Overall the most massive stars provide the most wind energy input , while objects beginning their evolution as B type stars contribute most of the supernova energy input .
A significant outflow from the disk ( mass loading \gtrsim 1 at 1 kpc ) can be launched by thermal gas pressure if more than 50 % of the volume near the disc mid-plane can be heated to T > 3 \times 10 ^ { 5 } K. Stellar winds alone can not create a hot volume-filling phase .
The models which are in best agreement with observed star formation rates drive either no outflows or weak outflows .