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Stellar winds contain enough energy to easily disrupt the parent cloudsurrounding a nascent star cluster, and for this reason have been consideredcandidates for regulating star formation. However, direct observations suggestmost wind power is lost, and Lancaster21a,b recently proposed that this is dueto efficient mixing and cooling processes. Here, we simulate star formationwith wind feedback in turbulent, self-gravitating clouds, extending ourprevious work. Our simulations cover clouds with initial surface density$10^2-10^4$ $M_{\odot} \, {\rm pc}^{-2}$, and show that star formation andresidual gas dispersal is complete within 2 - 8 initial cloud free-fall times.The "Efficiently Cooled" model for stellar wind bubble evolution predictsenough energy is lost for the bubbles to become momentum-driven, we find thisis satisfied in our simulations. We also find that wind energy losses fromturbulent, radiative mixing layers dominate losses by "cloud leakage" over thetimescales relevant for star formation. We show that the net star formationefficiency (SFE) in our simulations can be explained by theories that applywind momentum to disperse cloud gas, allowing for highly inhomogeneous internalcloud structure. For very dense clouds, the SFE is similar to those observed inextreme star-forming environments. Finally, we find that, while self-pollutionby wind material is insignificant in cloud conditions with moderate density(only $\lesssim 10^{-4}$ of the stellar mass originated in winds), oursimulations with conditions more typical of a super star cluster have starparticles that form with as much as 1\% of their mass in wind material.

Star Formation Regulation and Self-Pollution by Stellar Wind Feedback