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We have used the NIHAO simulations to explore how supernovae (SNe) affectstar formation in galaxies. We find that SN feedback operates on all scalesfrom the interstellar medium (ISM) to several virial radii. SNe regulate starformation by preventing condensation of HI into H$_2$ and by moving coldneutral gas to the hot HII phase. The first effect explains why the coldneutral gas in dwarf galaxies forms stars inefficiently. The second maintainsthe hot ISM of massive galaxies (HII vents out at lower masses). At $v_{\rmvir}\simeq 67{\rm\,km\,s}^{-1}$, the outflow rate follows the relation:$\dot{M}_{\rm out}=23\,(v_{\rm vir}/67{\rm\,km\,s}^{-1})^{-4.6}\,{\rm SFR}$.$20\%$ to $70\%$ of the gas expelled from galaxies escapes from the halo(ejective feedback) but outflows are dominated by cold swept-up gas, most ofwhich falls back onto the galaxy on a $\sim 1\,$Gyr timescale. This `fountainfeedback' reduces the masses of galaxies by a factor of two to four, since gasspends half to three quarter of its time in the fountain. Less than $10\%$ ofthe ejected gas mixes with the hot circumgalactic medium and this gas isusually not reaccreted. On scales as large as $6r_{\rm vir}$, galactic windsdivert the incoming gas from cosmic filaments and prevent if from accretingonto galaxies (pre-emptive feedback). This process is the main reason for thelow baryon content of ultradwarves.

NIHAO XIX: How supernova feedback shapes the galaxy baryon cycle