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tokens: At = 0, cold accretion and cold wind recycling each contributes roughly half of the total stars formed, while hot mode accretion contributes of star formation. Cold accretion dominates the supply of star-forming gas in all three simulations until = 2.0, after which cold wind recycling and hot mode accretion start to be important. Compared to the other simulations, the haloes in Refσ3 form many more stars from both cold accretion and wind recycling, not because of more inflow but because they have less outflow as a result of the smaller mass-loading factors. The slower wind speed in the RefSlow model increases cold wind recycling by a large amount compared to the fiducial simulation. As a result, the galaxies at = 0 are slightly more massive as wind recycling gains importance after = 2, but their stellar masses are still consistent with the observations. Intermediate-mass haloes : The = 0 stellar mass from all three simulations is consistent with the observations within a small factor. The evolution of stellar content in these haloes is qualitatively similar to the small-mass haloes but with several major differences. First, stars from all accretion channels formed earlier in these more massive haloes, as is expected from the hierarchical assembly of galaxies. Secondly, both hot accretion and hot wind recycling, though still subdominant over most of the time, become more important at low redshifts, and together contribute of the total stars formed at = 0. Thirdly, cold accretion still dominates star formation at > 2 but nearly stops after = 2 when the shock-heated gas starts to develop a hot corona in these haloes. In the end, cold accretion only accounts for of the total stars formed. Cold wind recycling still plays a critical role in determining the final stellar mass of the galaxies, and largely accounts for the differences among the three simulations. Its contribution is more prominent in the RefSlow simulation. Massive haloes : At the massive end, galaxies from the Ref and Refσ3 simulations evolve very similarly and overproduce stars by a factor of 3 at = 0 (Fig. 11 ). The Ref simulation has larger η in small haloes, but the differences in η decrease with σ and become the same when . Therefore, the larger mass-loading factor in the Ref simulation only affects the progenitor galaxies during the earliest stages of their assembly when they were still small. Since these haloes assembled fast at high redshifts, the different scalings of η and σ in the low-mass haloes have little effect on the massive galaxies in our simulations. Compared to the intermediate-mass haloes, they have even earlier star formation and a higher fraction of hot accretion and hot wind recycling. Except for the RefSlow simulation, where cold wind recycling is clearly more important for stellar growth than the other channels, all four accretion channels contribute comparable amounts in the other simulations, with cold accretion + cold wind recycling and hot accretion + hot