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We present three-dimensional radiation-hydrodynamical simulations of theimpact of stellar winds, photoelectric heating, photodissociating andphotoionising radiation, and supernovae on the chemical composition and starformation in a stratified disc model. This is followed with a sink-based modelfor star clusters with populations of individual massive stars. Stellar windsand ionising radiation regulate the star formation rate at a factor of ~10below the simulation with only supernova feedback due to their immediate impacton the ambient interstellar medium after star formation. Ionising radiation(with winds and supernovae) significantly reduces the ambient densities formost supernova explosions to rho < 10^-25 g cm^-3, compared to 10^-23 g cm^-3for the model with only winds and supernovae. Radiation from massive starsreduces the amount of molecular hydrogen and increases the neutral hydrogenmass and volume filling fraction. Only this model results in a molecular gasdepletion time scale of 2 Gyr and shows the best agreement with observations.In the radiative models, the Halpha emission is dominated by radiativerecombination as opposed to collisional excitation (the dominant emission innon-radiative models), which only contributes ~1-10 % to the total Halphaemission. Individual massive stars (M >= 30 M_sun) with short lifetimes areresponsible for significant fluctuations in the Halpha luminosities. Thecorresponding inferred star formation rates can underestimate the trueinstantaneous star formation rate by factors of ~10.

monthly notices of the royal astronomical society

The SILCC project --- IV. Impact of dissociating and ionising radiation  on the interstellar medium and Halpha emission as a tracer of the star  formation rate