When Feedback Fails: The Scaling and Saturation of Star Formation Efficiency

Abstract

We present a suite of 3D multiphysics MHD simulations following star formation in isolated turbulent molecular gas discs ranging from 5 to 500 parsecs in radius. These simulations are designed to survey the range of surface densities between those typical of Milky Way giant molecular clouds (GMCs) (∼10^2M⊙pc^(−2)) and extreme ultraluminous infrared galaxy environments (∼10^4M⊙pc^(−2)) so as to map out the scaling of the cloud-scale star formation efficiency (SFE) between these two regimes. The simulations include prescriptions for supernova, stellar wind, and radiative feedback, which we find to be essential in determining both the instantaneous per-freefall (ε_(ff)) and integrated (ε_(int)) star formation efficiencies. In all simulations, the gas discs form stars until a critical stellar surface density has been reached and the remaining gas is blown out by stellar feedback. We find that surface density is a good predictor of ε_(int), as suggested by analytic force balance arguments from previous works. SFE eventually saturates to ∼1 at high surface density. We also find a proportional relationship between ε_(ff) and ε_(int), implying that star formation is feedback-moderated even over very short time-scales in isolated clouds. These results have implications for star formation in galactic discs, the nature and fate of nuclear starbursts, and the formation of bound star clusters. The scaling of ε_(ff) with surface density is not consistent with the notion that ε_(ff) is always ∼ 1 per cent on the scale of GMCs, but our predictions recover the ∼ 1 per cent value for GMC parameters similar to those found in spiral galaxies, including our own.

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