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Radiation feedback from young star clusters embedded in giant molecularclouds (GMCs) is believed to be important to the control of star formation. Forthe most massive and dense clouds, including those in which super star clusters(SSCs) are born, pressure from reprocessed radiation exerted on dust grains maydisperse a significant portion of the cloud mass back into the interstellarmedium (ISM). Using our radiaton hydrodynamics (RHD) code, Hyperion, we conducta series of numerical simulations to test this idea. Our models follow theevolution of self-gravitating, strongly turbulent clouds in which collapsingregions are replaced by radiating sink particles representing stellar clusters.We evaluate the dependence of the star formation efficiency (SFE) on the sizeand mass of the cloud and $\kappa$, the opacity of the gas to infrared (IR)radiation. We find that the single most important parameter determining theevolutionary outcome is $\kappa$, with $\kappa \gtrsim 15 \text{ cm}^2 \text{g}^{-1}$ needed to disrupt clouds. For $\kappa = 20-40 \text{ cm}^2 \text{g}^{-1}$, the resulting SFE=50-70% is similar to empirical estimates for someSSC-forming clouds. The opacities required for GMC disruption likely apply onlyin dust-enriched environments. We find that the subgrid model approach ofboosting the direct radiation force $L/c$ by a "trapping factor" equal to acloud's mean IR optical depth can overestimate the true radiation force byfactors of $\sim 4-5$. We conclude that feedback from reprocessed IR radiationalone is unlikely to significantly reduce star formation within GMCs unlesstheir dust abundances or cluster light-to-mass ratios are enhanced.

Numerical Simulations of Turbulent Molecular Clouds Regulated by Reprocessed Radiation Feedback from Nascent Super Star Clusters