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[abridged] The pressure exerted by the radiation of young stars may be animportant feedback mechanism in forming star clusters and the disks ofstarburst galaxies. However, there is great uncertainty in how efficientlyradiation couples to matter in these high optical depth environments. Inparticular, it is unclear what levels of turbulence the radiation can produce,and whether the infrared radiation trapped by the dust opacity can give rise toheavily mass-loaded winds. In this paper we report a series of two-dimensionalflux-limited diffusion radiation-hydrodynamics calculations performed with thecode ORION in which we drive strong radiation fluxes through columns of dustymatter confined by gravity. We consider both systems where the radiation fluxis sub-Eddington throughout the gas column, and where it is super-Eddington atthe midplane but sub-Eddington in the atmosphere. In the latter, we find thatthe radiation-matter interaction gives rise to radiation-driven Rayleigh-Taylorinstability, which drives supersonic turbulence at a level sufficient to fullyexplain the turbulence seen in Galactic protocluster gas clouds, and to make anon-trivial contribution to the turbulence observed in starburst galaxy disks.However, the instability also produces a channel structure in which theradiation-matter interaction is reduced because the radiation field is notfully trapped. For astrophysical parameters relevant to forming star clustersand starburst galaxies, we find that this effect reduces the net momentumdeposition rate in the dusty gas by a factor of ~2-6 compared to simpleanalytic estimates, and that in steady state the Eddington ratio reaches unityand there are no strong winds. We provide an approximation formula, appropriatefor implementation in analytic models and non-radiative simulations, for theforce exerted by the infrared radiation field in this regime.

Direct Numerical Simulation of Radiation Pressure-Driven Turbulence and Winds in Star Clusters and Galactic Disks