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Momentum deposition by radiation pressure from young, massive stars may helpto destroy molecular clouds and unbind stellar clusters by driving large-scaleoutflows. We extend our previous numerical radiation hydrodynamic study ofturbulent, star-forming clouds to analyze the detailed interaction betweennon-ionizing UV radiation and the cloud material. Our simulations trace theevolution of gas and star particles through self-gravitating collapse, starformation, and cloud destruction via radiation-driven outflows. These modelsare idealized in that we include only radiation feedback and adopt anisothermal equation of state. Turbulence creates a structure of dense filamentsand large holes through which radiation escapes, such that only ~50% of theradiation is (cumulatively) absorbed by the end of star formation. The surfacedensity distribution of gas by mass as seen by the central cluster is roughlylognormal with sigma_ln(Sigma) = 1.3-1.7, similar to the externally-projectedsurface density distribution. This allows low surface density regions to bedriven outwards to nearly 10 times their initial escape speed v_esc. Althoughthe velocity distribution of outflows is broadened by the lognormal surfacedensity distribution, the overall efficiency of momentum injection to the gascloud is reduced because much of the radiation escapes. The mean outflowvelocity is approximately twice the escape speed from the initial cloud radius.Our results are also informative for understanding galactic-scale wind drivingby radiation, in particular the relationship between velocity and surfacedensity for individual outflow structures, and the resulting velocity and massdistributions arising from turbulent sources.

Numerical Simulations of Turbulent Molecular Clouds Regulated by Radiation Feedback Forces II: Radiation-Gas Interactions and Outflows