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Numerical Simulations of Turbulent, Molecular Clouds Regulated by Radiation Feedback Forces I: Star Formation Rate and Efficiency by Raskutti, Sudhir; Ostriker, Eve C.; Skinner, M. Aaron is a scholarly article available to read on EtoBox.

What is Numerical Simulations of Turbulent, Molecular Clouds Regulated by Radiation Feedback Forces I: Star Formation Rate and Efficiency about?

Radiation feedback from stellar clusters is expected to play a key role in setting the rate and efficiency of star formation in giant molecular clouds (GMCs). To investigate how radiation forces influence realistic turbulent systems, we have conducted a series of numerical simulations employing the {\it Hyperion} radiation hydrodynamics solver, considering the regime that is optically thick to ultraviolet (UV) and optically thin to infrared (IR) radiation. Our model clouds cover initial surface densities between $\Sigma_{\rm cl,0} \sim 10-300~M_{\odot}~{\rm pc^{-2}}$, with varying initial turbulence. We follow them through turbulent, self-gravitating collapse, formation of star clusters, and cloud dispersal by stellar radiation. All our models display a lognormal distribution of gas surface density $\Sigma$; for an initial virial parameter $\alpha_{\rm vir,0} = 2$, the lognormal standard deviation is $\sigma_{\rm ln \Sigma} = 1-1.5$ and the star formation rate coefficient $\varepsilon_{\rm ff,\bar\rho} = 0.3-0.5$, both of which are sensitive to turbulence but not radiation feedback. The net star formation efficiency $\varepsilon_\mathrm{final}$ increases with $\Sigma_{\rm cl,0}$ an

Author

Raskutti, Sudhir; Ostriker, Eve C.; Skinner, M. Aaron

Published

2016

Language

EN