Spectral shifting strongly constrains molecular cloud disruption by radiation pressure on dust

Abstract

$\mathbf{Aim}:$ To test the hypothesis that radiation pressure from star clusters acting on dust is the dominant feedback agent disrupting the largest star-forming molecular clouds and thus regulating the star-formation process. $\mathbf{Methods}:$ We perform multi-frequency, 3D, RT calculations including scattering, absorption, and re-emission to longer wavelengths for clouds with masses of $10^4$-$10^7$M${}_{\odot }$, with embedded clusters and a star formation efficiencies of 0.009%-91%, and varying maximum grain sizes up to 200$\mu$m. We calculate the ratio between radiative force and gravity to determine whether radiation pressure can disrupt clouds. $\mathbf{Results}:$ We find that radiation acting on dust almost never disrupts star-forming clouds. UV and optical photons to which the cloud is optically thick do not scatter much. Instead, they quickly get absorbed and re-emitted by at thermal wavelengths. As the cloud is typically optically thin to far-IR radiation, it promptly escapes, depositing little momentum. The resulting spectrum is more narrowly peaked than the corresponding Planck function with an extended tail at longer wavelengths. As the opacity drops significantly across the sub-mm and mm, the resulting radiative force is even smaller than for the corresponding single-temperature black body. The force from radiation pressure falls below the strength of gravitational attraction by an order of magnitude or more for either Milky Way or starbust conditions. For unrealistically large maximum grain sizes, and star formation efficiencies far exceeding 50% do we find that the strength of radiation pressure can exceed gravity. $\mathbf{Conclusions}:$ We conclude that radiation pressure acting on dust does not disrupt star-forming molecular clouds in any Local Group galaxies. Radiation pressure thus appears unlikely to regulate the star-formation process on either local or global scales.

20 pages, 17 figures

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• On the Origin of the High Star-Formation Efficiency in Massive Galaxies at Cosmic Dawn
• Optical depth in polarised Monte Carlo radiative transfer
• A deep-learning approach to the 3D reconstruction of dust density and temperature in star-forming regions