Outflows Driven by Direct and Reprocessed Radiation Pressure in Massive Star Clusters

Abstract

We use three-dimensional radiation hydrodynamic (RHD) simulations to study the formation of massive star clusters under the combined effects of direct ultraviolet (UV) and dust-reprocessed infrared (IR) radiation pressure. We explore a broad range of mass surface density $\Sigma \sim 10^2$-$10^5{\mathrm{M}}_{\odot }{\mathrm{pc}}^{-2}$, spanning values typical of weakly star-forming galaxies to extreme systems such as clouds forming super-star clusters, where radiation pressure is expected to be the dominant feedback mechanism. We find that star formation can only be regulated by radiation pressure for $\Sigma \lesssim 10^3{\mathrm{M}}_{\odot }{\mathrm{pc}}^{-2}$, but that clouds with $\Sigma \lesssim 10^5{\mathrm{M}}_{\odot }{\mathrm{pc}}^{-2}$ become super-Eddington once high star formation efficiencies ($\sim 80\%$) are reached, and therefore launch the remaining gas in a steady outflow. These outflows achieve mass-weighted radial velocities of $\sim 15$ - $30\mathrm{km}{\mathrm{s}}^{-1}$, which is $\sim 0.5$ - $2.0$ times the cloud escape speed. This suggests that radiation pressure is a strong candidate to explain recently observed molecular outflows found in young super-star clusters in nearby starburst galaxies. We quantify the relative importance of UV and IR radiation pressure in different regimes, and deduce that both are equally important for $\Sigma \sim 10^3{\mathrm{M}}_{\odot }{\mathrm{pc}}^{-2}$, whereas clouds with higher (lower) density are increasingly dominated by the IR (UV) component. Comparison with control runs without either the UV or IR bands suggests that the outflows are primarily driven by the impulse provided by the UV component, while IR radiation has the effect of rendering a larger fraction of gas super-Eddington, and thereby increasing the outflow mass flux by a factor of $\sim 2$.

15 pages, 11 figures. MNRAS accepted. v2: Minor changes in text made to address referee comments

References in corpus (28)

• Array Programming with NumPy
• Modeling Collapse and Accretion in Turbulent Gas Clouds: Implementation and Comparison of Sink Particles in AMR and SPH
• Momentum Injection by Supernovae in the Interstellar Medium
• The Effects of Radiative Transfer on Low-Mass Star Formation
• The Importance of Radiative Feedback for the Stellar Initial Mass Function
• The Dynamics of Radiation Pressure-Dominated HII Regions
• Dynamics of Dusty Radiation Pressure Driven Shells and Clouds: Fast Outflows from Galaxies, Star Clusters, Massive Stars, and AGN
• A robust numerical scheme for highly compressible magnetohydrodynamics: Nonlinear stability, implementation and tests
• Equations and Algorithms for Mixed Frame Flux-Limited Diffusion Radiation Hydrodynamics
• A Direct Multigrid Poisson Solver for Oct-Tree Adaptive Meshes
• An Unstable Truth: How Massive Stars get their Mass
• The molecular cloud lifecycle
• Numerical Simulations of Turbulent, Molecular Clouds Regulated by Radiation Feedback Forces I: Star Formation Rate and Efficiency
• Highly efficient star formation in NGC 5253 possibly from stream-fed accretion
• Radiation Feedback in ULIRGS: Are Photons Movers and Shakers?
• Which feedback mechanisms dominate in the high-pressure environment of the Central Molecular Zone?
• Modeling UV Radiation Feedback from Massive Stars: I. Implementation of Adaptive Ray Tracing Method and Tests
• Dense CO in Mrk 71-A: Superwind Suppressed in a Young Super Star Cluster
• Hybrid Adaptive Ray-Moment Method (HARM${}^2$): A Highly Parallel Method for Radiation Hydrodynamics on Adaptive Grids
• Numerical Simulations of Turbulent Molecular Clouds Regulated by Radiation Feedback Forces II: Radiation-Gas Interactions and Outflows
• Infrared Radiation Feedback Does Not Regulate Star Cluster Formation
• VETTAM: A scheme for radiation hydrodynamics with adaptive mesh refinement using the variable Eddington tensor method
• Embedded Young Massive Star Clusters in the Antennae Merger
• Implementation of stellar heating feedback in simulations of star cluster formation: effects on the initial mass function
• The Three Young Nuclear Super Star Clusters in NGC 5253
• Towards a More Complex Understanding of Natal Super Star Clusters with Multiwavelength Observations
• Which Molecular Cloud Structures Are Bound?
• Clustered Star Formation in the center of NGC 253 Contributes to Driving the Ionized Nuclear Wind

Cited by in corpus (24)

• Efficient Formation of Massive Galaxies at Cosmic Dawn by Feedback-Free Starbursts
• Feedback-Free Starbursts at Cosmic Dawn: Observable Predictions for JWST
• Nitrogen-enriched, highly-pressurized nebular clouds surrounding a super star cluster at cosmic noon
• Pre-supernova feedback sets the star cluster mass function to a power law and reduces the cluster formation efficiency
• Massive star cluster formation I. High star formation efficiency while resolving feedback of individual stars
• SPICE: the connection between cosmic reionisation and stellar feedback in the first galaxies
• Density modulated star formation efficiency: implications for the observed abundance of ultra-violet luminous galaxies at z>10
• Growth of Massive Black-Holes in FFB Galaxies at Cosmic Dawn
• Lyman-$\alpha$ feedback prevails at Cosmic Dawn: Implications for the first galaxies, stars, and star clusters
• Witnessing an extreme, highly efficient galaxy formation mode with resolved Ly$\alpha$ and LyC emission
• Linking stellar populations to HII regions across nearby galaxies. II. Infrared Reprocessed and UV Direct Radiation Pressure in HII Regions
• An Asymptotically-Correct Implicit-Explicit Time Integration Scheme for Finite Volume Radiation-Hydrodynamics
• On the Origin of the High Star-Formation Efficiency in Massive Galaxies at Cosmic Dawn
• Effects of feedback-free starburst galaxies on the 21-cm signal and reionization history
• Investigating the ultraviolet and infrared radiation through the turbulent life of molecular clouds
• Playing with FIRE: A Galactic Feedback-Halting Experiment Challenges Star Formation Rate Theories
• Dust Eddington Ratios for Star-Forming Galaxy Subregions
• Non-explosive pre-supernova feedback in the COLIBRE model of galaxy formation
• Radiation-driven dusty outflows from early galaxies
• Resonant Drag Instabilities for Polydisperse Dust, I. The Acoustic Resonant Drag Instability
• A novel numerical method for mixed-frame multigroup radiation-hydrodynamics with GPU acceleration implemented in the QUOKKA code
• Lyman-$\alpha$ radiation pressure regulates star formation efficiency
• The Star Formation Factory revisited I. The impact of metallicity on collapsing star-forming clouds
• Star Formation