Infrared Radiation Feedback Does Not Regulate Star Cluster Formation

Abstract

We present 3D radiation-hydrodynamical (RHD) simulations of star cluster formation and evolution in massive, self-gravitating clouds, whose dust columns are optically thick to infrared (IR) photons. We use \texttt{VETTAM} -- a recently developed, novel RHD algorithm, which uses the Variable Eddington Tensor (VET) closure -- to model the IR radiation transport through the cloud. We also use realistic temperature ($T$) dependent IR opacities ($\kappa$) in our simulations, improving upon earlier works in this area, which used either constant IR opacities or simplified power laws ($\kappa \propto T^2$). We investigate the impact of the radiation pressure of these IR photons on the star formation efficiency (SFE) of the cloud, and its potential to drive dusty winds. We find that IR radiation pressure is unable to regulate star formation or prevent accretion onto the star clusters, even for very high gas surface densities ($\Sigma >10^5{M}_{\odot }{\mathrm{pc}}^{-2}$), contrary to recent semi-analytic predictions and simulation results using simplified treatments of the dust opacity. We find that the commonly adopted simplifications of $\kappa \propto T^2$ or constant $\kappa$ for the IR dust opacities leads to this discrepancy, as those approximations overestimate the radiation force. By contrast, with realistic opacities that take into account the micro-physics of the dust, we find that the impact of IR radiation pressure on star formation is very mild, even at significantly high dust-to-gas ratios ($\sim 3$ times solar), suggesting that it is unlikely to be an important feedback mechanism in controlling star formation in the ISM.

28 pages, 19 figures. MNRAS accepted. v2: Minor changes made to address referee comments

References in corpus (43)

• Array Programming with NumPy
• Shocks and cold fronts in galaxy clusters
• Slow Star Formation in Dense Gas: Evidence and Implications
• The Density Probability Distribution in Compressible Isothermal Turbulence: Solenoidal versus Compressive Forcing
• Modeling Collapse and Accretion in Turbulent Gas Clouds: Implementation and Comparison of Sink Particles in AMR and SPH
• The Mass-Metallicity and the Fundamental Metallicity Relation revisited on a fully Te-based abundance scale for galaxies
• A new Jeans resolution criterion for (M)HD simulations of self-gravitating gas: Application to magnetic field amplification by gravity-driven turbulence
• The Dynamics of Radiation Pressure-Dominated HII Regions
• Inefficient star formation through turbulence, magnetic fields and feedback
• A scheme for radiation pressure and photon diffusion with the M1 closure in RAMSES-RT
• The Global Evolution of Giant Molecular Clouds. I: Model Formulation and Quasi-Equilibrium Behavior
• Modeling jet and outflow feedback during star cluster formation
• A robust numerical scheme for highly compressible magnetohydrodynamics: Nonlinear stability, implementation and tests
• Driving Turbulence and Triggering Star Formation by Ionizing Radiation
• Equations and Algorithms for Mixed Frame Flux-Limited Diffusion Radiation Hydrodynamics
• The dynamics and outcome of star formation with jets, radiation, winds, and supernovae in concert
• Cloud Scale ISM Structure and Star Formation in M51
• The sonic scale revealed by the world's largest supersonic turbulence simulation
• Studying the YMC population of M83: how long clusters remain embedded, their interaction with the ISM and implications for GC formation theories
• A Direct Multigrid Poisson Solver for Oct-Tree Adaptive Meshes
• Star clusters near and far; tracing star formation across cosmic time
• An Unstable Truth: How Massive Stars get their Mass
• The molecular cloud lifecycle
• Gone With the Wind: Where is the Missing Stellar Wind Energy from Massive Star Clusters?
• Numerical Simulations of Turbulent, Molecular Clouds Regulated by Radiation Feedback Forces I: Star Formation Rate and Efficiency
• The Spatial Relation between Young Star Clusters and Molecular Clouds in M 51 with LEGUS
• Feedback in Clouds II: UV Photoionisation and the first supernova in a massive cloud
• Highly efficient star formation in NGC 5253 possibly from stream-fed accretion
• Radiation Feedback in ULIRGS: Are Photons Movers and Shakers?
• An Implicit Finite Volume Scheme to Solve the Time Dependent Radiation Transport Equation Based on Discrete Ordinates
• Which feedback mechanisms dominate in the high-pressure environment of the Central Molecular Zone?
• A 33 GHz Survey of Local Major Mergers: Estimating the Sizes of the Energetically Dominant Regions from High Resolution Measurements of the Radio Continuum
• Modeling UV Radiation Feedback from Massive Stars: I. Implementation of Adaptive Ray Tracing Method and Tests
• Star-Gas Surface Density Correlations in Twelve Nearby Molecular Clouds I: Data Collection and Star-Sampled Analysis
• Slow Star Formation in the Milky Way: Theory Meets Observations
• Combining radiative transfer and diffuse interstellar medium physics to model star formation
• Non-linear Evolution of Rayleigh-Taylor Instability in a Radiation Supported Atmosphere
• New Insights into the Physical Conditions and Internal Structure of a Candidate Proto-Globular Cluster
• Embedded Young Massive Star Clusters in the Antennae Merger
• VETTAM: A scheme for radiation hydrodynamics with adaptive mesh refinement using the variable Eddington tensor method
• The Three Young Nuclear Super Star Clusters in NGC 5253
• Towards a More Complex Understanding of Natal Super Star Clusters with Multiwavelength Observations
• Is this an Early Stage Merger? A Case Study on Molecular Gas and Star Formation Properties of Arp 240

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