Simulations of pre-supernova feedback in spherical clouds

Abstract

We present a one-dimensional radiation-hydrodynamic model of a spherically symmetric cloud evolving under the influence of the self-gravity and the feedback from a star cluster forming in its centre. On one hand, the model is simple due to its 1D geometry, on the other hand, the feedback includes the ionising radiation, stellar winds and the radiation pressure acting on gas and dust. The star cluster is formed from the gas flowing into the cloud centre and the feedback parameters are determined from stellar evolution models and the cluster star forming history. The model is compared to the semi-analytic code WARPFIELD implementing similar physical processes and exploring the scenario that the young cluster R136 in the Large Magellanic Cloud was formed due to re-collapse of the shell formed by the previous generation star cluster. A good qualitative agreement is found, however, $3-4$ times higher stellar mass is needed to disrupt the cloud in our model, because it takes into account (contrary to WARPFIELD) self-gravity of the cloud surrounding the shell. We use the model to explore star formation in clouds with different mass, radius and density profile measuring their star formation efficiency (SFE), i.e. the fraction of the cloud mass converted to stars. We found that SFE is a function of a single parameter, $\log (\mathrm{SFE})\propto -n_{hm}^{-0.46}$, with $n_{hm}$ being the cloud mean particle density within its half-mass radius. Furthermore, we found that the feedback efficiency, i.e. a fraction of the feedback energy retained by gas, has a nearly constant value $\sim 10^{-3}$.

arXiv comment15 pages including appendix, 11 figures. Accepted for publication in MNRAS

References in corpus (91)

• The chemical composition of the Sun
• Galactic Stellar and Substellar Initial Mass Function
• The Star Formation Law in Nearby Galaxies on Sub-Kpc Scales
• Control of star formation by supersonic turbulence
• The Spitzer c2d Legacy Results: Star Formation Rates and Efficiencies; Evolution and Lifetimes
• Interstellar Turbulence I: Observations and Processes
• The Star Formation Rate of Turbulent Magnetized Clouds: Comparing Theory, Simulations, and Observations
• Self-Regulated Star Formation in Galaxies via Momentum Input from Massive Stars
• The Star Formation Rate of Supersonic MHD Turbulence
• Gravitational Collapse in Turbulent Molecular Clouds. I. Gasdynamical Turbulence
• An Origin of Supersonic Motions in Interstellar Clouds
• The SILCC (SImulating the LifeCycle of molecular Clouds) project: I. Chemical evolution of the supernova-driven ISM
• On the Role of Massive Stars in the Support and Destruction of Giant Molecular Clouds
• Massive stars in massive clusters II: Disruption of bound clusters by photoionization
• The lifecycle of molecular clouds in nearby star-forming disc galaxies
• The Dynamics of Radiation Pressure-Dominated HII Regions
• The Magellanic Mopra Assessment (MAGMA). I. The Molecular Cloud Population of the Large Magellanic Cloud
• The PdBI Arcsecond Whirlpool Survey (PAWS): Environmental Dependence of Giant Molecular Cloud Properties in M51
• Fast and inefficient star formation due to short-lived molecular clouds and rapid feedback
• Before the first supernova: combined effects of HII regions and winds on molecular clouds
• Modeling UV Radiation Feedback from Massive Stars: II. Dispersal of Star-Forming Giant Molecular Clouds by Photoionization and Radiation Pressure
• A new radiative cooling curve based on an up to date plasma emission code
• Dispersal of molecular clouds by ionising radiation
• On Radiation Pressure in Static, Dusty HII Regions
• Feedback from Winds and Supernovae in Massive Stellar Clusters. I: Hydrodynamics
• Supernova Driving. I. The Origin of Molecular Cloud Turbulence
• A Comparative Study of Giant Molecular Clouds in M51, M33 and the Large Magellanic Cloud
• The Exciting Lives of Giant Molecular Clouds
• Dynamically Driven Evolution of the Interstellar Medium in M51
• Why are most molecular clouds not gravitationally bound?
• A Simple Law of Star Formation
• Breakdown of Kennicutt-Schmidt Law at GMC Scales in M33
• Molecular Gas Properties on Cloud Scales Across the Local Star-forming Galaxy Population
• Cloud Scale ISM Structure and Star Formation in M51
• The massive star initial mass function of the Arches cluster
• Winds and radiation in unison: a new semi-analytic feedback model for cloud dissolution
• Studying the YMC population of M83: how long clusters remain embedded, their interaction with the ISM and implications for GC formation theories
• On the function describing the stellar initial mass function
• Cloud-cloud collisions and triggered star formation
• Winds driven by super-star clusters: The self-consistent radiative solution
• The Star Formation Efficiency per Free Fall Time in Nearby Galaxies
• The linewidth-size relationship in the dense ISM of the Central Molecular Zone
• Star Formation Efficiency and Dispersal of Giant Molecular Clouds with UV Radiation Feedback: Dependence on Gravitational Boundedness and Magnetic Fields
• Structure and Feedback in 30 Doradus II. Structure and Chemical Abundances
• Non-universal star formation efficiency in turbulent ISM
• A 50 pc scale view of star formation efficiency across NGC 628
• Efficiently Cooled Stellar Wind Bubbles in Turbulent Clouds I. Fractal Theory and Application to Star-Forming Clouds
• From molecules to Young Stellar Clusters: the star formation cycle across the M33 disk
• Numerical Simulations of Turbulent Molecular Clouds Regulated by Reprocessed Radiation Feedback from Nascent Super Star Clusters
• Star Formation Relations in the Milky Way
• Molecular Cloud Evolution V. Cloud Destruction by Stellar Feedback
• Connecting Young Star Clusters to CO Molecular Gas in NGC 7793 with ALMA-LEGUS
• The Spatial Relation between Young Star Clusters and Molecular Clouds in M 51 with LEGUS
• Numerical Simulations of Turbulent, Molecular Clouds Regulated by Radiation Feedback Forces I: Star Formation Rate and Efficiency
• A double cluster at the core of 30 Doradus
• The dynamical evolution of molecular clouds near the Galactic Centre - II. Spatial structure and kinematics of simulated clouds
• Star formation in 30 Doradus
• Importance of the Initial Conditions for Star Formation - III: Statistical Properties of Embedded Protostellar Clusters
• Hubble Tarantula Treasury Project: Unraveling Tarantula's Web. II. Optical and Near Infrared Star Formation History of the Starburst Cluster NGC 2070 in 30 Doradus
• A general theory for the lifetimes of giant molecular clouds under the influence of galactic dynamics
• Gemini/GMOS search of massive binaries in the ionizing cluster of 30 Dor
• Feedback from massive stars at low metallicities: MUSE observations of N44 and N180 in the Large Magellanic Cloud
• Two Populations of Molecular Clouds in the Antennae Galaxies
• On The Nature of Variations in the Measured Star Formation Efficiency of Molecular Clouds
• H$\alpha$ Morphologies of Star Clusters: A LEGUS study of HII region evolution timescales and stochasticity in low mass clusters
• Two-Dimensional Hydrodynamic Models of Super Star Clusters with a Positive Star Formation Feedback
• Which feedback mechanisms dominate in the high-pressure environment of the Central Molecular Zone?
• On the hydrodynamics of the matter reinserted within superstellar clusters
• Bonn Optimized Stellar Tracks (BoOST). Simulated Populations of Massive and Very Massive Stars for Astrophysical Applications
• The EDGE-CALIFA survey: the influence of galactic rotation on the molecular depletion time across the Hubble sequence
• Time Varying Dynamical Star Formation Rate
• Star cluster formation and cloud dispersal by radiative feedback: dependence on metallicity and compactness
• Supernova feedback and the energy deposition in molecular clouds
• Star Formation in Transient Molecular Clouds
• How Significant is Radiation Pressure in the Dynamics of the Gas Around Young Stellar Clusters?
• Simulating radiative feedback and star cluster formation in GMCs: I. Dependence on gravitational boundedness
• The formation of secondary stellar generations in massive young star clusters from rapidly cooling shocked stellar winds
• Diffuse X-Ray Emission from the Quiescent Superbubble M17, the Omega Nebula
• The roles of stellar feedback and galactic environment in star forming molecular clouds
• A model for the onset of self-gravitation and star formation in molecular gas governed by galactic forces: II. the bottleneck to collapse set by cloud-environment decoupling
• Forming clusters within clusters: How 30 Doradus recollapsed and gave birth again
• Spatial Decorrelation of Young Stars and Dense Gas as a Probe of the Star Formation-Feedback Cycle in Galaxies
• Numerical Simulations of Turbulent Molecular Clouds Regulated by Radiation Feedback Forces II: Radiation-Gas Interactions and Outflows
• The growth of H II regions around massive stars: the role of metallicity and dust
• How radiation affects superbubbles: Through momentum injection in early phase and photo-heating thereafter
• On the impact of radiation pressure on the dynamics and inner structure of dusty wind-driven shells
• Feedback in W49A diagnosed with radio recombination lines and models
• Infrared Radiation Feedback Does Not Regulate Star Cluster Formation
• Star formation efficiencies of molecular clouds in a galactic center environment
• Photoionising feedback in spiral arm molecular clouds
• PHANGS: Constraining Star Formation Timescales Using the Spatial Correlations of Star Clusters and Giant Molecular Clouds

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