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 $\sim 10^{-3}$.

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

References in corpus (27)

• The lifecycle of molecular clouds in nearby star-forming disc galaxies
• The Dynamics of Radiation Pressure-Dominated HII Regions
• 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
• Dynamically Driven Evolution of the Interstellar Medium in M51
• Cloud Scale ISM Structure and Star Formation in M51
• Studying the YMC population of M83: how long clusters remain embedded, their interaction with the ISM and implications for GC formation theories
• Star Formation Relations in the Milky Way
• 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
• The dynamical evolution of molecular clouds near the Galactic Centre - II. Spatial structure and kinematics of simulated clouds
• Two-Dimensional Hydrodynamic Models of Super Star Clusters with a Positive Star Formation Feedback
• H$\alpha$ Morphologies of Star Clusters: A LEGUS study of HII region evolution timescales and stochasticity in low mass clusters
• Which feedback mechanisms dominate in the high-pressure environment of the Central Molecular Zone?
• On the hydrodynamics of the matter reinserted within superstellar clusters
• 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
• The formation of secondary stellar generations in massive young star clusters from rapidly cooling shocked stellar winds
• The roles of stellar feedback and galactic environment in star forming molecular clouds
• Forming clusters within clusters: How 30 Doradus recollapsed and gave birth again
• 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
• 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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