How to inflate a wind-blown bubble

Abstract

Stellar winds are one of several ways that massive stars can affect the star formation process on local and galactic scales. In this paper we investigate the numerical resolution needed to inflate an energy-driven stellar wind bubble in an external medium. We find that the radius of the wind injection region, $r_{\mathrm{inj}}$, must be below a maximum value, $r_{\mathrm{inj},\max }$, in order for a bubble to be produced, but must be significantly below this value if the bubble properties are to closely agree with analytical predictions. The final bubble momentum is within 25 per cent of the value from a higher resolution reference model if $\chi =r_{\mathrm{inj}}/r_{\mathrm{inj},\max }$ = 0.1. Our work has significance for the amount of radial momentum that a wind-blown bubble can impart to the ambient medium in simulations, and thus on the relative importance of stellar wind feedback.

arXiv comment9 pages, 6 figures. Accepted by MNRAS

References in corpus (24)

• The lifecycle of molecular clouds in nearby star-forming disc galaxies
• Fast and inefficient star formation due to short-lived molecular clouds and rapid feedback
• Molecular Cloud Formation in Shock-Compressed Layers
• Before the first supernova: combined effects of HII regions and winds on molecular clouds
• Feedback from Winds and Supernovae in Massive Stellar Clusters. I: Hydrodynamics
• Superbubbles in the Multiphase ISM and the Loading of Galactic Winds
• Magnetohydronamic Evolution of HII Regions in Molecular Clouds: Simulation Methodology, Tests, and Uniform Media
• A Detailed Study of Feedback from a Massive Star
• Maximally Star-Forming Galactic Disks II. Vertically-Resolved Hydrodynamic Simulations of Starburst Regulation
• The relative impact of photoionizing radiation and stellar winds on different environments
• Efficiently Cooled Stellar Wind Bubbles in Turbulent Clouds I. Fractal Theory and Application to Star-Forming Clouds
• Ion-by-ion Cooling efficiencies
• Evolution of supernovae-driven superbubbles with conduction and cooling
• Efficiently Cooled Stellar Wind Bubbles in Turbulent Clouds II. Validation of Theory with Hydrodynamic Simulations
• Two-Dimensional Hydrodynamic Models of Super Star Clusters with a Positive Star Formation Feedback
• The Geometry and Dynamical Role of Stellar Wind Bubbles in Photoionised HII Regions
• Cosmological simulations of dwarfs: the need for ISM physics beyond SN feedback alone
• How fast do young star clusters expel their natal gas?: Estimating the upper limit of the gas expulsion time-scale
• MHD simulation of the formation of clumps and filaments in quiescent diffuse medium by thermal instability
• A new mechanical stellar wind feedback model for the Rosette Nebula
• Magnetohydrodynamic simulations of mechanical stellar feedback in a sheet-like molecular cloud
• A New Computational Fluid Dynamics Code I: Fyris Alpha
• Hydrodynamic simulations of mechanical stellar feedback in a molecular cloud formed by thermal instability
• Self-Sealing Shells: Blowouts and Blisters on the Surfaces of Leaky Wind-Blown-Bubbles and Supernova Remnants

Cited by in corpus (2)

• Formation of star clusters and enrichment by massive stars in simulations of low-metallicity galaxies with a fully sampled initial stellar mass function
• A Massive Star is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars