Hydrodynamic simulations of mechanical stellar feedback in a molecular cloud formed by thermal instability

Abstract

We have used the AMR hydrodynamic code, MG, to perform 3D hydrodynamic simulations with self-gravity of stellar feedback in a spherical clumpy molecular cloud formed through the action of thermal instability. We simulate the interaction of the mechanical energy input from 15 Msun, 40 Msun, 60 Msun and 120 Msun stars into a 100 pc-diameter 16,500 Msun cloud with a roughly spherical morphology with randomly distributed high density condensations. The stellar winds are introduced using appropriate non-rotating Geneva stellar evolution models. In the 15 Msun star case, the wind has very little effect, spreading around a few neighbouring clumps before becoming overwhelmed by the cloud collapse. In contrast, in the 40 Msun, 60 Msun and 120 Msun star cases, the more powerful stellar winds create large cavities and carve channels through the cloud, breaking out into the surrounding tenuous medium during the wind phase and considerably altering the cloud structure. After 4.97 Myrs, 3.97 Myrs and 3.01 Myrs respectively, the massive stars explode as supernovae (SNe). The wind-sculpted surroundings considerably affect the evolution of these SN events as they both escape the cloud along wind-carved channels and sweep up remaining clumps of cloud/wind material. The `cloud' as a coherent structure does not survive the SN from any of these stars, but only in the 120 Msun case is the cold molecular material completely destabilised and returned to the unstable thermal phase. In the 40 Msun and 60 Msun cases, coherent clumps of cold material are ejected from the cloud by the SN, potentially capable of further star formation.

33 pages, 26 figures, accepted to MNRAS 2017 June 6. Raw data available from http://doi.org/10.5518/201

References in corpus (10)

• Modelling the supernova-driven ISM in different environments
• Strong Lens Time Delay Challenge: II. Results of TDC1
• Million-Degree Plasma Pervading the Extended Orion Nebula
• The interaction of planetary nebulae and their AGB progenitors with the interstellar medium
• Gone With the Wind: Where is the Missing Stellar Wind Energy from Massive Star Clusters?
• The Massive Star-forming Regions Omnibus X-ray Catalog
• Feedback in Clouds II: UV Photoionisation and the first supernova in a massive cloud
• The Nature of the Velocity Field in Molecular Clouds. I. The Non-Magnetic Case
• Feedback from Winds and Supernovae in Massive Stellar Clusters - II. X-Ray Emission
• Radiation-pressure-driven dust waves inside bursting interstellar bubbles

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• Momentum and energy injection by a wind-blown bubble into an inhomogeneous interstellar medium
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