Feedback from winds and supernovae in massive stellar clusters – I. Hydrodynamics
Hazel Rogers,Julian M. Pittard +1 more
TLDR
In this paper, the authors used 3D hydrodynamical models to investigate the effects of massive star feedback from winds and supernovae on inhomogeneous molecular material left over from the formation of a massive stellar cluster, and found that the densest molecular regions are surprisingly resistant to ablation by the cluster wind, in part due to shielding by other dense regions closer to the cluster.Abstract:
We use 3D hydrodynamical models to investigate the effects of massive star feedback from winds and supernovae on inhomogeneous molecular material left over from the formation of a massive stellar cluster. We simulate the interaction of the mechanical energy input from a cluster with 3 O-stars into a giant molecular cloud (GMC) clump containing 3240 solar masses of molecular material within a 4 pc radius. The cluster wind blows out of the molecular clump along low-density channels, into which denser clump material is entrained. We find that the densest molecular regions are surprisingly resistant to ablation by the cluster wind, in part due to shielding by other dense regions closer to the cluster. Nonetheless, molecular material is gradually removed by the cluster wind during which mass-loading factors in excess of several 100 are obtained. Because the clump is very porous, 60-75 per cent of the injected wind energy escapes the simulation domain, with the difference being radiated. After 4.4 Myr, the massive stars in our simulation begin to explode as supernovae. The highly structured environment into which the SN energy is released allows even weaker coupling to the remaining dense material and practically all of the SN energy reaches the wider environment. The molecular material is almost completely dispersed and destroyed after 6 Myr. The escape fraction of ionizing radiation is estimated to be about 50 per cent during the first 4 Myr of the cluster's life. A similar model with a larger and more massive GMC clump reveals the same general picture, though more time is needed for it to be destroyed.read more
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Dwarf galaxies, cold dark matter, and biased galaxy formation
Avishai Dekel,Joseph Silk +1 more
TL;DR: In this article, a reexamination is conducted of the formation of dwarf, diffuse, metal-poor galaxies due to supernova-driven winds, in view of data on the systematic properties of dwarfs in the Local Group and Virgo Cluster.
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The SILCC (SImulating the LifeCycle of molecular Clouds) project – I. Chemical evolution of the supernova-driven ISM
Stefanie Walch,Philipp Girichidis,T. Naab,Andrea Gatto,Simon C. O. Glover,Richard Wünsch,Ralf S. Klessen,Ralf S. Klessen,Ralf S. Klessen,Paul C. Clark,Thomas Peters,Dominik Derigs,Christian Baczynski +12 more
TL;DR: In this paper, the authors simulate the evolution of the multiphase ISM in a (500 pc)2 × ± 5 kpc region of a galactic disc, with a gas surface density of ΣGAS=10M⊙pc−2.
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The big problems in star formation: The star formation rate, stellar clustering, and the initial mass function
TL;DR: A review of the current state of the field of star formation can be found in this article, focusing on three central questions: What controls the rate at which gas in a galaxy converts to stars? What determines how those stars are clustered, and what fraction of the stellar population ends up in gravitationally-bound structures?
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Early disc accretion as the origin of abundance anomalies in globular clusters
Nate Bastian,Henny J. G. L. M. Lamers,S. E. de Mink,S. E. de Mink,Steven N. Longmore,Simon P. Goodwin,Mark Gieles +6 more
TL;DR: In this article, the authors present a model for the formation of GCs, where low-mass pre-main-sequence stars accrete enriched material released from interacting massive binary and rapidly rotating stars on to their circumstellar discs, and ultimately on to the young stars.
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Before the first supernova: combined effects of H II regions and winds on molecular clouds
TL;DR: In this paper, the authors acknowledge the German Deutsche Forschungsgemeinschaft, DFGPR 569/9-1 for the FP7 ERC advanced grant project ECOGAL.
References
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