Gas expulsion versus gas retention in young stellar clusters–II. Effects of cooling and mass segregation
TLDR
In this paper, the early development of star clusters in the extreme environments and discuss the restrictions that strong radiative cooling and stellar mass segregation provide on the gas expulsion from dense star-forming clouds.Abstract:
Gas expulsion or gas retention is a central issue in most of the models for multiple stellar populations and light element anti-correlations in globular clusters. The success of the residual matter expulsion or its retention within young stellar clusters has also a fundamental importance in order to understand how star formation proceeds in present-day and ancient star-forming galaxies and if proto-globular clusters with multiple stellar populations are formed in the present epoch. It is usually suggested that either the residual gas is rapidly ejected from star-forming clouds by stellar winds and supernova explosions, or that the enrichment of the residual gas and the formation of the second stellar generation occur so rapidly, that the negative stellar feedback is not significant. Here we continue our study of the early development of star clusters in the extreme environments and discuss the restrictions that strong radiative cooling and stellar mass segregation provide on the gas expulsion from dense star-forming clouds. A large range of physical initial conditions in star-forming clouds which include the star-forming cloud mass, compactness, gas metallicity, star formation efficiency and effects of massive stars segregation are discussed. It is shown that in sufficiently massive and compact clusters hot shocked winds around individual massive stars may cool before merging with their neighbors. This dramatically reduces the negative stellar feedback, prevents the development of the global star cluster wind and expulsion of the residual and the processed matter into the ambient interstellar medium. The critical lines which separate the gas expulsion and the gas retention regimes are obtained.read more
Citations
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Generation of massive stellar black holes by rapid gas accretion in primordial dense clusters
TL;DR: In this paper, the mass gap is filled by black holes that grow by gas accretion in dense stellar clusters, such as protoglobular clusters, and the accretion proceeds rapidly, during the first 10 megayears of the cluster life, before the remnant gas is depleted.
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When H ii regions are complicated: considering perturbations from winds, radiation pressure, and other effects
TL;DR: In this article, simple algebraic models are used to describe the expansion of photoionized HII regions under the influence of gravity and accretion in power-law density fields with ρ ∝ r−w, and determine when terms describing winds, radiation pressure, gravity, and photon breakout become significant enough to affect the dynamics of the H II region where w = 2.
Journal ArticleDOI
Generation of massive stellar black holes by rapid gas accretion in primordial dense clusters
TL;DR: In this article, the mass gap is filled by black holes that grow by gas accretion in dense stellar clusters, such as protoglobular clusters, and the accretion proceeds rapidly, during the first 10 megayears of the cluster life, before the remnant gas is depleted.
Journal ArticleDOI
Explaining the Multiple Populations in Globular Clusters by Multiple Episodes of Star Formation and Enrichment without Gas Expulsion from Massive Star Feedback
Jenny J. Kim,Young-Wook Lee +1 more
TL;DR: In this article, the authors investigated the origin of multiple stellar populations found in globular clusters (GCs) in the halo and bulge of the Milky Way, and constructed chemical evolution models for their putative low-mass progenitors.
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Two Thresholds for Globular Cluster Formation and their Dominance of Star Formation in the Early-Universe
TL;DR: In this article, the authors consider the conditions needed for the formation of a ~10^6 Msun cluster and show that such a cluster can be formed by a star formation rate inside each independent region that exceeds 1 Msun/yr to sample the cluster mass function up to a high mass.
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