Open AccessJournal Article
The Formation and Early Dynamical Evolution of Bound Stellar Systems
TLDR
In this paper, the results of numerical N-body calculations which simulate the dynamical evolution of young clusters as they emerge from molecular clouds have been presented, and the combination of these parameters which result in the production of bound stellar groups after the gas not used in star formation is completely dispersed.Abstract:
We present the results of numerical N-body calculations which simulate the dynamical evolution of young clusters as they emerge from molecular clouds. We follow the evolution of initially virialized stellar systems of 50 and, in some cases, 100 stars from the point in time immediately after the stars have formed in a cloud until a time long after all the residual star-forming gas has been dispersed from the system. By varying the star formation efficiency and the gas dispersal time for each model, we determined the combination of these parameters which result in the production of bound stellar groups after the gas not used in star formation is completely dispersed.read more
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Journal ArticleDOI
Gas expulsion and the destruction of massive young clusters
Simon P. Goodwin,Nate Bastian +1 more
TL;DR: In this paper, the authors examined the luminosity and dynamical mass estimates for young massive stellar clusters and showed that 50% of these clusters are likely to be destroyed within a few 10s Myr of their formation.
Posted Content
The Genesis of Super Star Clusters as Self-Gravitating HII Regions
TL;DR: In this paper, the effects of ionization, radiation pressure and main sequence winds from massive stars on self-gravitating, clumpy molecular clouds, thereby modeling the formation and pre-supernova feedback of massive star clusters were examined.
Turbulent, Molecular Clouds Regulated by Radiation Feedback
TL;DR: In this paper, a series of simulations employing the Hyperion radiation hydrodynamics solver was conducted to investigate how radiation forces influence realistic clouds, considering the regime that is optically thick to ultraviolet and optically thin to infrared radiation.
DissertationDOI
Numerical simulations on the formation of massive star clusters
TL;DR: In this paper, the Einflus des Gasausstoses auf die dynamische Entwicklung of Sternentstehungsregionen wurde untersucht.
Posted Content
Open clusters in a dispersing molecular cloud
Hui Chen Chen,Chung Ming Ko +1 more
TL;DR: In this paper, the authors used N-body simulations to find that most star clusters survive for more than 40 Myr even when the mass loss rate is high, which is the main reason for high infant mortality in star clusters.
References
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Journal ArticleDOI
Embedded Clusters in Molecular Clouds
TL;DR: The first extensive catalog of galactic embedded clusters is compiled, finding that the embedded cluster birthrate exceeds that of visible open clusters by an order of magnitude or more indicating a high infant mortality rate for protocluster systems.
Journal ArticleDOI
Theory of Star Formation
TL;DR: In this paper, an overall theoretical framework and the observations that motivate it are outlined, outlining the key dynamical processes involved in star formation, including turbulence, magnetic fields, and self-gravity.
Journal ArticleDOI
Young Massive Star Clusters
TL;DR: A review of the current state of the art in observations and dynamical modeling of young massive star clusters can be found in this paper, where the authors focus on star clusters younger than 100$ Myr, more than a few current crossing times old, and more massive than 10^4$Msun.
Book
Gravitational N-Body Simulations
TL;DR: The N-body problem has been studied in a wide range of applications, e.g., prediction-corrector methods, neighbor treatments, tree codes, chain procedures, and chain procedures with GRAPE as mentioned in this paper.
Journal ArticleDOI
A Universal Formation Mechanism for Open and Globular Clusters in Turbulent Gas
TL;DR: In this article, a universal mechanism for cluster formation in all epochs and environments is found to be consistent with the properties and locations of young and old globular clusters, open clusters and unbound associations, and interstellar clouds.