Star Clusters as Tracers of Galactic Subsystems

1993 ◽  
pp. 323-324
Author(s):  
B. Barbuy ◽  
E. Bica ◽  
S. Ortolani
Keyword(s):  
Star Clusters

Star Clusters

1926 ◽  
Vol 134 (3) ◽  
pp. 157-157
Author(s):  
Henry Norris Russell
Keyword(s):  
Star Clusters

As Wonderful as Star Clusters: Instruments for Gazing at Tonality in Schubert

1999 ◽  
Vol 22 (3) ◽  
pp. 213-232 ◽  
Author(s):  
Richard L. Cohn
Keyword(s):  
Star Clusters

The Ionizing Star Clusters of Giant H [CSC]ii[/CSC] Regions in NGC 2403

1999 ◽  
Vol 117 (3) ◽  
pp. 1249-1274 ◽  
Author(s):  
Laurent Drissen ◽  
Jean-René Roy ◽  
Anthony F. J. Moffat ◽  
Michael M. Shara
Keyword(s):  
Star Clusters

scholarly journals Near-infrared surface brightness fluctuations and optical colours of Magellanic star clusters

2005 ◽  
Vol 363 (4) ◽  
pp. 1279-1289 ◽  
Author(s):  
R. A. González-Lópezlira ◽  
M. Y. Albarrán ◽  
M. Mouhcine ◽  
M. C. Liu ◽  
G. Bruzual-A. ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Near Infrared ◽  
Star Clusters ◽  
Surface Brightness Fluctuations

scholarly journals Formation of supermassive black hole seeds in nuclear star clusters via gas accretion and runaway collisions

2021 ◽  
Author(s):  
Arpan Das ◽  
Dominik R G Schleicher ◽  
Nathan W C Leigh ◽  
Tjarda C N Boekholt
Keyword(s):  
Black Holes ◽  
Initial Conditions ◽  
High Redshift ◽  
Star Clusters ◽  
Gas Reservoir ◽  
Highly Sensitive ◽  
Stellar Collisions ◽  
Key Variables ◽  
Chaotic Nature ◽  
Gas Accretion

Abstract More than two hundred supermassive black holes (SMBHs) of masses ≳ 109 M⊙ have been discovered at z ≳ 6. One promising pathway for the formation of SMBHs is through the collapse of supermassive stars (SMSs) with masses ∼103 − 5 M⊙ into seed black holes which could grow upto few times 109 M⊙ SMBHs observed at z ∼ 7. In this paper, we explore how SMSs with masses ∼103 − 5 M⊙ could be formed via gas accretion and runaway stellar collisions in high-redshift, metal-poor nuclear star clusters (NSCs) using idealised N-body simulations. We explore physically motivated accretion scenarios, e.g. Bondi-Hoyle-Lyttleton accretion and Eddington accretion, as well as simplified scenarios such as constant accretions. While gas is present, the accretion timescale remains considerably shorter than the timescale for collisions with the most massive object (MMO). However, overall the timescale for collisions between any two stars in the cluster can become comparable or shorter than the accretion timescale, hence collisions still play a crucial role in determining the final mass of the SMSs. We find that the problem is highly sensitive to the initial conditions and our assumed recipe for the accretion, due to the highly chaotic nature of the problem. The key variables that determine the mass growth mechanism are the mass of the MMO and the gas reservoir that is available for the accretion. Depending on different conditions, SMSs of masses ∼103 − 5 M⊙ can form for all three accretion scenarios considered in this work.

scholarly journals Ages of Galactic and Extragalactic Star Clusters of Various Abundances

1983 ◽  
Vol 6 ◽  
pp. 109-117 ◽  
Author(s):  
R.D. Cannon
Keyword(s):  
Star Clusters ◽  
Magellanic Clouds ◽  
Open Clusters ◽  
Simultaneous Solution ◽  
Low Mass Stars ◽  
Cluster Systems ◽  
Distant Cluster ◽  
Low Mass

In this review I shall concentrate mainly on globular star clusters in our Galaxy since these are the objects for which most work has been done recently, both observationally and theoretically. However, I shall also discuss briefly the oldest open clusters and clusters in the Magellanic Clouds. Little can be said about more distant cluster systems, since the only observations available are of integrated colours or spectra and these seem to be rather unreliable indicators of age. It is perhaps worth pointing out that the title may be slightly misleading; the problem is not so much to determine the ages of clusters of known abundances, as to obtain the best simultaneous solution for both age and composition, since some of the most important abundances (notably helium and oxygen) are virtually unobservable in little-evolved low mass stars.

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