The age distribution and history of formation of Large Magellanic Cloud clusters

1988 ◽  
Vol 100 ◽  
pp. 576 ◽  
Author(s):  
Paul Hodge
2018 ◽  
Vol 14 (S344) ◽  
pp. 118-121
Author(s):  
Rhorom Priyatikanto ◽  
Mochamad Ikbal Arifyanto ◽  
Rendy Darma ◽  
Aprilia ◽  
Muhamad Irfan Hakim

AbstractGlobal history of star or cluster formation in the Large Magellanic Cloud (LMC) has been the center of interest in several studies as it is thought to be influenced by tidal interaction with the Small Magellanic Cloud and even the Milky Way. This study focus on the formation history of the LMC in relation with the context of binary star clusters population, the apparent binary fraction (e.g., percentage of cluster pairs) in different epoch were calculated and analyzed. From the established distributions, it can be deduced that the binary clusters tend to be young (∽ 100 Myr) while their locations coincide with the locations of star forming complexes. There is an indication that the binary fraction increases as the rise of star formation rate in the last millions years. In the LMC, the increase of binary fraction at age ∽ 100 Myr can be associated to the last episode of close encounter with the Small Magellanic Cloud at ∽ 150 Myr ago. This observational evidence supports the theory of binary cluster formation through the fission of molecular cloud where the encounter between galaxies enhanced the clouds velocity dispersion which in turn increased the probability of cloud-cloud collisions that produce binary clusters.


1991 ◽  
Vol 148 ◽  
pp. 161-164 ◽  
Author(s):  
S. van den Bergh

Star clusters in the Magellanic Clouds (MCs) differ from those in the Galaxy in a number of respects: (1) the Clouds contain a class of populous open clusters that has no Galactic counterpart; (2) Cloud clusters have systematically larger radii rh than those in the Galaxy; (3) clusters of all ages in the Clouds are, on average, more flattened than those in the Galaxy. In the Large Magellanic Cloud (LMC) there appear to have been two distinct epochs of cluster formation. LMC globulars have ages of 12-15 Gyr, whereas most populous open clusters have ages <5 Gyr. No such dichotomy is observed for clusters in the Small Magellanic Cloud (SMC) The fact that the SMC exhibits no enhanced cluster formation at times of bursts of cluster formation in the LMC, militates against encounters between the Clouds as a cause for enhanced rates of star and cluster formation.


2018 ◽  
Vol 156 (3) ◽  
pp. 110 ◽  
Author(s):  
Chengyuan Li ◽  
Licai Deng ◽  
Kenji Bekki ◽  
Jongsuk Hong ◽  
Richard de Grijs ◽  
...  

2003 ◽  
Vol 125 (2) ◽  
pp. 754-769 ◽  
Author(s):  
Jong-Hak Woo ◽  
Carme Gallart ◽  
Pierre Demarque ◽  
Sukyoung Yi ◽  
Manuela Zoccali

2011 ◽  
Vol 414 (3) ◽  
pp. 2204-2214 ◽  
Author(s):  
Stefano Rubele ◽  
Léo Girardi ◽  
Vera Kozhurina-Platais ◽  
Paul Goudfrooij ◽  
Leandro Kerber

2011 ◽  
Vol 123 (903) ◽  
pp. 519-530 ◽  
Author(s):  
Andrés E. Piatti ◽  
Juan J. Clariá ◽  
María Celeste Parisi ◽  
Andrea V. Ahumada

1991 ◽  
pp. 191-192 ◽  
Author(s):  
Mario Mateo ◽  
Douglas Welch ◽  
Phil Fischer

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