The onset of gravothermal oscillations in globular cluster evolution

1994 ◽  
Vol 421 ◽  
pp. 195 ◽  
Author(s):  
Joseph L. Breeden ◽  
Haldan N. Cohn ◽  
Piet Hut
Keyword(s):  
Globular Cluster ◽  
Cluster Evolution

Primordial binaries and globular cluster evolution

Nature ◽  
1989 ◽  
Vol 339 (6219) ◽  
pp. 40-42 ◽  
Author(s):  
Jeremy Goodman ◽  
Piet Hut
Keyword(s):  
Globular Cluster ◽  
Cluster Evolution

Globular cluster evolution in the Galaxy - A global view

1987 ◽  
Vol 322 ◽  
pp. 113 ◽  
Author(s):  
David F. Chernoff ◽  
Stuart L. Shapiro
Keyword(s):  
Globular Cluster ◽  
Cluster Evolution ◽  
Global View ◽  
The Galaxy

Fokker-Planck models and globular cluster evolution - The problem of M71

1992 ◽  
Vol 386 ◽  
pp. 106 ◽  
Author(s):  
G. A. Drukier ◽  
G. G. Fahlman ◽  
H. B. Richer
Keyword(s):  
Globular Cluster ◽  
Cluster Evolution ◽  
Fokker Planck

scholarly journals The Binary Fraction of NGC 6397

2007 ◽  
Vol 3 (S246) ◽  
pp. 263-264
Author(s):  
D. Saul Davis ◽  
Harvey B. Richer ◽  
Jay Anderson ◽  
James Brewer
Keyword(s):  
Globular Cluster ◽  
Main Sequence ◽  
Cataclysmic Variables ◽  
Dynamical Evolution ◽  
Computing Power ◽  
Blue Stragglers ◽  
The Core ◽  
Cluster Evolution ◽  
Key Parameter

AbstractThe binary fraction, η, of a globular cluster (GC) is a key parameter in determining its dynamical evolution, as well as its content of rare stars, such as cataclysmic variables and blue stragglers. The precise value of η for a GC was historically difficult to constrain due to an inability to obtain reliable photometry for faint objects in dense stellar fields. However, today, the HST allows us to image the main sequence of the nearest GCs to their terminations. Using HST observations we constrain η for NGC 6397. While the necessary computing power is now available to realistically simulate entire GCs, large discrepancies in the assumed primordial binary fraction, ηp, of GCs still exist. Estimates range from 5% (Hurley et al. 2007) to 100% (Ivanova et al. 2005). The N-body models of Hurley et al. (2007) suggest that η beyond the half-mass radius remains close to ηp, while cluster evolution can increase the value in the core. We find η for NGC 6397 is 15.2±0.8% in a field centered on the core, and 1.1±0.3% in a field beyond the half mass radius. These findings suggests ηp ~ 1%.

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