scholarly journals The Clusters Ages Experiment (CASE). I. V209 ω Cen: An Eclipsing Post-Common-Envelope Binary in the Globular Cluster ω Cen

2007 ◽  
Vol 133 (6) ◽  
pp. 2457-2463 ◽  
Author(s):  
J. Kaluzny ◽  
S. M. Rucinski ◽  
I. B. Thompson ◽  
W. Pych ◽  
W. Krzeminski
Keyword(s):  
Globular Cluster ◽  
Common Envelope

scholarly journals Are most Cataclysmic Variables in Globular Clusters dynamically formed?

2019 ◽  
Vol 14 (S351) ◽  
pp. 404-407
Author(s):  
Diogo Belloni ◽  
Mirek Giersz ◽  
Liliana E. Rivera Sandoval ◽  
Abbas Askar ◽  
Pawel Ciecielag
Keyword(s):  
Globular Cluster ◽  
Globular Clusters ◽  
Cataclysmic Variables ◽  
Common Envelope ◽  
Long Time

AbstractWe have been investigating populations of cataclysmic variables (CVs) in a set of more than 300 globular cluster (GC) models evolved with themoccacode.[-120pt] One of the main questions we have intended to answer is whether most CVs in GCs are dynamically formed or not. Contrary to what has been argued for a long time, we found that dynamical destruction of primordial CV progenitors is much stronger in GCs than dynamical formation of CVs. In particular, we found that, on average, the detectable CV population is predominantly composed of CVs formed via a typical common envelope phase (≳70 per cent). However, core-collapsed models tend to have higher fractions of bright CVs than non-core-collapsed ones, which suggests then that the formation of CVs is indeed slightly favoured through strong dynamical interactions in core-collapsed GCs, due to the high stellar densities in their cores.

Recent Advances in High Dispersion Spectroscopy of Globular Cluster Stars

1988 ◽  
Vol 132 ◽  
pp. 525-530
Author(s):  
Raffaele G. Gratton
Keyword(s):  
Globular Cluster ◽  
Globular Clusters ◽  
High Dispersion ◽  
Photographic Material ◽  
Recent Advances ◽  
Metal Abundances ◽  
Ccd Detectors ◽  
Major Progress

The use CCD detectors has allowed a major progress in abundance derivations for globular cluster stars in the last years. Abundances deduced from high dispersion spectra now correlates well with other abundance indicators. I discuss some problems concerning the derivation of accurate metal abundances for globular clusters using high dispersion spectra from both the old photographic and the most recent CCD data. The discrepant low abundances found by Cohen (1980), from photographic material for M71 giants, are found to be due to the use of too high microturbulences.

Galactic orbits of stars

1966 ◽  
Vol 25 ◽  
pp. 93-97
Author(s):  
Richard Woolley
Keyword(s):  
Globular Cluster ◽  
Potential Field ◽  
High Velocity ◽  
Velocity Vector ◽  
Variable Stars ◽  
The Sun ◽  
Proper Motions ◽  
Rr Lyrae ◽  
The Galaxy

It is now possible to determine proper motions of high-velocity objects in such a way as to obtain with some accuracy the velocity vector relevant to the Sun. If a potential field of the Galaxy is assumed, one can compute an actual orbit. A determination of the velocity of the globular clusterωCentauri has recently been completed at Greenwich, and it is found that the orbit is strongly retrograde in the Galaxy. Similar calculations may be made, though with less certainty, in the case of RR Lyrae variable stars.

A Distance-Independent Age for the Globular Cluster M92

2000 ◽  
Vol 120 (4) ◽  
pp. 1884-1891 ◽  
Author(s):  
F. Grundahl, ◽  
D. A. VandenBerg, ◽  
R. A. Bell, ◽  
M. I. Andersen, ◽  
P. B. Stetson
Keyword(s):  
Globular Cluster

Elemental Abundances in Five Stars in M54, A Globular Cluster Associated with the Sagittarius Galaxy

1999 ◽  
Vol 118 (3) ◽  
pp. 1245-1251 ◽  
Author(s):  
Jeffery A. Brown ◽  
George Wallerstein ◽  
Guillermo Gonzalez
Keyword(s):  
Globular Cluster ◽  
Elemental Abundances

Proton Capture Chains in Globular Cluster Stars. III. Abundances of Giants in the Second-Parameter Globular Cluster NGC 7006

1998 ◽  
Vol 115 (4) ◽  
pp. 1500-1515 ◽  
Author(s):  
Robert P. Kraft ◽  
Christopher Sneden ◽  
Graeme H. Smith ◽  
Matthew D. Shetrone ◽  
Jon Fulbright
Keyword(s):  
Globular Cluster ◽  
Proton Capture

The Globular Cluster System in the Inner Region of M87

1999 ◽  
Vol 513 (2) ◽  
pp. 733-751 ◽  
Author(s):  
Arunav Kundu ◽  
Bradley C. Whitmore ◽  
William B. Sparks ◽  
F. Duccio Macchetto ◽  
Stephen E. Zepf ◽  
...  
Keyword(s):  
Globular Cluster ◽  
Cluster System ◽  
Globular Cluster System ◽  
Inner Region

scholarly journals The globular cluster system of the Auriga simulations

2020 ◽  
Vol 496 (1) ◽  
pp. 638-648 ◽  
Author(s):  
Timo L R Halbesma ◽  
Robert J J Grand ◽  
Facundo A Gómez ◽  
Federico Marinacci ◽  
Rüdiger Pakmor ◽  
...  
Keyword(s):  
Globular Cluster ◽  
Milky Way ◽  
Cluster Formation ◽  
Solar Radius ◽  
High Mass ◽  
Formation Model ◽  
The Galaxy ◽  
High Mass Loss ◽  
Globular Cluster System ◽  
Varying Mass

ABSTRACT We investigate whether the galaxy and star formation model used for the Auriga simulations can produce a realistic globular cluster (GC) population. We compare statistics of GC candidate star particles in the Auriga haloes with catalogues of the Milky Way (MW) and Andromeda (M31) GC populations. We find that the Auriga simulations do produce sufficient stellar mass for GC candidates at radii and metallicities that are typical for the MW GC system (GCS). We also find varying mass ratios of the simulated GC candidates relative to the observed mass in the MW and M31 GCSs for different bins of galactocentric radius metallicity (rgal–[Fe/H]). Overall, the Auriga simulations produce GC candidates with higher metallicities than the MW and M31 GCS and they are found at larger radii than observed. The Auriga simulations would require bound cluster formation efficiencies higher than 10 per cent for the metal-poor GC candidates, and those within the Solar radius should experience negligible destruction rates to be consistent with observations. GC candidates in the outer halo, on the other hand, should either have low formation efficiencies, or experience high mass-loss for the Auriga simulations to produce a GCS that is consistent with that of the MW or M31. Finally, the scatter in the metallicity as well as in the radial distribution between different Auriga runs is considerably smaller than the differences between that of the MW and M31 GCSs. The Auriga model is unlikely to give rise to a GCS that can be consistent with both galaxies.

scholarly journals A supra-massive population of stellar-mass black holes in the globular cluster Palomar 5

2021 ◽  
Author(s):  
Mark Gieles ◽  
Denis Erkal ◽  
Fabio Antonini ◽  
Eduardo Balbinot ◽  
Jorge Peñarrubia
Keyword(s):  
Black Holes ◽  
Globular Cluster ◽  
Stellar Mass
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