Erosion of globular cluster systems: the influence of radial anisotropy, central black holes and dynamical friction

Brockamp, M., Kupper, A. H. W., Thies, I., Baumgardt, H. and Kroupa, P. (2014) Erosion of globular cluster systems: the influence of radial anisotropy, central black holes and dynamical friction. Monthly Notices of the Royal Astronomical Society, 441 1: 150-171. doi:10.1093/mnras/stu562


Author Brockamp, M.
Kupper, A. H. W.
Thies, I.
Baumgardt, H.
Kroupa, P.
Title Erosion of globular cluster systems: the influence of radial anisotropy, central black holes and dynamical friction
Journal name Monthly Notices of the Royal Astronomical Society   Check publisher's open access policy
ISSN 1365-2966
0035-8711
Publication date 2014-06-11
Year available 2014
Sub-type Article (original research)
DOI 10.1093/mnras/stu562
Open Access Status DOI
Volume 441
Issue 1
Start page 150
End page 171
Total pages 22
Place of publication Oxford, United Kingdom
Publisher Oxford University Press
Language eng
Formatted abstract
We present the adaptable MUESLI code for investigating dynamics and erosion processes of globular clusters (GCs) in galaxies. MUESLI follows the orbits of individual clusters and applies internal and external dissolution processes to them. Orbit integration is based on the self-consistent field method in combination with a time-transformed leapfrog scheme, allowing us to handle velocity-dependent forces like triaxial dynamical friction. In a first application, the erosion of GC systems (GCSs) in elliptical galaxies is investigated. Observations show that massive ellipticals have rich, radially extended GCSs, while some compact dwarf ellipticals contain no GCs at all. For several representative examples, spanning the full mass scale of observed elliptical galaxies, we quantify the influence of radial anisotropy, galactic density profiles, supermassive black holes and dynamical friction on the GC erosion rate. We find that GC number density profiles are centrally flattened in less than a Hubble time, naturally explaining observed cored GC distributions. The erosion rate depends primarily on a galaxy's mass, half-mass radius and radial anisotropy. The fraction of eroded GCs is nearly 100 per cent in compact, M32-like galaxies and lowest in extended and massive galaxies. Finally, we uncover the existence of a violent tidal-disruption-dominated phase which is important for the rapid build-up of halo stars.
Keyword Methods: numerical
Galaxies: elliptical and lenticular, cD
Galaxies: nuclei
Galaxies: star clusters: general
Q-Index Code C1
Q-Index Status Confirmed Code
Institutional Status UQ

Document type: Journal Article
Sub-type: Article (original research)
Collections: School of Mathematics and Physics
Official 2015 Collection
 
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Citation counts: TR Web of Science Citation Count  Cited 19 times in Thomson Reuters Web of Science Article | Citations
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