Hostname: page-component-78c5997874-94fs2 Total loading time: 0 Render date: 2024-11-10T22:19:22.484Z Has data issue: false hasContentIssue false
  • English
  • Français

On the Efficiency of Field Star Capture by Star Clusters

Published online by Cambridge University Press:  01 September 2007

S. Mieske  and
H. Baumgardt
S. Mieske
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Str.2, 85748 Garching b. München, Germany email: smieske@eso.org, mhilker@eso.org
H. Baumgardt
Affiliation:
Argelander Institut für Astronomie, Auf dem Hügel 71, 53121 Bonn, Germany email: holger@astro.uni-bonn.de
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

An exciting recent finding regarding scaling relations among globular clusters is the so-called ‘blue tilt’: clusters of the blue sub-population follow a trend of redder colour with increasing luminosity. In this contribution we estimate by means of collisional N-body simulations to which extent this trend can be explained by field star capture occurring over a Hubble time. We investigate star clusters with 103 to 106 stars. We find that the ratio between captured field stars and total number of clusters stars is very low (≲ 10−4), even for co-rotation of the star cluster in a cold disk. This holds for star clusters in the mass range of both open clusters and globular clusters. Therefore, field star capture is not a probable mechanism for creating the colour-magnitude trend of metal-poor globular clusters.

Keywords

globular clusters: generalopen clusters and associations: generalstars: kinematicsgalaxies: kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S246: Dynamical Evolution of Dense Stellar Systems , September 2007 , pp. 195 - 196
Copyright
Copyright © International Astronomical Union 2008

References

Bekki, K., Yahagi, H., & Forbes, D. A. 2007, MNRAS, 377, 215Google Scholar
Cantiello, M., Blakeslee, J. P., & Raimondo, G. 2007, astro-ph/0706.3943Google Scholar
Harris, W. E. et al. 2006, ApJ, 636, 90Google Scholar
Mieske, S. et al. 2006, ApJ, 653, 193CrossRefGoogle Scholar
Mieske, S. & Baumgardt, H. 2007, A&A in press, arXiv:0709.1328Google Scholar
Spitler, L. R. et al. 2006, AJ, 132, 1593CrossRefGoogle Scholar
Strader, J., Brodie, J. P., Spitler, L., & Beasley, M. A. 2006, AJ, 132, 2333CrossRefGoogle Scholar