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Mass-Loss Timescale of Star Cluster in External Tidal Field

Published online by Cambridge University Press:  01 September 2007

T. Fukushige  and
A. Tanikawa
T. Fukushige
Affiliation:
K&F Computing Research Co. email: [email protected]
A. Tanikawa
Affiliation:
Department of General System Studies, College of Arts and Sciences, University of Tokyo email: [email protected]
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Abstract

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We investigate evolution of star clusters in steady external tidal field by means of N-body simulations. We followed several sets of cluster models whose strength and Coriolis's contribution of the external tidal field are different. We found that the mass loss timescale due to the escape of stars, t_mloss, and its dependence on the two-body relaxation timescale, trh,i, are determined by the strength of the tidal field. The logarithmic slope [≡ dln(tmloss)/dln(trh,i)] approaches unity for the cluster models in weaker tidal fields. We also found that stronger Coriolis force against others, produced by parent galaxy whose density profile is shallower, makes the mass loss timescale longer. This is due to the fact that a fraction of stars whose orbit are nearly regular increases as the Coriolis force becomes stronger.

Keywords

globular clusters: generalmethod: n-body simulations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S246: Dynamical Evolution of Dense Stellar Systems , September 2007 , pp. 191 - 192
Copyright
Copyright © International Astronomical Union 2008

References

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Tanikawa, A. & Fukushige, T. 2005, PASJ 57, 155CrossRefGoogle Scholar