Hostname: page-component-77c89778f8-swr86 Total loading time: 0 Render date: 2024-07-21T02:26:33.746Z Has data issue: false hasContentIssue false
  • English
  • Français

Binary-Single Encounters of 10 M⊙ Black Holes Including the Effects of Gravitational Radiation

Published online by Cambridge University Press:  25 May 2016

K. N. Kong  and
H. M. Lee
K. N. Kong
Affiliation:
Pusan University Department of Earth Sciences, Pusan 609-735, Korea
H. M. Lee
Affiliation:
Pusan University Department of Earth Sciences, Pusan 609-735, Korea

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.

We compute the outcomes of close encounters between a binary and a single black holes including the effects of gravitational radiation reaction. All masses of individual black holes are assumed to be 1 M⊙. We found that merger of two black holes takes place during the encounters in some cases. Thus the gravitational radiation can act as a mechanism for the dissipation of energy of a cluster mainly composed of 10 M⊙ black holes which are produced by the evolution of high mass stars. The merger probability depends on many parameters in a complex way. Our preliminary calculations show that about 10% of the strong encounters (i.e., rp ∼ a) between a binary of hardness 100 and a single lead to mergers of two black holes in the stellar system of one-dimensional velocity σ = 100 km/s.

Type
Stellar Evolution in Star Clusters
Information
Symposium - International Astronomical Union , Volume 174: Dynamical Evolution of Stars Clusters , 1996 , pp. 351 - 352
Copyright
Copyright © Kluwer 1996 

References

Aarseth, S. J., & Zare, K., 1974, Celestial Mechanics, 10, 185.CrossRefGoogle Scholar
Brown, G. E & Bethe, H. A., 1994, ApJ, 423, 659.CrossRefGoogle Scholar
Damour, T., 1987, in Three Hundred Years of Gravitation, ed. Hawking, S. & Israel, W. (Cambridge: Cambridge University Press), 128.Google Scholar
Lee, H. M., 1995, MNRAS, 272, 605.Google Scholar
Peters, P. C., 1964, Phys. Rev., 136, B1224.Google Scholar