Hostname: page-component-745bb68f8f-hvd4g Total loading time: 0 Render date: 2025-01-13T00:37:31.682Z Has data issue: false hasContentIssue false
  • English
  • Français

Escape Velocities from Unstable Triple Stars

Published online by Cambridge University Press:  25 May 2016

J. Anosova ,
K. Tanikawa ,
J. Colin ,
L. Kiseleva  and
P. Eggleton
J. Anosova
Affiliation:
National Astronomical Observatory, Tokyo 181, Japan
K. Tanikawa
Affiliation:
National Astronomical Observatory, Tokyo 181, Japan
J. Colin
Affiliation:
Observatoire de Bordeaux, Floirac, France
L. Kiseleva
Affiliation:
Institute of Astronomy, Cambridge CB3 0HA, UK
P. Eggleton
Affiliation:
Institute of Astronomy, Cambridge CB3 0HA, UK

Extract

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.

In order to investigate a possible origin for stars with high peculiar velocities in the thick disc of our Galaxy, the dynamical evolution of 16 000 three-dimensional triple systems which consist of a binary with equal or comparable masses of components M 1 and M 2 and a low-mass third body M 3 is considered. We examine an extensive range of initial conditions with positions of the body M 3 randomly distributed around and inside the binary orbit. M 3 was given the initial radial velocity V 0 with respect to the center of inertia of the binary. The following dynamical system of units is used in this work: the unit of distance is the semi-major axis of the binary orbit, the unit of time is the period of the binary; the universal constant of gravity is unity. In these units the total mass of the close binary is 4π2.

Type
Chapter 6: How are we to Understand the Large Scale Structure of the ISM?
Information
Symposium - International Astronomical Union , Volume 169: Unsolved Problems of the Milky Way , 1996 , pp. 527 - 528
Copyright
Copyright © Kluwer 1996 

References

Kiseleva, L., Anosova, J., Colin, J. IAU 164 Proceedings, 1994,in press.Google Scholar