Hostname: page-component-cd9895bd7-gxg78 Total loading time: 0 Render date: 2024-12-25T17:11:49.291Z Has data issue: false hasContentIssue false
  • English
  • Français

The Formation and Evolution of Black-Hole Binaries

Published online by Cambridge University Press:  25 May 2016

Roger W. Romani
Roger W. Romani*
Affiliation:
Department of Physics, Stanford University, Stanford, CA 94305-4060, U.S.A.

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.

The presence of accreting black holes (BH) among the X-ray binaries has been recognized for many years. Traditionally, Cyg X-1 and the handful of other candidates have been thought of as cousins of the HMXB neutron star systems. Recent studies of the soft X-ray transients such as A 0620-00 have, however, shown that the dynamical evidence makes these low-mass systems very strong black-hole candidates. Further, analysis of the eventual end-states of various high-mass X-ray binaries suggest that some could end as observable BH-pulsar binaries, although the first such system is yet to be discovered.

Type
1 Binary Evolution
Information
Symposium - International Astronomical Union , Volume 165: Compact Stars in Binaries , 1996 , pp. 93 - 103
Copyright
Copyright © Kluwer 1996 

References

Brown, G.E., Bruenn, S.W. & Wheeler, J.C. 1992, Com. Astrophys. 13, 153.Google Scholar
Chevalier, R.A. 1989, ApJ 346, 847.Google Scholar
Chevalier, R.A. 1993, ApJ 411, L33.Google Scholar
Cowley, A.P., Crampton, D. & Hutchings, J.B. 1983, ApJ 272, 118.Google Scholar
De Kool, M., Van den Heuvel, E.P.J. & Pylyser, E. 1987, A&A 183, 47.Google Scholar
Eggleton, P.P. & Verbunt, F. 1986, MNRAS 220, 13.Google Scholar
Lipunov, V.M. et al. 1994, ApJ 423, L121.CrossRefGoogle Scholar
Lyne, A.G. & Lorimer, D.R. 1994, Nat 369, 127.Google Scholar
Mineshige, S., Kim, S. & Wheeler, J.C. 1990, ApJ 358, L5.CrossRefGoogle Scholar
Nomoto, K. & Kondo, Y. 1991, ApJ 367, L19.CrossRefGoogle Scholar
Narayan, R., Piran, T. & Shemi, A. 1991, ApJ 379, L17.CrossRefGoogle Scholar
Podsiadlowski, P., Joss, P.C. & Hsu, J.J.L. 1992, ApJ 391, 246.CrossRefGoogle Scholar
Romani, R.W. 1992, ApJ 399, 621.Google Scholar
Romani, R.W. 1994, in Interacting Binary Stars , Shafter, A.E. (Ed.), ASP Conf. Proc. Vol. 56, p. 196.Google Scholar
Savonije, G.J. 1983, in Accretion Driven Stellar X-ray Sources , Lewin, W.H.G. & van den Heuvel, E.P.J. (Eds.), Cambridge Univ. Press, p. 434.Google Scholar
Tutukov, A.V. & Yungel'son, L.R. 1993, Ast. Rep. 37, 411.Google Scholar
Van den Heuvel, E.P.J. 1993, in Space Sciences with particular emphasis on High Energy Astrophysics , (ESA: ESTEC Noordwijk).Google Scholar
Van den Heuvel, E.P.J. & Habets, G.M.H.J. 1984, Nat 309, 689.Google Scholar
Webbink, R.F. 1992, in X-ray Binaries and Recycled Pulsars , van den Heuvel, E.P.J. & Rappaport, S.A. (Eds.), Kluwer Academic Publishers, p. 269.CrossRefGoogle Scholar
Wheeler, J.C. & Shields, G.A. 1976, Nat 259, 642.Google Scholar
Whitehurst, R. 1988, MNRAS 232, 35.Google Scholar
Woosley, S.E., Langer, N. & Weaver, T.A. 1993, ApJ 411, 823.Google Scholar
Yamaoka, H., Shigeyama, T. & Nomoto, K. 1993, A&A 267, 433.Google Scholar