Hostname: page-component-745bb68f8f-lrblm Total loading time: 0 Render date: 2025-01-12T21:03:24.521Z Has data issue: false hasContentIssue false
  • English
  • Français

Spin Evolution of the Progenitors of Binary and Millisecond Pulsars

Published online by Cambridge University Press:  25 May 2016

Pranab Ghosh
Pranab Ghosh*
Affiliation:
Tata Institute of Fundamental Research, Bombay 400 005, India

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 this symposium, I have been given the task of summarizing our current understanding of the evolutionary history of spin periods of the neutron stars that we now see as binary and millisecond pulsars, i.e., recycled pulsars. We believe that a newborn, fast-spinning neutron star (with a rather high magnetic field ∼1011–1013 G) in a binary system first operates as a spin-powered pulsar, subsequently as an accretion-powered pulsar when accretion begins after the pulsar has been spun down adequately, and finally as a spin-powered pulsar for the second time after having been recycled to become a very fast-rotating neutron star (with a rather low magnetic field ∼108–1011 G) (see Ghosh 1994a, b, hereafter G94a, b).

Type
1 Binary Evolution
Information
Symposium - International Astronomical Union , Volume 165: Compact Stars in Binaries , 1996 , pp. 57 - 64
Copyright
Copyright © Kluwer 1996 

References

Bhattacharya, D. & Van den Heuvel, E.P.J. 1991, Phys. Rep. 203, 1.CrossRefGoogle Scholar
Bjorkman, J.E. & Cassinelli, J.P. 1993, ApJ 409, 429 (BC).Google Scholar
De Kool, M. & Van Paradijs, J. 1987, A&A 173, 279.Google Scholar
Ghosh, P. 1994a, in The Evolution of X-ray Binaries , Holt, S.S. & Day, C.S. (Eds.), AIP Conf. Proc. Vol. 308, p. 439 (G94a).CrossRefGoogle Scholar
Ghosh, P. 1994b, in Pulsars: Festschrift for V. Radhakrishnan , Srinivasan, G. (Ed.), Indian Academy of Sciences (Bangalore), (in press) (G94b).Google Scholar
Ghosh, P. 1994c, ApJ (submitted) (G94c).Google Scholar
Grove, E. et al. 1994, ApJ (submitted).Google Scholar
Henrichs, H. 1983, in Accretion-Driven Stellar X-ray Sources , Lewin, W.H.G. & van den Heuvel, E.P.J. (Eds.), Cambridge Univ. Press, p. 393.Google Scholar
Illarionov, A.F. & Sunyaev, R.A. 1975, A&A 39, 185 (IS).Google Scholar
Johnston, S. et al. 1994a, MNRAS 268, 430 (J94a).Google Scholar
Johnston, S. 1994b, these Proceedings (J94b).Google Scholar
Joss, P.C., Rappaport, S. & Lewis, W. 1987, ApJ 319, 180.CrossRefGoogle Scholar
Kaspi, V.M. et al. 1994, ApJ 423, L43.Google Scholar
Kochanek, C. 1993, ApJ 406, 638.Google Scholar
Kulkarni, S.R. 1992, Phil. Trans. Roy. Soc. London A341, 77.Google Scholar
Mineshige, S., Rees, M.J. & Fabian, A.C. 1991, MNRAS 251, 555.CrossRefGoogle Scholar
Nagase, F. 1992, in Proc. Ginga Memorial Symposium , Makino, F. & Nagase, F. (Eds.), ISAS, p. 1.Google Scholar
Pylyser, E. & Savonije, G.J 1988, A&A 191, 57.Google Scholar
Van den Heuvel, E.P.J. 1992, in X-ray Binaries & Recycled Pulsars , van den Heuvel, E.P.J. & Rappaport, S. (Eds.), Kluwer Academic Publishers, p. 233 (vdH92).Google Scholar
Van den Heuvel, E.P.J. 1994, A&A (submitted).Google Scholar
Verbunt, F. 1994, in The Evolution of X-ray Binaries , Holt, S.S. & Day, C.S. (Eds.), AIP Conf. Proc. Vol. 308, p. 351.Google Scholar
Waters, L.B.F.M. 1986, A&A 162, 121 (W).Google Scholar
Webbink, R.F. 1992, in X-ray Binaries & Recycled Pulsars , van den Heuvel, E.P.J. & Rappaport, S. (Eds.), Kluwer Academic Publishers, p. 269.Google Scholar