Hostname: page-component-745bb68f8f-cphqk Total loading time: 0 Render date: 2025-01-25T21:13:47.304Z Has data issue: false hasContentIssue false
  • English
  • Français

Observations and Evolutionary Scenario For Be/X-Ray Binaries

Published online by Cambridge University Press:  23 September 2016

G.M.H.J. Habets
G.M.H.J. Habets*
Affiliation:
Sterrewacht ‘Sonnenborgh', Rijksuniversiteit Utrecht, Zonnenburg 2, 3512 NL Utrecht, The Netherlands

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.

Rappaport & Van den Heuvel (1982) suggested the following formation scenario for B emission (Be)/X-ray binaries: the progenitor of the neutron star is the initial primary star with mass M1 = 10-20 M⊙, which during hydrogen-shell burning transfers mass to the companion (with M2 < M1). The secondary is spun up due to disk-accretion (e.g. Packet 1981) and has become a rapidly rotating Be star (M ≃ 10-20 M⊙).

With this scenario the observed orbital periods (Porb > 15 d) of the Be/X-ray binaries can be explained. This was shown by van den Heuvel (1983) by adopting an idealized period distribution for unevolved O- and B-type close binaries with Porb, < 30 d (see Fig. 1) and assuming conservative evolution, i.e. that mass and angular momentum are conserved during mass transfer.

Type
V. Evolutionary Status of Be Stars
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 509 - 513
Copyright
Copyright © Cambridge University Press 1987

References

Doom, C. (1984). Astron. Astrophys., 138, 101.Google Scholar
Habets, G.M.H.J. (1986 a,b). Astron. Astrophys. (in press).Google Scholar
Hutchings, J.B., Crampton, D., Cowley, A.P., Olszweski, E., Thompson, I.B., & Suntzeff, N. (1985). Publ. Astron. Soc. Pacific, 97, 418.Google Scholar
Packet, W. (1981). Astron. Astrophysics., 102, 17.Google Scholar
Rappaport, S. & Van den Heuvel, E.P.J. (1982). In Be stars, eds. Jaschek, M. & H.-C. Groth, , IAU Symp. 98, 327. Google Scholar
Vanbeveren, D., De Grève, J.P., Van Dessel, E.L., & De Loore, C. (1979). Astron. Astrophys., 73, 19.Google Scholar
Van den Heuvel, E.P.J. (1983). In Accretion-driven Stellar X-ray Sources, eds. Lewin, W.H.G. & van den Heuvel, E.P.J, pp. 303–341. Cambridge: Cambridge Univ. Press.Google Scholar
Van den Heuvel, E.P.J. & Habets, G.M.H.J. (1984). Nature, 309, 598.Google Scholar