Formation of Thorne–Żytkow objects in close binaries

  • Bumareyamu Hutilukejiang
  • Chunhua Zhu
  • Zhaojun Wang
  • Guoliang Lü
Article
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Abstract

Thorne–Żytkow objects (TŻOs), originally proposed by Thorne and Żytkow, may form as a result of unstable mass transfer in a massive X-ray binary after a neutron star (NS) is engulfed in the envelope of its companion star. Using a rapid binary evolution program and the Monte Carlo method, we simulated the formation of TŻOs in close binary stars. The Galactic birth rate of TŻOs is about \(1.5\times 10^{-4}~\hbox {yr}^{-1}\). Their progenitors may be composed of a NS and a main-sequence star, a star in the Hertzsprung gap or a core-helium burning, or a naked helium star. The birth rates of TŻOs via the above different progenitors are \(1.7\times 10^{-5}\), \(1.2\times 10^{-4}\), \(0.7\times 10^{-5}\), \(0.6\times 10^{-5}~\hbox {yr}^{-1}\), respectively. These progenitors may be massive X-ray binaries. We found that the observational properties of three massive X-ray binaries (SMC X-1, Cen X-3 and LMC X-4) in which the companions of NSs may fill their Roche robes were consistent with those of their progenitors.

Keywords

Binary: close star: neutron X-ray: star. 
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Notes

Acknowledgements

This work was supported by XinJiang Science Fund for Distinguished Young Scholars under No. 2014721015, the National Natural Science Foundation of China under Nos. 11473024, 11363005, 11763007 and 11503008.

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Copyright information

© Indian Academy of Sciences 2018

Authors and Affiliations

  • Bumareyamu Hutilukejiang
    • 1
  • Chunhua Zhu
    • 1
  • Zhaojun Wang
    • 1
  • Guoliang Lü
    • 1
  1. 1.School of Physical Science and TechnologyXinjiang UniversityÜrümqiChina

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