Hostname: page-component-848d4c4894-ndmmz Total loading time: 0 Render date: 2024-05-14T01:22:50.352Z Has data issue: false hasContentIssue false
  • English
  • Français

ONe WD+He star systems as the progenitors of IMBPs

Published online by Cambridge University Press:  30 December 2019

Bo Wang  and
Dongdong Liu
Bo Wang
Affiliation:
Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China email: wangbo@ynao.ac.cn Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, China
Dongdong Liu
Affiliation:
Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China email: wangbo@ynao.ac.cn Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, China
Rights & Permissions [Opens in a new window]

Abstract

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.

Previous theoretical studies can only explain part of the observed intermediate-mass binary pulsars (IMBPs) with short orbital periods. Note that an ONe white dwarf (WD) accreting mass from a He star may experience the accretion-induced collapse process and eventually form IMBPs, known as the ONe WD+He star scenario. By investigating the evolution of a large number of ONe WD+He star binaries, we found that the ONe WD+He star scenario can form IMBPs including pulsars with 5 – 340 ms spin periods, and the orbital periods range from 0.04 to 900 d. Compared with the observed IMBPs, this scenario can cover almost all of the IMBPs with short orbital periods. Thus, we suggest that the ONe WD+He star channel is responsible for the formation of IMBPs with short orbital periods.

Keywords

binaries: closestars: evolutionwhite dwarfsstars: neutron
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 478 - 479
Copyright
© International Astronomical Union 2019 

References

Camilo, F., Nice, D. J., Shrauner, J. A., & Taylor, J. H., 1996, ApJ, 469, 819 CrossRefGoogle Scholar
Camilo, F. et al. 2001, ApJ, 548, L187 CrossRefGoogle Scholar
Chen, W. C., & Liu, W. M. 2013, MNRAS, 432, L75 CrossRefGoogle Scholar
Corbet, R. H. D. 1984, A&A, 141, 91 Google Scholar
Edwards, R. T., & Bailes, M. 2001, ApJ, 547, L37 CrossRefGoogle Scholar
Eggleton, P. P. 1973, MNRAS, 163, 279 CrossRefGoogle Scholar
Liu, D., Wang, B., Chen, W., Zuo, Z., & Han, Z. 2018, MNRAS, 477, 384 CrossRefGoogle Scholar
Manchester, R. N., Hobbs, G. B., Teoh, A., & Hobbs, M. 2005, AJ, 129, 1993 CrossRefGoogle Scholar
Tauris, T. M., Sanyal, D., Yoon, S. C., & Langer, N. 2013, A&A, 558, A39 Google Scholar
Tauris, T. M., van den Heuvel, E. P. J., & Savonije, G. J. 2000, ApJ, 530, L93 CrossRefGoogle Scholar
van den Heuvel, E. P. J. 1975, ApJ, 198, L109 CrossRefGoogle Scholar