Hostname: page-component-78c5997874-4rdpn Total loading time: 0 Render date: 2024-11-10T23:08:12.228Z Has data issue: false hasContentIssue false
  • English
  • Français

Minimum accretion rate for millisecond pulsar formation in binary system

Published online by Cambridge University Press:  21 February 2013

Yuanyue Pan ,
Chengmin Zhang  and
Na Wang
Yuanyue Pan
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China Email: panyuanyue@xao.ac.cn Xinjiang Astronomical Observatories, Chinese Academy of Sciences, Xinjiang 830011, China
Chengmin Zhang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China Email: panyuanyue@xao.ac.cn
Na Wang
Affiliation:
Xinjiang Astronomical Observatories, Chinese Academy of Sciences, Xinjiang 830011, 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.

186 binary pulsars are shown in the magnetic field versus spin period (B-P) diagram, and their relations to the millisecond pulsars can be clearly seen. We declaim a minimum accretion rate for the millisecond pulsar formation both from the observation and theory. If the accretion rate is lower than the minimum accretion rate, the pulsar in binary system will not become a millisecond pulsar after the evolution.

Keywords

Binary systemmillisecond pulsaraccretion rate
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S290: Feeding Compact Objects: Accretion on All Scales , August 2012 , pp. 291 - 292
Copyright
Copyright © International Astronomical Union 2013

References

Bhattacharya, D. & van den Heuvel, E. P. J. 1991, Phys. Rep., 203, 1CrossRefGoogle Scholar
Lyne, A. G., Burgay, M., Kramer, M.et al. 2004, Science, 303, 1153Google Scholar
Manchester, R. N., Hobbs, G. B., Teoh, A., & Hobbs, M. 2005, AJ, 129, 1993CrossRefGoogle Scholar
Stairs, I. H. 2004, Science, 304, 23Google Scholar
Tauris, M. 2012, Science, 335, 561Google Scholar
van den Heuvel, E. P. J. 2004, Science, 303, 20CrossRefGoogle Scholar
Wang, J., Zhang, C. M., Zhao, Y. H.et al. 2011, A&A, 526, 88Google Scholar
Wijnands, R. & van der Klis, M. 1998, Nature, 394, 344CrossRefGoogle Scholar
Zhang, C. M. & Kojima, Y. 2006, MNRAS, 336, 137CrossRefGoogle Scholar
Zhang, C. M., Wang, J., Zhao, Y. H.et al. 2011, A&A, 527, 83Google Scholar