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Seven pulsars in binary systems above the spin-up line

Published online by Cambridge University Press:  20 March 2013

Y. Y. Pan  and
N. Wang
Y. Y. Pan
Affiliation:
Xinjiang Astronomical Observatories, Chinese Academy of Sciences, Xinjiang 830011, China email: panyuanyue@xao.ac.cn
N. Wang
Affiliation:
Xinjiang Astronomical Observatories, Chinese Academy of Sciences, Xinjiang 830011, China email: panyuanyue@xao.ac.cn
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Abstract

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Using data from the ATNF pulsar catalogue, 186 binary pulsars are shown in the magnetic field versus spin period (B-P) diagram, and their relationship to the spin-up line is investigated. Generally speaking, pulsars in binary systems should be below the spin-up line when they get enough accretion mass from their companions. It is found that there are seven binary pulsars above the spin-up line. Based on the parameters of these seven binary systems, we describe possible reasons why they are above the spin-up line.

Keywords

Pulsarbinaryspin-up line
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S291: Neutron Stars and Pulsars: Challenges and Opportunities after 80 years , August 2012 , pp. 462 - 464
Copyright
Copyright © International Astronomical Union 2013

References

Alpar, M. A., Cheng, A. F., Ruderman, M. A., & Shaham, J., 1982, Nature, 300, 728CrossRefGoogle Scholar
Bhattacharya, D. & van den Heuvel, E. P. J. 1991, Phys. Rep., 203, 1Google Scholar
Camilo, F., Thorsett, S. E., & Kulkarni, S. R., 1994, ApJ, 421, L15Google Scholar
Lyne, A. G., Burgay, M. Kramer, M. et al., 2004, Science, 303, 1153.CrossRefGoogle Scholar
Manchester, R. N., 2004, Science, 304, 542Google 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, 561CrossRefGoogle Scholar
van den Heuvel, E. P. J., 2004, Science, 303, 20Google 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, 344Google Scholar
Zhang, C. M., Kojima, Y., 2006, MNRAS, 336, 137Google Scholar
Zhang, C. M., Wang, J., Zhao, Y. H.et al., 2011, A&A, 527, 83Google Scholar