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The superslow pulsation X-ray pulsars in high mass X-ray binaries

Published online by Cambridge University Press:  20 March 2013

Wei Wang*
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: [email protected]
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Abstract

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There exists a special class of X-ray pulsars that exhibit very slow pulsation of Pspin > 1000 s in the high mass X-ray binaries (HMXBs). We have studied the temporal and spectral properties of these superslow pulsation neutron star binaries in hard X-ray bands with INTEGRAL observations. Long-term monitoring observations find spin period evolution of two sources: spin-down trend for 4U 2206+54 (Pspin ~ 5560 s with spin ~ 4.9 × 10−7 s s−1) and long-term spin-up trend for 2S 0114+65 (Pspin ~ 9600 s with spin ~ −1 × 10−6 s s−1) in the last 20 years. A Be X-ray transient, SXP 1062 (Pspin ~ 1062 s), also showed a fast spin-down rate of spin ~ 3 × 10−6 s s−1 during an outburst. These superslow pulsation neutron stars cannot be produced in the standard X-ray binary evolution model unless the neutron star has a much stronger surface magnetic field (B > 1014 G). The physical origin of the superslow spin period is still unclear. The possible origin and evolution channels of the superslow pulsation X-ray pulsars are discussed. Superslow pulsation X-ray pulsars could be younger X-ray binary systems, still in the fast evolution phase preceding the final equilibrium state. Alternatively, they could be a new class of neutron star system – accreting magnetars.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013

References

Bhattacharya, D. & van den Heuvel, E. P. J. 1991, Phys. Rep., 203, 1Google Scholar
Crampton, D., Hutchings, J. B., & Cowley, A. P., 1985, ApJ, 299, 839Google Scholar
De Luca, A., et al. 2006, Science, 313, 814CrossRefGoogle Scholar
Farrell, S. A., et al. 2008, MNRAS, 389, 608Google Scholar
Finger, M. H., et al. 2010, ApJ, 709, 1249CrossRefGoogle Scholar
Haberl, F., et al. 2012, A&A, 537, L1Google Scholar
Henault-Brunet, V., et al.MNRAS, 420, L13CrossRefGoogle Scholar
Ikhsanov, N. R. 2007, MNRAS, 375, 698Google Scholar
Li, X. D. & van den Heuvel, E. P. J. 1999, ApJ, 513, L45Google Scholar
Mattana, F., et al. 2006, A&A, 460, L1Google Scholar
Reig, P., et al. 2009, A&A, 494, 1073Google Scholar
Shakura, N., et al. 2012, MNRAS, 420, 216Google Scholar
Walter, R., et al. 2006, A&A, 476, 133Google Scholar
Wang, W. 2009, MNRAS, 398, 1428Google Scholar
Wang, W. 2010, A&A, 520, 22Google Scholar
Wang, W. 2011, MNRAS, 413, 1083Google Scholar