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Impact of accretion on the statistics of neutron star masses

Published online by Cambridge University Press:  21 February 2013

Z. Cheng ,
A. Taani  and
Y. H. Zhao
Z. Cheng*
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
A. Taani
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
Y. H. Zhao
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China
*
†email: chengzheng@bao.ac.cn
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Abstract

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We have collected the parameter of 38 neutron stars (NSs) in binary systems with spin periods and measured masses. By adopting the Boot-strap method, we reproduced the procedure of mass calculated for each system separately, to determine the truly mass distribution of the NS that obtained from observation. We also applied the Monte-Carlo simulation and introduce the characteristic spin period 20 ms, in order to distinguish between millisecond pulsars (MSPs) and less recycled pulsars. The mass distributions of MSPs and the less recycled pulsars could be fitted by a Gaussian function as 1.45±0.42 M⊙ and 1.31±0.17 M⊙ (with 1σ) respectively. As such, the MSP masses are heavier than those in less recycled systems by factor of ~ 0.13M⊙, since the accretion effect during the recycling process.

Keywords

Neutron starpulsarmassMonte-carlo simulation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S290: Feeding Compact Objects: Accretion on All Scales , August 2012 , pp. 195 - 196
Copyright
Copyright © International Astronomical Union 2013

References

Bhattacharya, D. & van den Heuvel, E. P. J. 1991, Phys. Rep, 203, 1Google Scholar
Haensel, P., Potekhin, A. Y., & Yakovlev, D. G. 2007, Neutron Stars 1. Equation of State and Structure (New York: Springer)Google Scholar
Kiziltan, A. K. & Thorsett, S. E. 2010, arXiv:1011.4291Google Scholar
Miller, C. 2002, Nature, 420, 31CrossRefGoogle Scholar
Ozel, F., Psaltis, D., Narayan, R., et al. 2012, ApJ, 757, 55CrossRefGoogle Scholar
Thorsett, S. E. & Chakrabarty, D. 1999, ApJ, 512, 288Google Scholar
Valentim, R., Rangel, E., & Horvath, J. E. 2011, MNRAS, 414, 1427CrossRefGoogle Scholar
Zhang, C. M., Wang, J., Zhao, Y. H., et al. 2011, A&A, 527, 83Google Scholar