Exploration of Spin-down Rate of Neutron Star in High Mass X-ray Binaries

We use the evolutionary population synthesis method to investigate the statistical properties of the wind-fed neutron star (NS) compact (\(P_{\rm orb}<10\) days) high-mass X-ray binaries (HMXBs) in our Galaxy, based on different spin-down models. We find that the spin-down rate in the supersonic...

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Published inarXiv.org
Main Authors Dai, Hai-Lang, Liu, Xi-Wei, Li, Xiang-Dong
Format Paper Journal Article
LanguageEnglish
Published Ithaca Cornell University Library, arXiv.org 12.01.2016
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Summary:We use the evolutionary population synthesis method to investigate the statistical properties of the wind-fed neutron star (NS) compact (\(P_{\rm orb}<10\) days) high-mass X-ray binaries (HMXBs) in our Galaxy, based on different spin-down models. We find that the spin-down rate in the supersonic propeller phase given \textbf{by assuming that the surrounding material is treated as forming a quasi-static atmosphere} or \textbf{by assuming that the characteristic velocity of matter and the typical Alfv\(\acute{e}\)n velocity of material in the magnetospheric boundary layer are comparable to the sound speed in the external medium} is too low to produce the observed number of compact HMXBs. We also find that the models suggested \textbf{by assuming that the infalling material is ejected with the corotation velocity at the magnetospheric radius when the magnetospheric radius is larger than the corotation radius} and \textbf{by simple integration of the magnetic torque over the magnetosphere} with a larger spin-down rate than that given by \citet{dav81} or \citet{is75} can predict a reasonable number of observed wind-fed NS compact HMXBs. Our calculated results indicate that subsonic propeller phase may not exist at all by comparing with the observed particular distributions of wind-fed NS compact HMXBs in the \(P_s-P_{orb}\) diagram. However, the spin-down rate suggested by \citet{wan85,dai06,jia05} and that given by \citet{dav73} both seem reasonable to produce the observed distribution of wind-fed NS compact HMXBs in the \(P_s-P_{orb}\) diagram. We cannot find which spin-down rate seems more reasonable from our calculations.
ISSN:2331-8422
DOI:10.48550/arxiv.1601.02891