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Dai, Hai-Lang; Liu, Xi‐Wei; Li, Xiangdong

doi:10.1086/508735

Cited by 19 publications

(21 citation statements)

References 36 publications

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“…Our calculation shows the similar conclusion for the spin-down model described by Mori & Ruderman (2003) when γ = −1. We also find that the model suggested by Wang & Robertson (1985), Dai, Liu & Li (2006) and Jiang & Li (2005) with a larger spin-down rate than that given by Davies & Pringle (1981) can predict a reasonable number of observed wind-fed compact NS HMXBs no matter whether the subsonic propeller phase exists or not. We can also derive the similar conclusion for the spin-down model described by Mori & Ruderman (2003) when γ = 0.…”

Section: Resultssupporting

confidence: 67%

“…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 Wang & Robertson (1985); Dai, Liu & Li (2006);Jiang & Li (2005) and that given by Davidson & Ostriker (1973) 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.…”

mentioning

confidence: 55%

“…Some authors proposed a different spin-down model for the propeller phase (Wang & Robertson 1985;Dai, Liu & Li 2006;Jiang & Li 2005;Ikhsanov 2001). They assumed that the plasma is accelerated outward with the corotation velocity at Rm, and the spin-down torque is…”

Section: Spin Evolutionmentioning

confidence: 99%

“…The typical spin-down time-scale τ = |Ωs/Ωs| can be estimated to be (Dai, Liu & Li 2006). The process of spin-down ceases when Ps reaches the equilibrium spin period…”

Section: Spin Evolutionmentioning

confidence: 99%

“…Mori & Ruderman (2003) suggested that two parameters can classify many proposed propeller spin-down models. Many authors have derived the spin-down rate of propeller phase 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 (Wang & Robertson 1985;Dai, Liu & Li 2006;Jiang & Li 2005). Besides, a large number of authors (see, e.g., Spruit & Taam 1993;Rappaport et al 2004;D'Angelo & Spruit 2010, 2012 have investigated the spin-down rate of NS accreting from a disk in a NS HMXB.…”

Section: Introductionmentioning

confidence: 99%

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Exploration of spin-down rate of neutron stars in high-mass X-ray binaries

Dai¹,

Liu²,

Li³

2016

Mon. Not. R. Astron. Soc.

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We use the evolutionary population synthesis method to investigate the statistical properties of the wind-fed neutron star (NS) compact (P 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 by assuming that the surrounding material is treated as forming a quasi-static atmosphere or by assuming that the characteristic velocity of matter and the typical Alfvén 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 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 by simple integration of the magnetic torque over the magnetosphere with a larger spin-down rate than that given by Davies & Pringle (1981) or Illarionov & Sunyaev (1975) 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 Wang & Robertson (1985); Dai, Liu & Li (2006);Jiang & Li (2005) and that given by Davidson & Ostriker (1973) 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.

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Section: Resultssupporting

confidence: 67%

mentioning

confidence: 55%

Section: Spin Evolutionmentioning

confidence: 99%

“…The typical spin-down time-scale τ = |Ωs/Ωs| can be estimated to be (Dai, Liu & Li 2006). The process of spin-down ceases when Ps reaches the equilibrium spin period…”

Section: Spin Evolutionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Exploration of spin-down rate of neutron stars in high-mass X-ray binaries

Dai¹,

Liu²,

Li³

2016

Mon. Not. R. Astron. Soc.

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Be/X-ray binaries

Reig

2011

Astrophys Space Sci

527

522

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The purpose of this work is to review the observational properties of Be/X-ray binaries. The open questions in Be/X-ray binaries include those related to the Be star companion, that is, the so-called "Be phenomenon", such as, timescales associated to the formation and dissipation of the equatorial disc, mass-ejection mechanisms, V/R variability, and rotation rates; those related to the neutron star, such as, mass determination, accretion physics, and spin period evolution; but also, those that result from the interaction of the two constituents, such as, disc truncation and mass transfer. Until recently, it was thought that the Be stars' disc was not significantly affected by the neutron star. In this review, I present the observational evidence accumulated in recent years on the interaction between the circumstellar disc and the compact companion. The most obvious effect is the tidal truncation of the disc. As a result, the equatorial discs in Be/X-ray binaries are smaller and denser than those around isolated Be stars.Comment: "The final publication is available at http://www.springerlink.com". This review article has been accepted for publication in Astrophysics and Space Scienc

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An alternative evolution scenario for OAO 1657-415 and IGR J18483-0311

Liu

Yan

2010

Sci. China Phys. Mech. Astron.

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The relation between the spin period and the orbital period in high-mass X-ray binaries is investigated. Be/X-ray binaries and SG/X-ray binaries occupy different areas in Corbet's diagram. The two SG/X-ray binaries, IGR J18483-0311 and OAO 1657-415, however, appear to occupy a transition region between Be/X-ray binaries and wind-fed SG/X-ray binaries. This can be understood by noting that the neutron stars in the two SG/X-ray binaries have not reached their equilibrium spin periods when the donors evolved off the main sequence. Here, we provide an alternative scenario to explain their location in Corbet's diagram: the SG/X-ray binaries are the descendants of Be/X-ray binaries, i.e. the supergiants in these systems were formed from O-type emission line stars instead of normal main-sequence stars. Furthermore, we suggest that there are two types of SG/X-ray binaries: one is directly evolved from a normal OB-type main sequence and neutron star system without an X-ray history, and the other evolved from a Be/X-ray binary with an X-ray history.high-mass X-ray binary, pulsar, Corbet's diagram, stellar evolution High-mass X-ray binaries (HMXBs) consist of a compact object, mostly a magnetized neutron star or a black hole, orbiting an early-type massive star. Conventionally, HMXBs can be further divided into two subgroups: Those in which the primary is a Be star (Be/X-ray binary) and those in which the primary is a supergiant (SG/X-ray binary). The majority of the known HMXBs are Be/X-ray systems [1]. Most Be/X-ray binaries have relatively wide orbits with moderate eccentricity and the compact companion spends most of its time far away from the disc surrounding the Be star [2]. An X-ray outburst will be expected during the time of the neutron star's periastron passage, from a low velocity extended envelope around a Be star, and thus collectively termed Be/X-ray transients. In the second group of HMXB systems, the compact star orbits a supergiant early type star, deep inside the highly supersonic wind. The X-ray luminosity is either powered by pure stellar wind accretion or, in the case of the brighter systems, by Roche-lobe overflow via an accretion disk. As a result, the SG/X-ray systems are persistent sources of X-rays, while the Be/X-ray systems are very variable and frequently much brighter.Corbet [3] was the first to notice that there is a relation between the spin period and the orbital period of Be/X-ray binaries. Corbet [4] showed that massive X-ray binaries fall into three separate groups when the pulse period is plotted versus the orbital period. Those systems with unevolved Be companions have a strong correlation between the orbital and spin periods, while systems with wind-fed and disk-fed OB supergiant companions fall into two separate broad regions of the diagram. Therefore, the Corbet's diagram has a predictive as well as diagnostic value [5,6].Corbet [3,4] interpreted this correlation in terms of the equilibrium periods of magnetized neutron stars accreting matter. The equilibrium period corresponds to th...

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Cited by 19 publications

References 36 publications

Exploration of spin-down rate of neutron stars in high-mass X-ray binaries

Exploration of spin-down rate of neutron stars in high-mass X-ray binaries

Be/X-ray binaries

An alternative evolution scenario for OAO 1657-415 and IGR J18483-0311

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