The correlations between the spin frequencies and kHz QPOs of neutron stars in LMXBs

Yin, H. X.; Zhang, C. M.; Zhao, Yi; Lei, Y. J.; Qu, J. L.; Song, Liming; Zhang, Faming

doi:10.1051/0004-6361:20077069

Cited by 36 publications

(34 citation statements)

References 40 publications

(27 reference statements)

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“…The 24 accretion millisecond X-ray pulsars discovered by RXTE (see e.g. Wijnands 2005;Lamb & Yu 2005;Yin et al 2007) are put in the spin period histogram.…”

Section: Introductionmentioning

confidence: 99%

Spin period evolution of a recycled pulsar in an accreting binary

Wang

Zhang

Zhao

et al. 2011

A&A

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We investigate the spin period evolutions of recycled pulsars in binary accreting systems. Taking both the accretion induced field decay and spin-up into consideration, we calculate their spin period evolutions influenced by the initial magnetic field strengths, initial spin periods, and accretion rates. The results indicate that the minimum spin period (or maximum spin frequency) of a millisecond pulsar (MSP) is independent of the initial conditions and accretion rate when the neutron star (NS) accretes the mass of ∼0.2 M . The accretion torque with the fastness parameter and gravitational wave (GW) radiation torque may be responsible for the formation of the minimum spin period (maximum spin frequency). The fastest spin frequency (716 Hz) of MSP can be inferred to associate with a critical fastness parameter of about ω c = 0.55. Furthermore, comparisons with the observational data are presented in the field period (B − P) diagram.

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“…The 24 accretion millisecond X-ray pulsars discovered by RXTE (see e.g. Wijnands 2005;Lamb & Yu 2005;Yin et al 2007) are put in the spin period histogram.…”

Section: Introductionmentioning

confidence: 99%

Spin period evolution of a recycled pulsar in an accreting binary

Wang

Zhang

Zhao

et al. 2011

A&A

Self Cite

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“…With mass accretion rates and f max = 584 Hz for GX 17+2 and f max = 658 Hz for Cyg X-2 (Yin et al 2007), we infer the limits of B 0 and get (1 B 0 5) × 10 8 G and (1 B 0 3) × 10 8 G for GX 17+2 and Cyg X-2, respectively, which are higher than the reported B 0 ∼ (0.3 − 1) × 10 8 G of atoll source Aql X-1 (Zhang et al 1998), compatible with B 0 ∼ (1 − 5) × 10 8 G of accreting millisecond X-ray pulsar SAX J1808.4-3658 (Di Salvo & Burderi 2003), but lower than B 0 ∼ (1 − 3) × 10 9 G of the first transient Z source XTE J1701-462 (Ding et al 2011) or B 0 ∼ (1 − 8) × 10 9 G of Cir X-1 . Since the B 0 of Z sources is not inferior to that of millisecond X-ray pulsars or atoll source, pulsations should have been observed in the former, as in the latter.…”

Section: Resultsmentioning

confidence: 99%

Determining the neutron star surface magnetic field strength of two Z sources

Ding¹,

Huang²,

Wang³

2012

Proc. IAU

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Abstract. From the extreme position of disk motion, we infer the neutron star (NS) surface magnetic field strength (B0) of Z-source GX 17+2 and Cyg X-2. The inferred B0 of GX 17+2 and Cyg X-2 are ∼(1-5)×108 G and ∼(1-3)×10 8 G, respectively, which are not inferior to that of millisecond X-ray pulsars or atoll sources. It is likely that the NS magnetic axis of Z sources is parallel to the axis of rotation, which could result in the lack of pulsations in these sources.

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“…Several LMXBs have been observed with known spin rate and showing the twin peak QPO phenomenon, see for instance [4]. Depending on the neutron star rotation speed, they have been classified as slow rotator for ν * 400 Hz or as fast rotator for ν * 400 Hz, (ν * = Ω * /2 π).…”

Section: Model and Methodsmentioning

confidence: 99%

Constraining the mass and moment of inertia of neutron star from quasi-periodic oscillations in X-ray binaries

Pétri¹

2011

Proceedings of Fast X-Ray Timing and Spectroscopy at Extreme Count Rates — PoS(HTRS 2011)

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Neutron stars are the densest objects known in the Universe. Being the final product of stellar evolution, their internal composition and structure is rather poorly constrained by measurements. We put some constraints on the mass and moment of inertia of these neutron stars based on the interpretation of quasi-periodic oscillations observed in low mass X-ray binaries (LMXBs). More specifically, we use observations of high-frequency quasi-periodic observations (HF-QPOs) to look for the average mass and moment of inertia of neutron stars. This is done by applying our parametric resonance model to discriminate between slow and fast rotators. We fit our model to data from ten LMXBs for which HF-QPOs have been seen and the spin of the enclosed accreting neutron star is known. We find an average mass M * ≈ 2.0 − 2.2 M ⊙ . The corresponding average moment of inertia is then I * ≈ 1 − 3 × 10 38 kg m 2 ≈ 0.5 − 1.5 (10 km) 2 M ⊙ .

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The correlations between the spin frequencies and kHz QPOs of neutron stars in LMXBs

Cited by 36 publications

References 40 publications

Spin period evolution of a recycled pulsar in an accreting binary

Spin period evolution of a recycled pulsar in an accreting binary

Determining the neutron star surface magnetic field strength of two Z sources

Constraining the mass and moment of inertia of neutron star from quasi-periodic oscillations in X-ray binaries

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