A Brief Review for Quasi-Periodic Oscillations in Neutron-Star Low-Mass X-Ray Binaries

Wang, Jing

doi:10.4236/ijaa.2016.61006

Cited by 17 publications

(11 citation statements)

References 91 publications

(105 reference statements)

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“…In the EPIC-pn data, we find a prominent narrow feature at ∼8 mHz, resembling a QPO (see, e.g., Wang 2016, for a recent review), while the broad-band noise is characterized by four zero-centered Lorentzians (L 1 -L 4 ). In the harder NuSTAR band, the broad-band noise has a similar shape, while the narrow 8 mHz feature disappears, substituted by a narrow weak feature at roughly double its frequency (QPO 2 in Table 2 with rms 7%) and by a broader component at a slightly lower frequency (6 mHz).…”

Section: The Timing Analysismentioning

confidence: 73%

Discovery of a soft X-ray 8 mHz QPO from the accreting millisecond pulsar IGR J00291+5934

Ferrigno

Bozzo

Sanna

et al. 2016

Mon. Not. R. Astron. Soc.

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In this paper, we report on the analysis of the peculiar X-ray variability displayed by the accreting millisecond X-ray pulsar IGR J00291+5934 in a 80 ks-long joint NuSTAR and XMM-Newton observation performed during the source outburst in 2015. The light curve of the source was characterized by a flaring-like behavior, with typical rise and decay time scales of ∼120 s. The flares are accompanied by a remarkable spectral variability, with the X-ray emission being generally softer at the peak of the flares. A strong quasi periodic oscillation (QPO) is detected at ∼8 mHz in the power spectrum of the source and clearly associated with the flaring-like behavior. This feature has the strongest power at soft X-rays ( < ∼ 3 keV). We carried out a dedicated hardness-ratio resolved spectral analysis and a QPO phase-resolved spectral analysis, together with an in-depth study of the source timing properties, to investigate the origin of this behavior. We suggest that the unusual variability of IGR J00291+5934 observed by XMM-Newton and NuSTAR could be produced by an heartbeat-like mechanism, similar to that operating in black-hole X-ray binaries. The possibility that this variability, and the associated QPO, are triggered by phases of quasi-stable nuclear burning, as suggested in the literature for a number of other neutron star binaries displaying a similar behavior, cannot be solidly tested in the case of IGR J00291+5934 due to the paucity of type-I X-ray bursts observed from this source.

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Section: The Timing Analysismentioning

confidence: 73%

Discovery of a soft X-ray 8 mHz QPO from the accreting millisecond pulsar IGR J00291+5934

Ferrigno

Bozzo

Sanna

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Initially, we looked at observations that contained a QPO detectable in most energy bands and confirmed that the frequency of the kHz QPO in different bands is consistent with being the same, within the chosen frequency intervals, during the same observation. This is an important information to investigate the nature of kHz QPOs (Mukherjee & Bhattacharyya 2012;Wang 2016). In Fig.…”

Section: The Conditional Distributions Of the Rms Amplitude Vs Qpo Fmentioning

confidence: 99%

“…Twenty years after the discovery of kilohertz quasi-periodic oscillations (kHz QPOs, Strohmayer et al 1996;van der Klis et al 1996) in neutron-star low-mass X-ray binaries (NS-LMXB), a satisfactory explanation of the origin of these QPOs remains a challenge (Gilfanov et al 2003;Mendez 2006;de Avellar et al 2013;Barret 2013;Peille et al 2015;Wang 2016;Cackett 2016;Troyer et al 2018). Both the timing and spectral properties of these high-frequency oscillations are likely driven by general relativistic effects (Stella & Vietri 1998Kato 2005), the neutron-star mass and radius , and the physical processes taking 2018).…”

Section: Introductionmentioning

confidence: 99%

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The amplitude of the kilohertz quasi-periodic oscillations in 4U 1636–53 in the frequency-energy space

Ribeiro

Méndez

Avellar

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present for the neutron-star low-mass X-ray binary 4U 1636−53, and for the first time for any source of kilohertz quasi-periodic oscillations (kHz QPOs), the twodimensional behaviour of the fractional rms amplitude of the kHz QPOs in the parameter space defined by QPO frequency and photon energy. We find that the rms amplitude of the lower kHz QPO increases with energy up to ∼ 12 keV and then decreases at higher energies, while the rms amplitude of the upper kHz QPO either continues increasing or levels off at high energies. The rms amplitude of the lower kHz QPO increases and then decreases with frequency, peaking at ∼ 760 Hz, while the amplitude of the upper kHz QPO decreases with frequency, with a local maximum at around ∼ 770 Hz, and is consistent with becoming zero at the same QPO frequency, ∼ 1400 Hz, in all energy bands, thus constraining the neutron-star mass at M N S ≤ 1.6M , under the assumption that this QPO reflects the Keplerian frequency at the inner edge of the accretion disc. We show that the slope of the rms energy spectrum is connected to the changing properties of the kHz QPOs in different energy bands as its frequencies change. Finally, we discuss a possible mechanism responsible for the radiative properties of the kHz QPOs and, based on a model in which the QPO arises from oscillations in a Comptonising cloud of hot electrons, we show that the properties of the kHz QPOs can constrain the thermodynamic properties of the inner accretion flow.

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“…We used the MC method to simulate quasi-periodic oscillations (QPOs), which are typical signals in the astronomical timing analysis. In the PSD, QPOs commonly appear as a peak at a certain frequency with a finite width, which can be described as a Lorentzian function (Wang 2016)…”

Section: Qpo Signalsmentioning

confidence: 99%

The influence of the Insight-HXMT/LE time response on timing analysis

Zhou,

Zheng,

Song

et al. 2020

Preprint

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LE is the low energy telescope of Insight-HXMT. It uses swept charge devices (SCDs) to detect soft X-ray photons. The time response of LE is caused by the structure of SCDs. With theoretical analysis and Monte Carlo simulations we discuss the influence of LE time response (LTR) on the timing analysis from three aspects: the power spectral density, the pulse profile and the time lag. After the LTR, the value of power spectral density monotonously decreases with the increasing frequency. The power spectral density of a sinusoidal signal reduces by a half at frequency 536 Hz. The corresponding frequency for QPO signals is 458 Hz. The Root mean square (RMS) of QPOs holds the similar behaviour. After the LTR, the centroid frequency and full width at half maxima (FWHM) of QPOs signals do not change. The LTR reduces the RMS of pulse profiles and shifts the pulse phase. In the time domain, the LTR only reduces the peak value of the crosscorrelation function while it does not change the peak position. Thus it will not affect the result of the time lag. When considering the time lag obtained from two instruments and one among them is LE, a 1.18 ms lag is expected caused by the LTR. The time lag calculated in the frequency domain is the same as that in the time domain.

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A Brief Review for Quasi-Periodic Oscillations in Neutron-Star Low-Mass X-Ray Binaries

Cited by 17 publications

References 91 publications

Discovery of a soft X-ray 8 mHz QPO from the accreting millisecond pulsar IGR J00291+5934

Discovery of a soft X-ray 8 mHz QPO from the accreting millisecond pulsar IGR J00291+5934

The amplitude of the kilohertz quasi-periodic oscillations in 4U 1636–53 in the frequency-energy space

The influence of the Insight-HXMT/LE time response on timing analysis

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