The orbital resonance model for twin peak kHz quasi periodic oscillations in microquasars

Török, Gabriel; Abramowicz, Marek A.; Kluźniak, W.; Stuchlík, Zdeněk

doi:10.1051/0004-6361:20047115

Cited by 211 publications

(252 citation statements)

References 25 publications

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“…The twin peak separation being either ∆ν = ν * for slow rotator (ν * ≈ 300 Hz) or ∆ν = ν * /2 for fast rotator (ν * ≈ 600 Hz) is also explained. Indeed, it was previously argued by Kluźniak et al (2005) that the 3:2 QPOs recently observed in white dwarf sources by Warner & Woudt (2005) have the same nature as the strong gravity 3:2 QPOs observed in neutron star and black hole sources. All of them are resonant accretion disk oscillations.…”

Section: Resultsmentioning

confidence: 73%

An explanation for the kHz-QPO twin peaks separation in slow and fast rotators

Pétri

2005

A&A

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Abstract. In this Letter we further explore the idea, suggested previously by Kluźniak and collaborators, that the high frequency QPOs may be explained as a resonant coupling between the neutron star spin and two epicyclic modes of accretion disk oscillations. We confirm result of Lee et al. (2004, ApJ, 603, L93) that the strongest response occurs when the frequency difference of the two modes equals either the spin frequency (for "slow rotators") or half of it (for "fast rotators"). New points discussed in this Letter are: (1) we suggest that the coupling is gravitational, and due to a non-axially symmetric structure of the rotating neutron star; (2) we found that two excited modes may be both connected to vertical oscillations of the disk, and that strong gravity is not needed to excite the modes.

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Section: Resultsmentioning

confidence: 73%

An explanation for the kHz-QPO twin peaks separation in slow and fast rotators

Pétri

2005

A&A

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“…Some researchers proposed the sonic-point and spin-resonance models (Lamb & Miller, 2001, 2003Miller et al, 1998), which explain that the frequency separation of the twin kHz QPOs is close to the spin frequency of NS or its half. Abramowicz et al (2003a,b); Kluźniak & Abramowicz (2001) introduced the resonance model with the upper frequency corresponding to the vertical epicyclic frequency and the lower frequency corresponding to the radial epicyclic frequency, which accords with observational data quite well in the black-hole binary systems (Török et al, 2005. But the last two models show the inconsistent with the subsequent twin kHz QPO observations (Belloni et al, 2007;Jonker et al, 2002a;Muno, 2004;Strohmayer & Bildsten, 2006;Urbanec et al, 2010;van der Klis, 2006;Wijnands et al, 2003;Zhang et al, 2006a).…”

Section: Introductionmentioning

confidence: 76%

Statistical properties of twin kilohertz quasi‐periodic oscillations in neutron star low‐mass X‐ray binaries

et al. 2014

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We collect the data of twin kilohertz quasi-periodic oscillations (kHz QPOs) published before 2012 from 26 neutron star (NS) low-mass X-ray binary (LMXB) sources, then we analyze the centroid frequency (ν) distribution of twin kHz QPOs (lower frequency ν1 and upper frequency ν2) both for Atoll and Z sources. For the data without shift-and-add, we find that Atoll and Z sources show the different distributions of ν1, ν2 and ν2/ν1, but the same distribution of ∆ν (difference of twin kHz QPOs), which indicates that twin kHz QPOs may share the common properties of LXMBs and have the same physical origins. The distribution of ∆ν is quite different from constant value, so is ν2/ν1 from constant ratio. The weighted mean values and maxima of ν1 and ν2 in Atoll sources are slightly higher than those in Z sources. We also find that shift-and-add technique can reconstruct the distribution of ν1 and ∆ν. The K-S test results of ν1 and ∆ν between Atoll and Z sources from data with shift-and-add are quite different from those without it, and we think that this may be caused by the selection biases of the sample. We also study the properties of the quality factor (Q) and the root-mean-squared (rms) amplitude of 4U 0614+09 with the data from the two observational methods, but the errors are too big to make a robust conclusion. The NS spin frequency (νs) distribution of 28 NS-LMXBs show a bigger mean value (∼ 408 Hz) than that (∼ 281 Hz) of the radio binary millisecond pulsars (MSPs), which may be due to the lack of the spin detections from Z sources (systematically lower than 281 Hz). Furthermore, on the relations between the kHz QPOs and NS spin frequency νs, we find the approximate correlations of the mean values of ∆ν with NS spin and its half, respectively.

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“…In this context we note that the high spins we have measured for three of the four BHs listed in Table 1 were very likely imparted to these BHs during the process of their formation (see §6.2 in . Knowledge of BH spin is also crucial for the development of gravitational-wave astronomy and for models of quasiperiodic oscillations in BH X-ray binaries (Török et al 2005).…”

Section: Discussionmentioning

confidence: 99%

Estimating the Spins of Stellar-Mass Black Holes by Fitting Their Continuum Spectra

Narayan¹,

McClintock²,

Shafee³

2008

AIP Conference Proceedings

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Abstract.We have used the Novikov-Thorne thin disk model to fit the continuum X-ray spectra of three transient black hole X-ray binaries in the thermal state. From the fits we estimate the dimensionless spin parameters of the black holes to be: 4U 1543-47, a * ≡ a/M = 0.7 − 0.85; GRO J1655-40, a * = 0.65 − 0.8; GRS 1915+105, a * = 0.98 − 1. We plan to expand the sample of spin estimates to about a dozen over the next several years. Some unresolved theoretical issues are briefly discussed.

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The orbital resonance model for twin peak kHz quasi periodic oscillations in microquasars

Cited by 211 publications

References 25 publications

An explanation for the kHz-QPO twin peaks separation in slow and fast rotators

An explanation for the kHz-QPO twin peaks separation in slow and fast rotators

Statistical properties of twin kilohertz quasi‐periodic oscillations in neutron star low‐mass X‐ray binaries

Estimating the Spins of Stellar-Mass Black Holes by Fitting Their Continuum Spectra

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