A model for 3:2 HFQPO pairs in black hole binaries based on cosmic battery

Huang, Chang‐Yin; Ye, Yong‐Chun; Wang, Ding-Xiong; Li, Yang

doi:10.1093/mnras/stw226

Cited by 3 publications

(7 citation statements)

References 63 publications

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“…As suggested by Kylafis et al (2012), the current is generated near the innermost stable circular orbit (ISCO) of the disk. Fitting the 3:2 HFQPO pairs and the associated spectrum from BHXBs by Huang et al (2016) also indicates that the current is very near the ISCO. For simplicity, We set r PRCB = 1.01r ISCO in this work, where r ISCO is the radius of ISCO.…”

Section: The Magnetic Disk-corona Modelmentioning

confidence: 89%

“…In the PRCB scenario, electrons in the inner accretion disk feel a much stronger radiation-drag force than the ions due to a much larger Thompson cross-section leading to an electric current loop generated near the inner edge of the accretion disk. The current intensity can be estimated as (Huang et al, 2016)…”

Section: The Magnetic Disk-corona Modelmentioning

confidence: 99%

“…where ∆t and ∆S are the average scattering time of electrons with photons and the cross-section of the current, respectively, F is the radiation flux from the relativistic accretion disk (Novikov & Thorne, 1973;Page & Thorne, 1974), n is the number density of electrons, v k is the Kepler velocity, σ T is the Thompson cross-section and e is the electric quality of an electron. Following Huang et al (2016), we set ∆t = 10 −9 s and ∆S = (0.01M BH ) 2 , where M BH is the BH mass. The values of F , n and v k are all evaluated at the radius r PRCB where the current is generated.…”

Section: The Magnetic Disk-corona Modelmentioning

confidence: 99%

“…The magnetic fields generated by the PRCB current can be calculated in the frame of general relativity (Linet, 1979;Li, 2002b). As shown in Huang et al (2016), two types of MC configurations are created by the PRCB current with one connecting the BH horizon and the disk and the other connecting the plunging region and the inner disk. The rotational energy of both the BH and the plunging region can be transferred to the inner disk by these two MC processes.…”

Section: The Magnetic Disk-corona Modelmentioning

confidence: 99%

“…However, quantitative and numerical analyses are needed to test this result. In this paper, we estimate the BH mass in NGC 1313 X-1 by modelling the 3:2 QPOs and the associated X-ray spectrum simultaneously based on the epicyclic resonance model (ERM) and a magnetic disk-corona model developed by Huang et al (2016).…”

Section: Introductionmentioning

confidence: 99%

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Estimating the black hole mass of NGC1313 X-1 based on the spectral and timing properties

Huang¹,

Chang-Yin²

2019

Preprint

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The discovery of 3:2 quasi-periodic oscillations (QPOs) in the ultraluminous X-ray source NGC 1313 X-1 suggests it harbors an intermediate-mass black hole (IMBH). We test this numerically by modelling the 3:2 QPOs and the associated X-ray spectrum based on the epicyclic resonance model and a disk-corona model with large-scale magnetic fields generated by the Cosmic Battery mechanism. The combined QPO-frequency and spectral fitting indicates that the BH mass ranges from 2524M⊙ to 6811M⊙ confirming its IMBH nature, and the BH spin is probably higher than ∼ 0.3.

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Section: The Magnetic Disk-corona Modelmentioning

confidence: 89%

Section: The Magnetic Disk-corona Modelmentioning

confidence: 99%

Section: The Magnetic Disk-corona Modelmentioning

confidence: 99%

Section: The Magnetic Disk-corona Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Estimating the black hole mass of NGC1313 X-1 based on the spectral and timing properties

Huang¹,

Chang-Yin²

2019

Preprint

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Accretion tori around rotating neutron stars

Matuszková,

Török,

Klimovičová

et al. 2024

A&A

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The four characteristic oscillation frequencies of accretion flows (in addition to the Keplerian orbital frequency) are often discussed in the context of the time variability of black hole and neutron star (NS) low-mass X-ray binaries (LMXBs). These four frequencies are the frequencies of the axisymmetric radial and vertical epicyclic oscillations, and the frequencies of non-axisymmetric oscillations corresponding to the periastron (radial) and Lense-Thirring (vertical) precessions. In this context, we investigated the effect of the quadrupole moment of a slowly rotating NS and provide complete formulae for calculating these oscillation and precession frequencies, as well as convenient approximations. Simple formulae corresponding to the geodesic limit of a slender torus (and test-particle motion) and the limit of a marginally overflowing torus (a torus exhibiting a critical cusp) are presented, and more general approximate formulae are included to allow calculations for arbitrarily thick tori. We provide the Wolfram Mathematica code used for our calculations together with the C++ and PYTHON codes for calculating the frequencies. Our formulae can be used for various calculations regarding the astrophysical signatures of the NS super-dense matter equation of state. For instance, we demonstrate that even for a given fixed number of free parameters, a model that accounts for fluid flow precession matches the frequencies of twin-peak quasiperiodic oscillations observed in NS LMXBs better than a model that uses geodesic precession.

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Simple Analytic Formula Relating the Mass and Spin of Accreting Compact Objects to Their Rapid X-Ray Variability

Török

Kotrlová

Matuszková

et al. 2022

ApJ

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Following the previous research on epicyclic oscillations of accretion disks around black holes (BHs) and neutron stars (NSs), a new model of high-frequency quasiperiodic oscillations (QPOs) has been proposed, so-called cusp torus (CT) model, which deals with oscillations of fluid in marginally overflowing accretion tori (i.e., tori terminated by cusps). According to preliminary investigations, the model provides better fits of the NS QPO data compared to the relativistic precession (RP) model. It also implies a significantly higher upper limit on the Galactic microquasar BH spins. A short analytic formula has been noticed to well reproduce the model’s predictions on the QPO frequencies in Schwarzschild spacetimes. Here we derive an extended version of this formula that applies to rotating compact objects. We start with the consideration of Kerr spacetimes and derive a formula that is not restricted to a particular specific angular momentum distribution of the inner accretion flow, such as a Keplerian or constant one. Finally, we consider Hartle–Thorne spacetimes and include corrections implied by the NS oblateness. For a particular choice of a single parameter, our relation provides frequencies predicted by the CT model. For another value, it provides frequencies predicted by the RP model. We conclude that the formula is well applicable to rotating oblate NSs and both models. We briefly illustrate the application of our simple formula on several NS sources and confirm the expectation that the CT model is compatible with realistic values of the NS mass and provides better fits of data than the RP model.

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A model for 3:2 HFQPO pairs in black hole binaries based on cosmic battery

Cited by 3 publications

References 63 publications

Estimating the black hole mass of NGC1313 X-1 based on the spectral and timing properties

Estimating the black hole mass of NGC1313 X-1 based on the spectral and timing properties

Accretion tori around rotating neutron stars

Simple Analytic Formula Relating the Mass and Spin of Accreting Compact Objects to Their Rapid X-Ray Variability

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