A study of natural frequencies in a dynamic corona – disk system

Mastichiadis, A.; Πετροπούλου, Μαρία; Kylafis, N. D.

doi:10.1051/0004-6361/202243397

Cited by 18 publications

(10 citation statements)

References 55 publications

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“…Finally, the QPO shows a double-peak structure during the peak of the outburst, implying that the structure of the accretion column or the physics of the radiation mechanism that produces the QPO changes at high luminosity. Some of the above results are analogous to what is observed in lowfrequency QPOs in black-hole binaries, which have been proposed to be due to a resonance of the X-ray corona and the accretion disc (Mastichiadis, Petropoulou, & Kylafis 2022). Considering some of the similarities between the mHz QPO in 1A 0535+262 and the lowfrequency QPOs in black-hole binaries, the QPO in 1A 0535+262 could be due to a resonance between the accretion column and the accretion disc or the neutron-star surface (or both).…”

Section: Discussionsupporting

confidence: 80%

High energy millihertz quasi-periodic oscillations in 1A 0535 + 262 with Insight-HXMT challenge current models

Tao

Zhang

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We studied the millihertz quasi-periodic oscillation (mHz QPO) in the 2020 outburst of the Be/X-ray binary 1A 0535+262 using Insight-HXMT data over a broad energy band. The mHz QPO is detected in the 27–120 keV energy band. The QPO centroid frequency is correlated with the source flux, and evolves in the 35–95 mHz range during the outburst. The QPO is most significant in the 50–65 keV band, with a significance of ∼8σ, but is hardly detectable (<2σ) in the lowest (1–27 keV) and highest (>120 keV) energy bands. Notably, the detection of mHz QPO above 80 keV is the highest energy at which mHz QPOs have been detected so far. The fractional rms of the mHz QPO first increases and then decreases with energy, reaching the maximum amplitude at 50–65 keV. In addition, at the peak of the outburst, the mHz QPO shows a double-peak structure, with the difference between the two peaks being constant at ∼ 0.02 Hz, twice the spin frequency of the neutron star in this system. We discuss different scenarios explaining the generation of the mHz QPO, including the beat frequency model, the Keplerian frequency model, the model of two jets in opposite directions, and the precession of the neutron star, but find that none of them can explain the origin of the QPO well. We conclude that the variability of non-thermal radiation may account for the mHz QPO, but further theoretical studies are needed to reveal the physical mechanism.

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Section: Discussionsupporting

confidence: 80%

High energy millihertz quasi-periodic oscillations in 1A 0535 + 262 with Insight-HXMT challenge current models

Tao

Zhang

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…Our results are not necessarily inconsistent with the QPO frequency being due to Lense-Thirring Precession (LTP, Stella & Vietri 1998; but see Mastichiadis et al 2022). For instance, Ingram et al (2016) fitted the energy spectra of the BHXRB H1743−322 over the cycle of a ∼4-5 QPO and concluded that the results are consistent with LTP of an inner hot torus in this source.…”

Section: Size Of the Coronasupporting

confidence: 52%

The comptonizing medium of the black hole X-ray binary MAXI J1535−571 through type-C quasi-periodic oscillations

Rawat

Méndez

García

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present a detailed spectral and temporal analysis of the black-hole candidate MAXI J1535−571 using NICER observations in September and October 2017. We focus specifically on observations in the hard-intermediate state when the source shows type-C quasi-periodic oscillations (QPOs). We fitted the time-averaged spectrum of the source and the rms and phase-lag spectra of the QPO with a one-component time-dependent Comptonization model. We found that the corona contracts from ∼104 to ∼3 × 103 km as the QPO frequency increases from ∼1.8 Hz to ∼9.0 Hz. The fits suggest that the system would consists of two coronas, a small one that dominates the time-averaged spectrum and a larger one, possibly the jet, that dominates the rms and lag spectra of the QPO. We found a significant break in the relation of the spectral parameters of the source and the properties of the QPO, including its lag spectra, with QPO frequency. The change in the relations happens when the QPO frequency crosses a critical frequency νc ≈ 3.0 Hz. Interestingly, the QPO reaches this critical frequency simultaneously as the radio emission from the jet in this source is quenched.

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“…The geometry of the accretion flow near the black hole in these systems remains a topic of debate, and several accretion disc-corona coupling models have been proposed (e.g., Reig et al 2003;Ingram et al 2009;Kylafis & Reig 2018;Marcel et al 2018;Zdziarski et al 2021;Kawamura et al 2022;Mastichiadis et al 2022).…”

Section: Geometry Of the Corona From The Energy-dependent Variabilitymentioning

confidence: 99%

A variable corona during the transition from type-C to type-B quasi-periodic oscillations in the black hole X-ray binary MAXI J1820+070

Méndez

García

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We analyze a Neutron Star Interior Composition Explorer (NICER) observation of the black hole X-ray binary MAXI J1820+070 during a transition from type-C to type-B quasi-periodic oscillations (QPOs). We find that below ∼2 keV, for the type-B QPOs the rms amplitude is lower and the magnitude of the phase lags is larger than for the type-C QPOs. Above that energy, the rms and phase-lag spectra of the type-B and type-C QPOs are consistent with being the same. We perform a joint fit of the time-averaged spectra of the source, and the rms and phase-lag spectra of the QPOs with the time-dependent Comptonization model vkompth to study the geometry of the corona during the transition. We find that the data can be well-fitted with a model consisting of a small and a large corona that are physically connected. The sizes of the small and large coronae increase gradually during the type-C QPO phase whereas they decrease abruptly at the transition to type-B QPO. At the same time, the inner radius of the disc moves inward at the QPO transition. Combined with simultaneous radio observations showing that discrete jet ejections happen around the time of the QPO transition, we propose that a corona that expands horizontally during the type-C QPO phase, from ∼104 km (∼800 Rg) to 105 km (∼8000 Rg) overlying the accretion disc, transforms into a vertical jet-like corona extending over ∼104 km (∼800 Rg) during the type-B QPO phase.

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A study of natural frequencies in a dynamic corona – disk system

Cited by 18 publications

References 55 publications

High energy millihertz quasi-periodic oscillations in 1A 0535 + 262 with Insight-HXMT challenge current models

High energy millihertz quasi-periodic oscillations in 1A 0535 + 262 with Insight-HXMT challenge current models

The comptonizing medium of the black hole X-ray binary MAXI J1535−571 through type-C quasi-periodic oscillations

A variable corona during the transition from type-C to type-B quasi-periodic oscillations in the black hole X-ray binary MAXI J1820+070

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