The evolution of the corona in MAXI J1535−571 through type-C quasi-periodic oscillations with <i>Insight</i>-HXMT

Zhang, Yuexin; Méndez, Mariano; García, Federico; Zhang, Shuang‐Nan; Καρπούζας, Κωνσταντίνος; Altamirano, D.; Belloni, T.; Qu, J. L.; Zhang, Shu; Tao, Lian; Zhang, Liang; Huang, Y.; Kong, L. D.; Ma, Ruican; Yu, Wei; Rawat, Divya; Bellavita, Candela

doi:10.1093/mnras/stac690

Cited by 33 publications

(43 citation statements)

References 75 publications

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“…This was expected given the energy coverage from RXTE, which was not sensitive below ∼3 keV. In addition, recently Zhang et al (2022) successfully applied the vkompthdk model to fit the type-C QPOs in MAXI J1535-571, using HXMT data ranging from 1 to 100 keV. Therefore, we conclude that this variable-Comptonisation model is able to explain both type-B and type-C low-frequency QPOs in BH LMXB binaries.…”

Section: Discussionsupporting

confidence: 51%

vKompth: a variable Comptonization model for low-frequency quasi-periodic oscillations in black hole X-ray binaries

Bellavita

García

Méndez

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Low mass X-ray binaries (LMXBs) show strong variability over a broad range of time scales. The analysis of this variability, in particular of the quasi-periodic oscillations (QPO), is key to understanding the properties of the innermost regions of the accretion flow in these systems. We present a time-dependent Comptonisation model that fits the energy-dependent rms-amplitude and phase-lag spectra of low-frequency QPOs in black hole (BH) LMXBs. We model the accretion disc as a multi-temperature blackbody source emitting soft photons which are then Compton up-scattered in a spherical corona, including feedback of Comptonised photons that return to the disc. We compare our results with those obtained with a model in which the seed-photons source is a spherical blackbody: at low energies the time-averaged, rms and phase-lag spectra are smoother for the disk-blackbody than for a blackbody, while at high energies both models give similar spectra. In general, we find that the rms increases with energy, the slope of the phase-lag spectrum depends strongly on the feedback, while the minimum-lag energy is correlated with the disc temperature. We fit the model to a 4.45-Hz type-B QPO in the BH LMXB MAXI J1438–630 and find statistically-better fits and more compatible parameters with the steady-state spectrum than those obtained with a blackbody seed-photons source. Furthermore, we successfully apply the model to the type-C QPO in the BH LMXB GRS 1915+105, and thus conclude that this variable-Comptonisation model reproduces the rms and phase-lags of both type B and C low-frequency QPOs in BH LMXBs.

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Section: Discussionsupporting

confidence: 51%

vKompth: a variable Comptonization model for low-frequency quasi-periodic oscillations in black hole X-ray binaries

Bellavita

García

Méndez

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…Ingram, Done & Fragile 2009 ;You, Bursa & Życki 2018 ;You et al 2020 ). This Comptonization model was used to study the Comptonizing medium in the neutron star 4U 1636 − 53 through the lower kilohertz QPOs (Karpouzas et al 2020 ), and the rms and lag-energy spectra of the type-B QPOs in MAXI J1348 − 630 (Garc ía et al 2021 ) and the type-C QPOs in MAXI J1535 − 571 (Zhang et al 2022 ). Further studies are ongoing to apply this model to the LFQPOs in the black hole GRS 1915 + 105(see also Karpouzas et al 2021 ;Garc ía et al 2022 ).…”

Section: Discussionmentioning

confidence: 99%

The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE

Zhang

Méndez

García

et al. 2022

Monthly Notices of the Royal Astronomical Society

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GRS 1915+105 can show type-C quasi-periodic oscillations (QPOs) in the power density spectrum. A high-frequency QPO (HFQPO) at 67 Hz has been observed in this source, albeit less often than the type-C QPOs. Besides these features, GRS 1915+105 sometimes shows a broad bump in the power spectrum at around 30–150 Hz. We study the power spectra of GRS 1915+105 with the Rossi X-ray Timing Explorer when the source was in the χ class. We find that the rms amplitude of the bump depends strongly upon both the frequency of the type-C QPO and the hardness ratio, and is correlated with the corona temperature and anti-correlated with the radio flux at 15 GHz. The characteristic frequency of the bump is better correlated with a combination of the frequency of the type-C QPO and the hardness ratio than with the frequency of the type-C QPO alone. The rms amplitude of the bump generally increases with energy from ∼1–2 per cent at ∼3 keV to ∼10–15 per cent at ∼30 keV. We suggest that the bump and the high-frequency QPO may be the same variability component but the properties of the corona affect the coherence of this variability, leading either to a HFQPO when the spectrum is in the relatively soft γ class, or to a bump when the spectrum is in the hard χ class. Finally, we discuss the anti-correlation between the rms amplitude of the bump and the radio flux in the context of the relation between the corona and the jet.

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“…Note that this model does not explain the dynamical origin of the QPOs, but assumes that the QPO frequency is produced by some mechanisms (e.g., Ingram et al 2009;You et al 2018You et al , 2020. This Comptonization model was used to study the Comptonizing medium in the neutron star 4U 1636−53 through the lower kilohertz QPOs (Karpouzas et al 2020), and the rms and lag-energy spectra of the type-B QPOs in MAXI J1348−630 (García et al 2021) and the type-C QPOs in MAXI J1535−571 (Zhang et al 2022). Further studies are ongoing to apply this model to the LFQPOs in the black hole GRS 1915+105 (see also Karpouzas et al 2021;García et al 2022).…”

Section: Discussionmentioning

confidence: 99%

The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE

Zhang,

Méndez,

García

et al. 2022

Preprint

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GRS 1915+105 can show type-C quasi-periodic oscillations (QPOs) in the power density spectrum. A high-frequency QPO (HFQPO) at 67 Hz has been observed in this source, albeit less often than the type-C QPOs. Besides these features, GRS 1915+105 sometimes shows a broad bump in the power spectrum at around 30-150 Hz. We study the power spectra of GRS 1915+105 with the Rossi X-ray Timing Explorer when the source was in the 𝜒 class. We find that the rms amplitude of the bump depends strongly upon both the frequency of the type-C QPO and the hardness ratio, and is correlated with the corona temperature and anti-correlated with the radio flux at 15 GHz. The characteristic frequency of the bump is better correlated with a combination of the frequency of the type-C QPO and the hardness ratio than with the frequency of the type-C QPO alone. The rms amplitude of the bump generally increases with energy from ∼1-2% at ∼3 keV to ∼10-15% at ∼30 keV. We suggest that the bump and the high-frequency QPO may be the same variability component but the properties of the corona affect the coherence of this variability, leading either to a HFQPO when the spectrum is in the relatively soft 𝛾 class, or to a bump when the spectrum is in the hard 𝜒 class. Finally, we discuss the anti-correlation between the rms amplitude of the bump and the radio flux in the context of the relation between the corona and the jet.

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The evolution of the corona in MAXI J1535−571 through type-C quasi-periodic oscillations with Insight-HXMT

Cited by 33 publications

References 75 publications

vKompth: a variable Comptonization model for low-frequency quasi-periodic oscillations in black hole X-ray binaries

vKompth: a variable Comptonization model for low-frequency quasi-periodic oscillations in black hole X-ray binaries

The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE

The evolution of the high-frequency variability in the black hole candidate GRS 1915+105 as seen by RXTE

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