Testing Evolution of LFQPOs with Mass Accretion Rate in GRS 1915+105 with Insight-HXMT

Ji, Long; Bambi, Cosimo; Jain, Pankaj; Misra, Ranjeev; Rawat, Divya; Yadav, J. S.; Zhang, Yuexin

doi:10.3847/1538-4357/abdf65

Cited by 17 publications

(8 citation statements)

References 61 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This becomes obvious if we recast the function 𝑓 𝑄𝑃𝑂 / 𝑀 ∝ 𝑅 𝑝 𝑖𝑛 in terms of 𝑓 𝑄𝑃𝑂 , 𝐾𝑇 𝑖𝑛 and 𝑁 𝑑𝑖𝑠𝑐 and by noting that although the constant of the proportionality may depend on the assumed values, the form of the proportionality itself is independent. However, we emphasize that unlike the analysis undertaken on GRS 1915+105 by Misra et al (2020) and Liu et al (2021), the spectra of MAXI J1535-571 here is dominated by the Comptonized component and the disc component is relatively weak. We defer a discussion on these results to the last section.…”

Section: Spectral and Timing Analysiscontrasting

confidence: 61%

“…We found a correlation between the QPO frequency and scattering fraction which is opposite to the anti-correlation reported by Stiele et al (2013) for other black hole binaries like GX 339-4, H1743-322 and XTE J1650-550 using RXTE data. Misra et al (2020)) and Liu et al (2021) have shown that for the black hole system GRS 1915+105, the QPO frequency divided by the accretion rate has a functional dependence on the inner disc radius, allowing them to identify the frequency as the sound crossing time-scale in General Relativity. For an assumed distance, black hole mass, inclination angle and color factor in our analysis, we did find the QPO frequency divided by the accretion rate to be ∝ 𝑅 −2.5 𝑖𝑛 .…”

Section: Discussionmentioning

confidence: 99%

“…However, there is a positive correlation between 𝑅 𝑖𝑛 and 𝑀 as can be seen in the bottom panel where 𝑀 ∝ 𝑅 2.4 𝑖𝑛 . For the QPO and spectral observations of the black hole system, GRS 1915+105, Misra et al (2020) and Liu et al (2021) have shown that the QPO frequency divided by the accretion rate has a functional dependence on the inner disc radius as predicted in General Relativity if the frequency is identified as the dynamical one (i.e. related to the sound crossing time-scale).…”

Section: Spectral and Timing Analysismentioning

confidence: 91%

See 2 more Smart Citations

On the energy dependence of the QPO phenomenon in the black hole system MAXI J1535-571

Garg,

Misra,

Sen

2022

Preprint

Self Cite

View full text Add to dashboard Cite

Previous analysis of AstroSat observations of the black hole system MAXI J1535-571, have revealed the presence of a strong Quasi-Periodic Oscillation (QPO) whose frequency is correlated with the high energy spectral index. Here, we fit the spectra as emitted from a truncated disc with an inner hot corona, study the QPO frequency dependence on other spectral parameters and model the energy dependent r.m.s and time-lag of the QPO to identify the physical spectral parameters whose variation are responsible for the QPO. The QPO frequency is found to also correlate with the scattering fraction (i.e. the fraction of the soft photons Comptonized) and its dependence on the accretion rate and inner disc radii is consistent with it being the dynamical frequency. The time-lag between the hard and soft photons is negative for QPO frequency > 2.2 Hz and is positive for lesser values, making this the second black hole system to show this behaviour after GRS 1915+105. Modelling the energy dependent time-lag and r.m.s requires correlated variation of the accretion rate, inner disc radii and the coronal heating rate, with the latter having a time-lag compared to the other two for QPO frequencies less than < 2.2 Hz and which changes sign (i.e. the coronal heating variation precedes the accretion rate one) for higher values. The implications of the results are discussed.

show abstract

Section: Spectral and Timing Analysiscontrasting

confidence: 61%

Section: Discussionmentioning

confidence: 99%

Section: Spectral and Timing Analysismentioning

confidence: 91%

See 1 more Smart Citation

On the energy dependence of the QPO phenomenon in the black hole system MAXI J1535-571

Garg,

Misra,

Sen

2022

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…We find that the autocorrelation length is typically 1000 elements, so the net number of independent samples in the parameter space we have is of the order of 10 4 . In order to further test the convergence of the MCMC chain, we compare the one-and two-dimensional projections of the posterior distributions for each parameter from the first and second halves of the chain (see also Liu et al 2021), and we find no significant differences. In Appendix, we present the contour maps and probability distributions for each free parameter.…”

Section: Phase-resolved Spectramentioning

confidence: 99%

A Phase-resolved View of the Low-frequency Quasiperiodic Oscillations from the Black Hole Binary MAXI J1820+070

Shui,

Zhang,

Zhang

et al. 2023

ApJ

View full text Add to dashboard Cite

Although low-frequency quasiperiodic oscillations (LFQPOs) are commonly detected in the X-ray light curves of accreting black hole X-ray binaries, their origin still remains elusive. In this study, we conduct phase-resolved spectroscopy in a broad energy band for LFQPOs in MAXI J1820+070 during its 2018 outburst, utilizing Insight-HXMT observations. By employing the Hilbert–Huang transform method, we extract the intrinsic quasiperiodic oscillation (QPO) variability, and obtain the corresponding instantaneous amplitude, phase, and frequency functions for each data point. With well-defined phases, we construct QPO waveforms and phase-resolved spectra. By comparing the phase-folded waveform with that obtained from the Fourier method, we find that phase folding on the phase of the QPO fundamental frequency leads to a slight reduction in the contribution of the harmonic component. This suggests that the phase difference between QPO harmonics exhibits time variability. Phase-resolved spectral analysis reveals strong concurrent modulations of the spectral index and flux across the bright hard state. The modulation of the spectral index could potentially be explained by both the corona and jet precession models, with the latter requiring efficient acceleration within the jet. Furthermore, significant modulations in the reflection fraction are detected exclusively during the later stages of the bright hard state. These findings provide support for the geometric origin of LFQPOs and offer valuable insights into the evolution of the accretion geometry during the outburst in MAXI J1820+070.

show abstract

“…The LFQPOs in GRS 1915 + 105 have been intensively studied in the past (e.g. Reig et al 2000 ;Yan et al 2013 ;Ingram & van der Klis 2015 ;Zhang et al 2020 ;Liu et al 2021 ). The rms amplitude of the LFQPOs increases with energy and then gradually flattens, indicating that the energy that sustains the QPOs possibly originates from the hot corona (Yan et al 2013 ).…”

mentioning

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

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Testing Evolution of LFQPOs with Mass Accretion Rate in GRS 1915+105 with Insight-HXMT

Cited by 17 publications

References 61 publications

On the energy dependence of the QPO phenomenon in the black hole system MAXI J1535-571

On the energy dependence of the QPO phenomenon in the black hole system MAXI J1535-571

A Phase-resolved View of the Low-frequency Quasiperiodic Oscillations from the Black Hole Binary MAXI J1820+070

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

Contact Info

Product

Resources

About