Evolution of X-Ray Properties of MAXI J1535-571: Analysis with the TCAF Solution

Shang, Jie-Rou; Debnath, Dipak; Chatterjee, Debjit; Jana, Arghajit; Chakrabarti, Sandip K.; Chang, Hsiang-Kuang; Yap, Y. X. Jane; Chiu, C.-L.

doi:10.3847/1538-4357/ab0c1e

Cited by 59 publications

(23 citation statements)

References 46 publications

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“…The hydrogen column density was fixed to 3.2 × 10 22 cm −2 , the resulting value from fitting the spectrum in our sample with the highest net counts number. This value is consistent with previous estimates (Tao et al 2018;Kennea et al 2017;Stiele & Kong 2018;Shang et al 2019). Given that the cutoff energy of the Comptonised component lies outside of our energy range, we fixed the electron temperature.…”

Section: Energy Spectrasupporting

confidence: 91%

“…where the disc component dominates) and the X-ray variability decreases, reaching fractional rms amplitudes < 5 per cent. It is worth noting that quasi-periodic oscillations (QPOs) were detected during the main outburst of J1535 (Mereminskiy et al 2018;Stevens et al 2018;Huang et al 2018;Stiele & Kong 2018;Shang et al 2019;Sreehari et al 2019), however, we did not detect any significant QPO during the reflares. This result could potentially be related to differences in the physical conditions during the normal bright outburst and the fainter reflares or it could be that QPOs are too weak to be detected at the low count rates we ob-serve.…”

Section: Outburst Reflares Of Maxi J1535-571: the State Transition Identificationcontrasting

confidence: 66%

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A NICER look at the state transitions of the black hole candidate MAXI J1535−571 during its reflares

Cúneo

Alabarta

Zhang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The black hole candidate and X-ray binary MAXI J1535−571 was discovered in 2017 September. During the decay of its discovery outburst, and before returning to quiescence, the source underwent at least four reflaring events, with peak luminosities of ∼1035–36 erg s−1 (d/4.1 kpc)2. To investigate the nature of these flares, we analysed a sample of NICER (Neutron star Interior Composition Explorer) observations taken with almost daily cadence. In this work, we present the detailed spectral and timing analysis of the evolution of the four reflares. The higher sensitivity of NICER at lower energies, in comparison with other X-ray detectors, allowed us to constrain the disc component of the spectrum at ∼0.5 keV. We found that during each reflare the source appears to trace out a q-shaped track in the hardness–intensity diagram similar to those observed in black hole binaries during full outbursts. MAXI J1535−571 transits between the hard state (valleys) and softer states (peaks) during these flares. Moreover, the Comptonized component is undetected at the peak of the first reflare, while the disc component is undetected during the valleys. Assuming the most likely distance of 4.1 kpc, we find that the hard-to-soft transitions take place at the lowest luminosities ever observed in a black hole transient, while the soft-to-hard transitions occur at some of the lowest luminosities ever reported for such systems.

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Section: Energy Spectrasupporting

confidence: 91%

Section: Outburst Reflares Of Maxi J1535-571: the State Transition Identificationcontrasting

confidence: 66%

A NICER look at the state transitions of the black hole candidate MAXI J1535−571 during its reflares

Cúneo

Alabarta

Zhang

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Therefore, we do not include a few more recent BHXB sources in our search (e.g. Uttley et al 2018;Armas Padilla et al 2019;Shang et al 2019;Xu et al 2020). Calibrating the power colours across different instruments is an interesting problem to be considered in future works.…”

Section: Source Selectionmentioning

confidence: 99%

Evidence for an expanding corona based on spectral-timing modelling of multiple black hole X-ray binaries

Cao

Lucchini

Markoff

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Galactic black hole X-ray binaries (BHXBs) provide excellent laboratories to study accretion, as their relatively quick evolution allows us to monitor large changes in the in-flowing and/or out-flowing material over human timescales. However, the details of how the inflow-outflow coupling evolves during a BHXB outburst remain an area of active debate. In this work we attempt to probe the physical changes underlying the system evolution, by performing a systematic analysis of the multi-wavelength data of three BHXB sources: XTE J1752-223, MAXI J1659-152, and XTE J1650-500, during hard and hard-intermediate states. Using the power spectral hue which characterises the X-ray variability properties, we identify several clusters of BHXB epochs and perform the joint multi-wavelength spectral modelling to test their commonality with a physical jet model. Under the assumption that the corona is related to the base of the jet, we find that the power spectral hue traces the variation of the coronal radius (from ∼10Rg − ∼ 40Rg) in multiple BHXBs at hard and hard-intermediate states, and that the data are consistent with moderately truncated accretion discs (<25Rg) during hard-intermediate states. We also find that all epochs of low disc reflection have high hue located near the hard-intermediate to soft-intermediate state transition, indicating that in these states the vertical extent of the corona and/or its bulk speed are increasing. Our results link the geometrical similarity in the corona among multiple BHXB sources to their timing characteristics, and probe the corona responding to the disc-jet interactions at hard and intermediate states during outbursts.

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“…m h , X s , R) other than mass of the black hole (M BH ) and normalization (N). In the recent years, accretion flow dynamics around several black holes are studied quite successfully using TCAF model [45][46][47][48]. Frequencies of the dominating QPOs are predicted from the TCAF model fitted shock parameters [49].…”

Section: Hsmentioning

confidence: 99%

Study of Accretion Flow Dynamics of V404 Cygni during Its 2015 Outburst

et al. 2021

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The 2015 Outburst of V404 Cygni is an unusual one with several X-ray and radio flares and rapid variation in the spectral and timing properties. The outburst occurred after 26 years of inactivity of the black hole. We study the accretion flow properties of the source during its initial phase of the outburst using Swift/XRT and Swift/BAT data in the energy range of 0.5–150 keV. We have done spectral analysis with the two component advective flow (TCAF) model fits file. Several flow parameters such as two types of accretion rates (Keplerian disk and sub-Keplerian halo), shock parameters (location and compression ratio) are extracted to understand the accretion flow dynamics. We calculated equipartition magnetic field Beq for the outburst and found that the highest Beq∼900 Gauss. Power density spectra (PDS) showed no break, which indicates no or very less contribution of the Keplerian disk component, which is also seen from the result of the spectral analysis. No signature of prominent quasi-periodic oscillations (QPOs) is observed in the PDS. This is due to the non-satisfaction of the condition for the resonance shock oscillation as we observed mismatch between the cooling timescale and infall timescale of the post-shock matter.

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Evolution of X-Ray Properties of MAXI J1535-571: Analysis with the TCAF Solution

Cited by 59 publications

References 46 publications

A NICER look at the state transitions of the black hole candidate MAXI J1535−571 during its reflares

A NICER look at the state transitions of the black hole candidate MAXI J1535−571 during its reflares

Evidence for an expanding corona based on spectral-timing modelling of multiple black hole X-ray binaries

Study of Accretion Flow Dynamics of V404 Cygni during Its 2015 Outburst

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