Broadband Variability Study of Maxi J1631-479 in Its Hard-intermediate State Observed with Insight-HXMT

Bu, Q. C.; Zhang, S. N.; Santangelo, A.; Belloni, T.; Zhang, L.; Qu, J. L.; Tao, Lian; Huang, Y.; Ma, Xiang; Li, Z. S.; Zhang, S.; Chen, L.; Cai, C.; Cao, X. L.; Chang, Zhi; Chen, T. X.; Chen, Y.; Chen, Y. P.; Cui, Wei; Du, Yongzhai; Gao, G. H.; Ge, M. Y.; Gu, Y. D.; Guan, J.; Guo, Chengcheng; Han, Danxiang; Jia, Haiqiang; Jia, S.; Jiang, Weichun; Jin, J.; Kong, L. D.; Li, B.; Li, C. K.; Li, G.; Li, T. P.; Li, W.; Li, X.; Li, X. B.; Li, X. F.; Li, Z. W.; Liang, X. H.; Liao, J. Y.; Liu, C. Z.; Liu, H. X.; Liu, Han–Wen; Liu, X. J.; Lu, X. F.; Luo, Q.; Luo, T.; Ma, Ruican; Meng, Bin; Nang, Y.; Nie, J. Y.; Ou, G.; Sai, N.; Song, L. M.; Song, X. Y.; Sun, Liang; Tan, Ying; Tuo, Y. L.; Wang, C.; Wang, L. J.; Wang, P. J.; Wang, W. S.; Wang, Y. S.; Wen, Xiang-Yang; Wu, B. Y.; Wu, B. B.; Wu, Mei‐Hwan; Xiao, G. C.; Xiao, Shuo; Xiong, S. L.; Xu, Y. P.; Yang, S.; Yang, Yi-Jung; Yi, Q. B.; Yin, Q. Q.; You, Y.; Zhang, Faming; Zhang, H. M.; Zhang, J.; Zhang, P.; Zhang, W. C.; Zhang, W.; Zhang, Y. F.; Zhang, Y. H.; Zhao, H. S.; Zhao, Xiaofan; Zheng, S.; Zhou, D. K.

doi:10.3847/1538-4357/ac11f5

Cited by 26 publications

(21 citation statements)

References 52 publications

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“…The study of the energy-dependent timing properties in the BHTs provides important insights to differentiate the properties of the intermediate states from those of the soft states. The appearance of the type C QPOs is one of the most salient features seen in the HIMS; therefore, the study of these QPOs acts as an important tool to further investigate the characteristics of BHTs in the HIMS (Bu et al 2021). Although the exact physical origin of these QPOs is still not clear, sufficient indications have been found in support of the geometric origin of the type C QPOs (Gilfanov 2010).…”

Section: Discussion and Concluding Remarksmentioning

confidence: 99%

“…Flux is in units of erg cm −2 s −1 . (Belloni et al 2011), Cyg X-1, XTE 1752-223 (Muñoz-Darias et al 2010), GRS 1915+105 (Rodriguez et al 2004Yan et al 2012;Yadav et al 2016b;Rawat et al 2019;Zhang et al 2020;Karpouzas et al 2021), XTE J1650-500 (Gierlinski & Zdziarski 2005), XTE J1859+226 (Casella et al 2004), H1743-322 (Li et al 2013a), XTE J1550-564 (Li et al 2013b), and MAXI J1631-479 (Bu et al 2021), where an increase in the amplitude of the fractional variability up to ∼10 keV and then a flattening or decrease has been found. This increase in the fractional rms of the QPOs with photon energy (positive correlation) is usually found in the intermediate states, and the positive correlation implies the origin of the QPOs from the coronal region (see Li et al 2013aLi et al , 2013b With respect to the 3-5 keV band, the decreasing trend in the time lags with energy estimated at the QPOs and the subharmonic frequencies (see Figure 7) implies the presence of a soft or negative lag, where the hard photons arrive before the soft ones.…”

Section: Discussion and Concluding Remarksmentioning

confidence: 99%

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AstroSat View of the Newly Discovered X-Ray Transient MAXI J1803–298 in the Hard-intermediate State

Chand

Dewangan

Thakur

et al. 2022

ApJ

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We perform comprehensive temporal and spectral analysis of the newly discovered X-ray transient MAXI J1803–298 using an AstroSat target of opportunity observation on 2021 May 11 during its outburst. The source was found to be in the hard-intermediate state. We detect type C quasi-periodic oscillations (QPOs) at the frequencies of ∼5.4 and ∼6.3 Hz along with a subharmonic at ∼2.8 Hz in the 3–15 keV band. The frequency and fractional rms amplitude of the QPO in the 15–30 keV band are found to be higher than those in the 3–15 keV band. We find soft lags of ∼3.8 and ∼6.8 ms for the respective QPOs at ∼5.4 and ∼6.3 Hz, whereas a soft lag of ∼4.7 ms is found at the subharmonic frequency. The increase in the soft lags at the QPO frequencies with energy is also observed in other black hole transients and attributed to the inclination dependence of the lags. The rms energy spectra indicate the power-law component to be more variable than the disk and reflection components. We find a broad iron line with an equivalent width of ∼0.17–0.19 keV and a reflection hump above ∼12 keV in the energy spectrum. Based on the X-ray spectroscopy and considering the distance to the source as 8 kpc, the estimated mass (∼8.5–16 M ⊙) and spin (a ≳ 0.7) of the black hole suggest that the source is likely to be a stellar mass Kerr black hole X-ray binary.

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Section: Discussion and Concluding Remarksmentioning

confidence: 99%

Section: Discussion and Concluding Remarksmentioning

confidence: 99%

AstroSat View of the Newly Discovered X-Ray Transient MAXI J1803–298 in the Hard-intermediate State

Chand

Dewangan

Thakur

et al. 2022

ApJ

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show abstract

“…The propagation of fluctuations in mass accretion rate may also give rise to the observed variability (Ingram & van der Klis 2013). Alternatively, if the coronal fluctuation is giving rise to the observed variability, in that case, the decrease in variability at the high energy can be due to the non-thermal acceleration in the hot plasma (Zdziarski et al 1990;Bu et al 2021). This effect is dominated by Compton cooling, resulting in decreased variability in the higher energy range (Gierlinski & Zdziarski 2005).…”

Section: Timing Studiesmentioning

confidence: 99%

Probing spectral and temporal evolution of the neutron star low-mass X-ray binary 4U 1724-30 with AstroSat

Kashyap,

Chakraborty,

Bhattacharyya

2022

Preprint

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We report the broadband spectro-temporal study of the poorly studied accreting neutron star (NS) low mass X-ray binary (LMXB) 4U 1724-30 using data from Soft X-ray Telescope (SXT) and Large Area X-ray Proportional Counters (LAXPC) instruments on board AstroSat. The dim persistent LMXB source was observed with AstroSat over 4 epochs in 2017, all of which corresponded to a low-luminosity non-thermal emission dominated (hard/island) emission state with modest spectral evolution. All the X-ray broadband spectra can be modelled by a combination of thermal emission from the NS boundary layer (BL) or NS surface and a non-thermal emission component possibly originating from the inverse Comptonization of the disc seed photons. We investigate the presence of frequency and energy-dependent variabilities to probe the origin of the disc/coronal fluctuations. We also report the detection of a Type-I X-ray burst displaying a photospheric radius expansion (PRE). During the burst, a hard Xray shortage in the 30-80 keV energy band and the enhancement of the persistent emission reveal the burst feedback on the overall accretion process. Using the touch-down burst flux ∼ 4.25 × 10 −8 erg s −1 cm −2 , the distance of the source is estimated as ∼ 8.4 kpc.

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“…Type-C QPOs often appear when the source is in the low-hard state and the hard-intermediate state, with central frequency in the range ∼ 0.1-15 Hz and associated strong broadband noise in the PDS (Casella et al 2005). The rms amplitude of the type-C QPOs can increase with energy, and reach ∼ 15% at 100 keV (e.g., Huang et al 2018;Bu et al 2021), indicating that the radiative mechanism of the type-C QPO has to be related to the corona.…”

Section: Introductionmentioning

confidence: 99%

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

Zhang,

Méndez,

García

et al. 2022

Preprint

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Type-C quasi-periodic oscillations (QPOs) in black hole X-ray transients can appear when the source is in the low-hard and hard-intermediate states. The spectral-timing evolution of the type-C QPO in MAXI J1535−571 has been recently studied with Insight-HXMT. Here we fit simultaneously the time-averaged energy spectrum, using a relativistic reflection model, and the fractional rms and phase-lag spectra of the type-C QPOs, using a recently developed time-dependent Comptonization model when the source was in the intermediate state. We show, for the first time, that the time-dependent Comptonization model can successfully explain the X-ray data up to 100 keV. We find that in the hard-intermediate state the frequency of the type-C QPO decreases from 2.6 Hz to 2.1 Hz, then increases to 3.3 Hz, and finally increases to ∼ 9 Hz. Simultaneously with this, the evolution of corona size and the feedback fraction (the fraction of photons up-scattered in the corona that return to the disc) indicates the change of the morphology of the corona. Comparing with contemporaneous radio observations, this evolution suggests a possible connection between the corona and the jet when the system is in the hard-intermediate state and about to transit into the soft-intermediate state.

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Broadband Variability Study of Maxi J1631-479 in Its Hard-intermediate State Observed with Insight-HXMT

Cited by 26 publications

References 52 publications

AstroSat View of the Newly Discovered X-Ray Transient MAXI J1803–298 in the Hard-intermediate State

AstroSat View of the Newly Discovered X-Ray Transient MAXI J1803–298 in the Hard-intermediate State

Probing spectral and temporal evolution of the neutron star low-mass X-ray binary 4U 1724-30 with AstroSat

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

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