Accretion flow properties of GRS 1716-249 during its 2016–17 ‘failed’ outburst

Chatterjee, Kabita; Debnath, Dipak; Chatterjee, Debjit; Jana, Arghajit; Nath, Sujoy Kumar; Bhowmick, Riya; Chakrabarti, Sandip K.

doi:10.1007/s10509-021-03967-x

Cited by 11 publications

(13 citation statements)

References 45 publications

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“…NS systems, on the contrary, can show variability up to 500-1000 Hz. The lack of X-ray pulsations and kilo-herz QPOs in the PDS (typical signatures of neutron star systems), the presence of type-C and type-B QPOs in the PDS of GRS 1716−249 (Chatterjee et al 2021), and the strong decline of the power spectra below 10 Hz all reinforce the identification of the compact object as a BH.…”

Section: Bh Nature Of Grs 1716−249mentioning

confidence: 83%

“…In addition to the previous evidence, the X-ray timing properties of GRS 1716−249 also suggest that the compact object of the system is a BH. Chatterjee et al (2021) report different power density spectra (PDS) of GRS 1716−249 in their Fig. 4, all of which show a strong decline from ∼3 Hz to 10 Hz.…”

Section: Bh Nature Of Grs 1716−249mentioning

confidence: 99%

“…An analysis of the broadband (1-78 keV) X-ray spectra of the source taken by NuSTAR and Swift constrained the accretion disk density parameter of GRS 1716−249 to be in the range of 10 19 -10 20 cm −3 (Jiang et al 2017). Recently, the black hole mass was claimed to lie in the range of 4.5-5.9 M according to a two-component advective flow (TCAF) model (Chatterjee et al 2021), although this method uses model-dependent spectral fitting of the source to obtain these values.…”

Section: System Parameters Of Grs 1716−249mentioning

confidence: 99%

“…Later, Tao et al (2019) studied three quasi-simultaneous NuSTAR and Swift datasets of the system in its hard intermediate state, and assuming a distance of 2.4 kpc, constrained the upper limit for the compact object mass to be <8.0 M , at a 90% confidence level. Chatterjee et al (2021) also used X-ray spectral analysis of the source during outburst to suggest a BH nature of the compact object. They fitted the X-ray spectra of GRS 1716−249 with the physical two-component advective flow (TCAF) model, keeping the mass of the primary as a free parameter, and constrained the mass of the compact object in the range of 4.5-5.9 M , but the values obtained are highly modeldependent and very unlikely to be a realistic range.…”

Section: Bh Nature Of Grs 1716−249mentioning

confidence: 99%

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A multi-wavelength study of GRS 1716-249 in outburst : constraints on its system parameters

Saikia,

Russell,

Baglio

et al. 2022

Preprint

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We present a detailed study of the evolution of the Galactic black hole transient GRS 1716−249 during its 2016-2017 outburst at optical (Las Cumbres Observatory), mid-infrared (Very Large Telescope), near-infrared (Rapid Eye Mount telescope), and ultraviolet (the Neil Gehrels Swift Observatory Ultraviolet/Optical Telescope) wavelengths, along with archival radio and X-ray data. We show that the optical/near-infrared and UV emission of the source mainly originates from a multi-temperature accretion disk, while the mid-infrared and radio emission are dominated by synchrotron emission from a compact jet. The optical/UV flux density is correlated with the X-ray emission when the source is in the hard state, consistent with an X-ray irradiated accretion disk with an additional contribution from the viscous disk during the outburst fade. We find evidence for a weak, but highly variable jet component at mid-infrared wavelengths. We also report the long-term optical light curve of the source and find that the quiescent i -band magnitude is 21.39±0.15 mag. Furthermore, we discuss how previous estimates of the system parameters of the source are based on various incorrect assumptions, and so are likely to be inaccurate. By comparing our GRS 1716−249 data-set to those of other outbursting black hole X-ray binaries, we find that while GRS 1716−249 shows similar X-ray behaviour, it is noticeably optically fainter, if the literature distance of 2.4 kpc is adopted. Using several lines of reasoning, we argue that the source distance is further than previously assumed in the literature, likely within 4-17 kpc, with a most likely range of ∼ 4-8 kpc.

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Section: Bh Nature Of Grs 1716−249mentioning

confidence: 83%

Section: Bh Nature Of Grs 1716−249mentioning

confidence: 99%

Section: System Parameters Of Grs 1716−249mentioning

confidence: 99%

Section: Bh Nature Of Grs 1716−249mentioning

confidence: 99%

See 2 more Smart Citations

A multi-wavelength study of GRS 1716-249 in outburst : constraints on its system parameters

Saikia,

Russell,

Baglio

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…Additionally, a mass parameter, giving the mass of the BH, and one normalization factor (that gives the ratio of emitted to observed X-ray spectrum) are also needed. One can obtain the best fitted values of these physical parameters which are directly related to the accretion process and infer on the accretion dynamics, as has been done for several BH candidates (Debnath et al 2017;Mondal et al 2016;Chatterjee et al 2020;Shang et al 2019;Chatterjee et al 2021). Intrinsic source parameters, such as the mass of the BH (Molla et al 2016(Molla et al , 2017Chatterjee et al 2016Chatterjee et al , 2019Chatterjee et al 2020;Jana et al 2016 and jet/outflow X-ray flux (Jana et al 2017;) also has been estimated from spectral analysis with the TCAF model.…”

mentioning

confidence: 99%

Accretion Flow Properties of MAXI J1910-057/Swift J1910.2-0546 During Its 2012-13 Outburst

Nath,

Debnath,

Chatterjee

et al. 2021

Preprint

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Galactic black hole candidate MAXI J1910-057/Swift J1910.2-0546 was simultaneously discovered by MAXI/GSC and Swift/BAT satellites during its first outburst in 2012. We study detailed spectral and temporal properties of the source in a broad energy range using archival data from Swift/XRT, MAXI/GSC and Swift/BAT instruments. Low frequency quasi periodic oscillations are observed on several instances of observations. The combined 1-50 keV spectra are analyzed using the transonic flow solution based Two Component Advective Flow (TCAF) model. Based on the variation of soft and hard X-ray fluxes, their hardness ratios and the variation of the spectral model parameters, we found that the source has evolved through six spectral states, which is unusual in the case of transient black holes. We interpret this unusual spectral state evolution to be a result of two overlapping outbursts where the leftover matter from a primary outburst is released from the pile-up radius due to a sudden rise of viscosity causing a secondary outburst. From the spectral analysis with TCAF model, we estimate the mass of the black hole to be 9.98 +3.54 −3.09 M ⊙ , and the source distance is estimated to be 4.6 − 14.6 kpc from transition luminosity considerations. Keywords: X-ray binary stars(1811) -X-ray transient sources(1852) -Black holes(162) -Black hole physics(159) -Accretion(14) a UT Date in mm-dd format. b TCAF model fitted spectral parameters are shown in columns (6)-(12). NH values are in 10 22 atoms per cm −2 . c χ 2 values and degrees of freedom (dof) of the TCAF spectral model fits are shown in columns (13).Notes. Superscripts on the parameter values represent average error values obtained using the err task in XSPEC with 90% confidence.

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Accretion flow properties of MAXI J1910-057/Swift J1910.2–0546 during its 2012–13 outburst

Nath

Debnath

Chatterjee

et al. 2023

Advances in Space Research

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Accretion flow properties of GRS 1716-249 during its 2016–17 ‘failed’ outburst

Cited by 11 publications

References 45 publications

A multi-wavelength study of GRS 1716-249 in outburst : constraints on its system parameters

A multi-wavelength study of GRS 1716-249 in outburst : constraints on its system parameters

Accretion Flow Properties of MAXI J1910-057/Swift J1910.2-0546 During Its 2012-13 Outburst

Accretion flow properties of MAXI J1910-057/Swift J1910.2–0546 during its 2012–13 outburst

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