Accretion Flow Properties of Swift J1753.5-0127 during Its 2005 Outburst

Debnath, Dipak; Jana, Arghajit; Chakrabarti, Sandip K.; Chatterjee, Debjit; Mondal, Santanu

doi:10.3847/1538-4357/aa9077

Cited by 40 publications

(29 citation statements)

References 38 publications

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“…According to Bharali et al (2019), the orbital period of the source is 14.7 hrs. So, this nature of the non-observation of the softer spectral states is consistent with other short orbital period objects, such as MAXI J1836-194 (Jana et al 2016), Swift J1753.5-0127 (Debnath et al 2017), XTE J1118+480 . A similar presence of only HS during 2000 & 2005 outbursts of the short orbital period (∼ 4.1 hrs) transient BHC XTE J1118+480 was noticed (see, Debnath et al 2020).…”

Section: Discussionsupporting

confidence: 86%

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Accretion Flow Properties of GRS 1716-249 during its 2016-17 'failed' Outburst

Chatterjee,

Debnath,

Chatterjee

et al. 2021

Preprint

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In 2016 − 17, the Galactic transient black hole candidate GRS 1716-249 exhibited an outburst event after a long period of quiescence of almost 23 years. The source remained in the outbursting phase for ∼ 9 months. We study the spectral and temporal properties of the source during this outburst using archival data from four astronomy satellites, namely MAXI, Swift, NuSTAR and AstroSat. Initial spectral analysis is done using combined disk black body and power-law models. For a better understanding of the accretion flow properties, we studied spectra with the physical two component advective flow (TCAF) model. Accretion flow parameters are extracted directly from the spectral fits with the TCAF model. Low frequency quasi-periodic oscillations are also observed in the Swift/XRT and As-troSat/LAXPC data. From the nature of the variation of the spectral and temporal properties, we find the source remains in hard state during the entire outburst. It never had a transition to other states which makes this event a 'failed' outburst. An absence of the softer spectral states is consistent with the class of short orbital period objects, where the

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Section: Discussionsupporting

confidence: 86%

“…Depending upon the nature of outbursts, transient black hole candidates (BHCs) show two types of outburst, such as type-I and type-II (Debnath et al 2017). Those outbursts, where all four canonical spectral states are observed in the above mentioned sequence, are known as type-I or classical outburst.…”

Section: Introductionmentioning

confidence: 99%

Accretion Flow Properties of GRS 1716-249 during its 2016-17 'failed' Outburst

Chatterjee,

Debnath,

Chatterjee

et al. 2021

Preprint

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“…In the past two and half decades of the post RXTE era, GX 339-4 showed outbursts of both type-I & II. According to Debnath et al (2017), in type-I or complete outbursts, all four commonly identified spectral states (HS, HIMS, SIMS, SS) are found to form hysteresis loop, while in the type-II or harder spectral states, we do not see any soft spectral state. Sometimes even intermediate states are found to be missing in the type-II outbursts.…”

Section: Discussion and Concluding Remarksmentioning

confidence: 81%

Properties of 2017-18 'failed' Outburst of GX 339-4

Debnath¹,

Chatterjee²,

Nath³

et al. 2021

Preprint

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The Galactic transient black hole candidate GX 339-4 is a very interesting object to study as it showed both complete and failed types of outbursts. We studied both spectral and temporal properties of the 2017-18 outburst of the source using archival data of NICER and AstroSat instruments. This 2017-18 outburst is found to be failed in nature, as during the entire period of the outburst, the source was only in the hard spectral state. Source spectra were highly dominated with the non-thermal fluxes. When we tried to fit spectra with phenomenological models, most of the spectra were fitted with only the powerlaw model, and only six spectra required disk black body plus powerlaw models. While fitting spectra with the physical two-component advective flow (TCAF) model, we observed that the flow was highly dominated by the sub-Keplerian halo rate. The presence of stronger shock at a larger radius from the black hole was also observed during the rising and declining phases of the outburst. A prominent signature of 0.31 Hz QPO is observed with its four harmonics. Mass of the black hole was also estimated from our spectral analysis with the TCAF model as 11.24 +0.59 −1.25 M ⊙ .

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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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Accretion Flow Properties of Swift J1753.5-0127 during Its 2005 Outburst

Cited by 40 publications

References 38 publications

Accretion Flow Properties of GRS 1716-249 during its 2016-17 'failed' Outburst

Accretion Flow Properties of GRS 1716-249 during its 2016-17 'failed' Outburst

Properties of 2017-18 'failed' Outburst of GX 339-4

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

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