Delayed outburst of H 1743–322 in 2003 and relation with its other outbursts

Chakrabarti, Sandip K.; Debnath, Dipak; Nagarkoti, Shreeram

doi:10.1016/j.asr.2019.02.014

Cited by 21 publications

(30 citation statements)

References 49 publications

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“…This faint X-ray activity of XTE J1908+094 in 2019 could be due to the sudden enhancement of viscosity and supply of matter from the pile-up radius. This type of behavior was observed in the case of H1743-322 [2] and GX 339-4 [52]. As the supply of residual matter from the previous outburst (2012-2013) was exhausted, the very short-term X-ray activity was also faded.…”

Section: Discussionmentioning

confidence: 71%

“…After a long period of quiescence, they show a sudden outburst. The sudden enhancement of viscosity at the piling radius could trigger the outburst [1][2][3]. The spectral and temporal properties of the source change during the outburst and evolves through the hard state (HS), hard intermediate state (HIMS), soft intermediate state (SIMS), and soft state (SS) [4][5][6].…”

Section: Introductionmentioning

confidence: 99%

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Properties of Faint X-ray Activity of XTE J1908+094 in 2019

et al. 2021

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We study the properties of the faint X-ray activity of Galactic transient black hole candidate XTE J1908+094 during its 2019 outburst. Here, we report the results of detailed spectral and temporal analysis during this outburst using observations from Nuclear Spectroscopic Telescope Array (NuSTAR). We have not observed any quasi-periodic-oscillations (QPOs) in the power density spectrum (PDS). The spectral study suggests that the source remained in the softer (more precisely, in the soft–intermediate) spectral state during this short period of X-ray activity. We notice a faint but broad Fe Kα emission line at around 6.5 keV. We also estimate the probable mass of the black hole to be 6.5−0.7+0.5M⊙, with 90% confidence.

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Section: Discussionmentioning

confidence: 71%

Section: Introductionmentioning

confidence: 99%

Properties of Faint X-ray Activity of XTE J1908+094 in 2019

et al. 2021

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“…The outburst must have been triggered at R 0 and the long duration of irradiation continued in the outburst for over 200 days. The 2004 outburst was possi-bly produced from the unused matter of 2003 (Chakrabarti et al 2019) and could continue to produce another long outburst, but one that is much weaker than the 2003 outburst. Whereas, the outbursts between 2008 and 2011 are more frequent, fainter outbursts with a duration of ∼60 days.…”

Section: Modelling the Evolution Of Accretion Parametersmentioning

confidence: 99%

Spectral and accretion evolution of H1743−322 during outbursts in RXTE era

Aneesha

Mandal

2020

A&A

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Aims. We study the spectral evolution of the H1743−322 during outbursts in the RXTE era. We aim to connect the variation of the spectral parameters with the accretion parameters along with the progress of the outbursts. We understand the evolution of the accretion parameters and hence the dynamics of the accretion process in light of the irradiated disc instability model. Methods. We provide a comprehensive study of all the outbursts of H1743−322 between 2003 and 2011. We performed spectral modelling of all the RXTE/PCA observations using phenomenological models. Also, we carried out spectral modelling by a hydrodynamic accretion flow model and estimated the accretion parameters. We applied the irradiated disc instability scenario in the presence of both Keplerian and sub-Keplerain accretion components to understand the evolution of accretion parameters. For this purpose, we propose a toy model for the time variation of the accretion rates following a powerlaw during outbursts. Results. All of the outbursts show spectral state transitions in the hardness-intensity diagram. The 2003 and 2004 outbursts are long-duration outbursts and relatively softer than the other outbursts. The 2008b and 2011 outbursts provide a unique opportunity to estimate the critical accretion rate (ṁdc) for triggering an outburst in this system within a narrow range of 0.076 < ṁdc < 0.086 (in Eddington units). In the absence of any dynamical measurement, we attempt to constrain a few orbital parameters of the system using an assumed mass and ṁdc in the range.

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“…This faint X-ray activity of XTE J1908+094 in 2019 could be due to the sudden enhancement of viscosity and supply of matter from the pile-up radius. This type of behavior has been observed in the case of H1743-322 [2] and GX 339-4 [52]. As the supply of residual matter from the previous outburst (2012-2013) was exhausted, the very short-term X-ray activity was also faded.…”

Section: Discussionmentioning

confidence: 56%

Properties of Faint X-ray Activity of XTE J1908+094 in 2019

Chatterjee,

Jana,

Chatterjee

et al. 2021

Preprint

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We study the properties of the faint X-ray activity of Galactic transient black hole candidate XTE J1908+094 during its 2019 outburst. Here, we report the results of detailed spectral and temporal analysis during this outburst using observations from Nuclear Spectroscopic Telescope Array (NuSTAR). We have not observed any quasi-periodic-oscillations (QPOs) in the power density spectrum (PDS). The spectral study suggests that the source remained in the softer (more precisely in soft-intermediate) spectral state during this short period of the X-ray activity. We notice a faint but broad Fe Kα emission line at around 6.5 keV. We also estimate the probable mass of the black hole to be 6.5 +0.5 −0.7 M with 90% confidence.

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Delayed outburst of H 1743–322 in 2003 and relation with its other outbursts

Abstract: of the next outburst could depend.

Cited by 21 publications

References 49 publications

Properties of Faint X-ray Activity of XTE J1908+094 in 2019

Properties of Faint X-ray Activity of XTE J1908+094 in 2019

Spectral and accretion evolution of H1743−322 during outbursts in RXTE era

Properties of Faint X-ray Activity of XTE J1908+094 in 2019

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