Study of the long-term evolution of the accretion dynamics of GX 339-4

Aneesha, U; Mandal, Samir; Sreehari, H.

doi:10.1093/mnras/stz1000

Cited by 22 publications

(19 citation statements)

References 78 publications

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“…We were not able to estimate t r and t h for the 2004, 2008a, and 2010a outbursts since the PCA observations are not available during the rising phase of these outbursts. It is also important to note that a time-lag between t h and t r is expected, and the same has been observed (Yu et al 2004;Aneesha et al 2019) in many outbursting sources. But it is difficult to detect this time-lag for H1743−322 as the outbursts rising time is short (∼10 days), and the closest interval between successive PCA observations are of the order of a day.…”

Section: Modelling the Evolution Of Accretion Parameterssupporting

confidence: 58%

“…GX 339−4 belongs to the first category, whereas H1743−322 is an example of the latter category. Tetarenko et al (2018a,b) fitted the lightcurves of GX 339−4 and estimated the viscosity parameters, whereas Aneesha et al (2019) unified all of the outbursts of GX 339−4 and studied the evolution of accretion parameters using irradiated DIM. Recently, Mondal (2020) determined the lightcurve decay time scale and viscosity parameter of the outbursting XRBs.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Modelling the Evolution Of Accretion Parameterssupporting

confidence: 58%

Section: Introductionmentioning

confidence: 99%

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

Aneesha

Mandal

2020

A&A

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“…A good linear relation between the outbursts and the quiescence phases is found from their analysis. A similar long-term variability of the source was also studied by Aneesha et al (2019). In the past two and half decades of the post RXTE era, GX 339-4 showed outbursts of both type-I & II.…”

Section: Discussion and Concluding Remarksmentioning

confidence: 69%

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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“…Similarly, the Swift/XRT spectra are extracted following Radhika et al (2018). The energy spectra thus extracted are modelled using phabs(diskbb+smedge×powerlaw) following Radhika & Nandi (2014) and Aneesha et al (2019). The total flux in 3 − 20 keV corresponding to the best fitting model is used to generate the HID.…”

Section: Spectral Analysis and Modellingmentioning

confidence: 99%

“…During the RXTE era, it has gone into multiple outbursts in , 2002, 2007(Sreehari et al 2019a). We use complete q-diagrams during 2002, 2007(Belloni et al 2005Nandi et al 2012;Aneesha et al 2019) to classify the spectral states with the aid of K-Means clustering algorithm. The EVRs for the parameters considered for all outbursts are tabulated in Table 2.…”

Section: Xte J1859+226: 1999 Outburstmentioning

confidence: 99%

A Machine Learning approach for classification of accretion states of Black hole binaries

Sreehari,

Nandi

2021

Preprint

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Study of the long-term evolution of the accretion dynamics of GX 339-4

Cited by 22 publications

References 78 publications

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

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

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

A Machine Learning approach for classification of accretion states of Black hole binaries

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