Characterization of GX 339-4 outburst of 2010–11: analysis by xspec using two component advective flow model

Debnath, Dipak; Mondal, Santanu; Chakrabarti, Sandip K.

doi:10.1093/mnras/stu2588

Cited by 78 publications

(82 citation statements)

References 60 publications

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“…3 of Debnath et al (2015a) it is shown that there is a time delay of ∼ 7 days between the peaks of the advective and Keplerian disk components in the 2010-11 outburst of GX339-4. This is interpreted to be due to the viscous time delay of the Keplerian component.…”

Section: -11 Outburst Of Gx339-4mentioning

confidence: 97%

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Viscosity parameter in dissipative accretion flows with mass outflow around black holes

Nagarkoti

Chakrabarti

2016

Mon. Not. R. Astron. Soc.

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Numerical hydrodynamic simulation of inviscid and viscous flows have shown that significant outflows could be produced from the CENtrifugal pressure supported BOundary Layer or CENBOL of an advective disk. However, this barrier is weakened in presence of viscosity, more so, if there are explicit energy dissipations at the boundary layer itself. We study effects of viscosity and energy dissipation theoretically on the outflow rate and show that as the viscosity or energy dissipation (or both) rises, the prospect of formation of outflows is greatly reduced, thereby verifying results obtained through observations and numerical simulations. Indeed, we find that in a dissipative viscous flow, shocks in presence of outflows can be produced only if the Shakura-Sunyaev viscosity parameter α is less than 0.2. This is a direct consequence of modification of the Rankine-Hugoniot relation across the shock in a viscous flow, when the energy dissipation and mass loss in the form of outflows from the post-shock region are included. If we ignore the effects of mass loss altogether, the standing dissipative shocks in viscous flows may occur only if α < 0.27. These limits are tighter than the absolute limit of α = 0.3 valid for a situation when the shock itself neither dissipates energy nor any outflow is formed. We compute typical viscosity parameters required to understand spectral and temporal properties of several black hole candidates such as GX399-4, MAXI J1659-152 and MAXI J1836-194 and find that required α are indeed well within our prescribed limit.

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Section: -11 Outburst Of Gx339-4mentioning

confidence: 97%

“…The general behaviour of the physical parameters have been discussed in Debnath et al (2015a). They analysed the data of 2010-11 outburst of GX339-4 using two component advective flow model of CT95.…”

Section: Estimation Of α During Outbursts Of Various Sourcesmentioning

confidence: 99%

Viscosity parameter in dissipative accretion flows with mass outflow around black holes

Nagarkoti

Chakrabarti

2016

Mon. Not. R. Astron. Soc.

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“…We analyze archival data of the RXTE PCA instrument using HEASARC's software package HeaSoft version HEADAS 6.15 and follow the standard data analysis techniques (2,16,17) to analyze the PCA data. For timing analysis we use PCA Event mode data with a maximum timing resolution of 125μs.…”

Section: Observation and Data Analysismentioning

confidence: 99%

Temporal and spectral properties of MAXI J1659-152 during its 2010 outburst

Molla¹,

Debnath²,

Chakrabarti³

et al. 2017

The Fourteenth Marcel Grossmann Meeting

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Transient black hole candidate MAXI J1659-152 showed rapid spectral and temporal evolution during its very first outburst. Our understanding about accretion flow dynamics around black hole candidates has improved much more after the inclusion of Chakrabarti-Titarchuk Two Component Advective Flow (TCAF) model as an additive table model in XSPEC. In this paper we make a detail study of temporal and spectral properties of black hole candidate MAXI J1659-152 during its 2010 outburst with TCAF and POS model. From our fit, we extract accretion flow parameters (Keplerian disk and sub-Keplerian halo rates, shock location, shock strength). We find mass of the object to be 4.17-7.74 M .

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“…Exactly opposite scenario is observed during declining phase. Recently, 19,13,15,16 also showed physical reason behind spectral state transitions from spectral model fitted parameters of TCAF model for two different Galactic BHCs H1743-322, GX 339-4 and MAXI J1659-152 during their outbursts. QPOs frequencies are then obtained from shock locations which are obtained from the TCAF fitting.…”

Section: Introductionmentioning

confidence: 97%

Study of shock propagation velocity and accretion flow dynamics around the black hole candidate H1743-322

Mondal¹,

Chakrabarti²,

Debnath³

et al. 2017

The Fourteenth Marcel Grossmann Meeting

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The inner region of a transient source is cooled down by the inverse Comptonization of soft photons from the Keplerian disk component. The reduction of pressure forces the outer boundary of the Compton cloud, namely, the centrifugal pressure supported shock to move inward slowly in order to satisfy Rankine-Hugoniot conditions. We consider the transient source H1743-322 to study this movement of the shock. The presence of cooling changes the geometry of the Compton cloud gradually. We also see how the flow parameters of this source change day by day during a complete outburst. As the shock-oscillation could also modulate harder X-rays, we want to resolve the question: are QPOs originated from shock oscillations and can the time variation of the QPO frequency be explained by this slow propagation of the shock? For that we solve the Rankine-Hugoniot conditions and derive the condition of shock formation in presence of Compton cooling. We also compute inward velocity of the shock Compton cloud to be a few meters per second, which agrees well with earlier observational results.

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Characterization of GX 339-4 outburst of 2010–11: analysis by xspec using two component advective flow model

Cited by 78 publications

References 60 publications

Viscosity parameter in dissipative accretion flows with mass outflow around black holes

Viscosity parameter in dissipative accretion flows with mass outflow around black holes

Temporal and spectral properties of MAXI J1659-152 during its 2010 outburst

Study of shock propagation velocity and accretion flow dynamics around the black hole candidate H1743-322

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