Accretion flow properties of XTE J1118+480 during its 2005 outburst

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

doi:10.1088/1674-4527/20/11/175

Cited by 15 publications

(8 citation statements)

References 47 publications

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“…) could be seen in the intermediate shock strength, i.e., in the intermediate states (see, Chakrabarti 1999a). This is what we see during the present outburst as well as earlier studied two BHCs (Swift J1753.5-0127 and MAXI J1836-194) by our group (Jana et al 2017(Jana et al , 2020.…”

Section: Discussion and Concluding Remarkssupporting

confidence: 92%

Jet Properties of XTE J1752-223 During its 2009-2010 Outburst

Debnath,

Chatterjee,

Chatterjee

et al. 2021

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Galactic short orbital period black hole candidate (BHC) XTE J1752-223 was discovered on 2009 Oct 21 by the Rossi X-ray Timing Explorer (RXTE). We study the spectral properties of this outburst using transonic flow solution based two component advective flow (TCAF) model. TCAF model fitted spectrum gives an estimation of the physical flow parameters, such as the Keplerian disk rate, sub-Keplerian halo rate, properties of the so-called Compton cloud, other than the mass of the source and normalization ( ). is a standardized ratio of emitted to observed photon flux in TCAF which does not include X-ray emission from jets. In the presence of jets, this ratio changes and this deviation is used to obtain the estimation of X-ray contribution from the jets. Nature of the jet is found to be compact during low luminous hard state and discrete or blobby during high luminous intermediate states. We find a correlation between the radio (5.5 GHz) and X-ray (2.5 − 25 keV) fluxes from different components. The radio ( ) and jet X-ray ( ) fluxes are found to be correlated within the acceptable range of the standard correlation (0.6 to 0.7). A similar correlation indices were reported by our group for three other short orbital period transient BHCs (Swift J1753.5-0127, MAXI J1836-194 & XTE J1118+480).

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Section: Discussion and Concluding Remarkssupporting

confidence: 92%

Jet Properties of XTE J1752-223 During its 2009-2010 Outburst

Debnath,

Chatterjee,

Chatterjee

et al. 2021

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“…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: 60%

“…are present. Recently, after its (TCAF) inclusion as an additive table model in XSPEC (Debnath et al 2014(Debnath et al , 2015a, spectra of many BHC have been successfully fitted and described by our group (Debnath et al 2015a(Debnath et al ,b,2017(Debnath et al ,2020Mondal et al 2014Mondal et al , 2016Chatterjee et al 2016Chatterjee et al ,2019Jana et al 2016Jana et al ,2020aChatterjee et al 2020, Shang et al 2019. Estimation of mass of these sources has also been done using the TCAF model.…”

Section: Introductionmentioning

confidence: 99%

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

Chatterjee,

Debnath,

Chatterjee

et al. 2021

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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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“…Since in HR, we use two fixed energy band photon rates/fluxes, transition dates between the spectral states may not be same, i.e., may differ slightly when we confirm from the spectral analysis with phenomenological (for e.g., disk black body plus power-law models) or physical models, such as TCAF solution, developed by Chakrabarti and his collaborators (Chakrabarti & Titarchuk 1995;Chakrabarti 1997). TCAF model has successfully designated the spectral states of many black hole candidates during their outbursts (Nandi et al 2012;Debnath et al 2013Debnath et al , 2014Debnath et al , 2015aDebnath et al ,b, 2017Debnath et al , 2020Mondal et al 2014Mondal et al , 2016Chatterjee et al 2016Chatterjee et al , 2019Chatterjee et al , 2020Jana et al 2016Jana et al , 2020Shang et al 2019). However, according to literature (see for example, Debnath et al 2008;Nandi et al 2012 and references therein) it is believed that in the harder states HR values are higher and in the softer states HR values are low.…”

Section: Calculation Of Softer State Durationmentioning

confidence: 64%

Relation Between Quiescence and Outbursting Properties of GX 339-4

Bhowmick,

Debnath,

Chatterjee

et al. 2021

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Galactic black hole candidate (BHC) GX 339-4 underwent several outbursting phases in the past two and a half decades at irregular intervals of 2 − 3 years. Nature of these outbursts in terms of the duration, number of peaks, maximum peak intensity, etc. varies. We present a possible physical reason behind the variation of outbursts. From a physical point of view, if the supply of matter from the companion is roughly constant, the total energy release in an outburst is expected to be proportional to the quiescence period prior to the outburst when the matter is accumulated. We use archival data of RXTE/ASM from January 1996 to June 2011, and MAXI/GSC from August 2009 to July 2020 data. Initial five outbursts of GX 339-4 between 1997 and 2011 were observed by ASM and showed a good linear relation between the accumulation period and the amount of energy released in each outburst, but the outbursts after 2013 behaved quite differently. The 2013, 2017 − 18, and 2018 − 19 outbursts were of short duration, and incomplete or 'failed' in nature. We suggest that the matter accumulated during the quiescence periods prior to these outbursts were not cleared through accretion due to lack of viscosity. The leftover matter was cleared in the immediate next outbursts. Our study thus sheds light on long term accretion dynamics in outbursting sources.

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Accretion flow properties of XTE J1118+480 during its 2005 outburst

Cited by 15 publications

References 47 publications

Jet Properties of XTE J1752-223 During its 2009-2010 Outburst

Jet Properties of XTE J1752-223 During its 2009-2010 Outburst

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

Relation Between Quiescence and Outbursting Properties of GX 339-4

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