Spectral and QPO Properties of GRO J1655-40 in the 2005 Outburst

Chakrabarti, Sandip K.; Nandi, A.; Debnath, Dipak; Sarkar, R.; Dutta, Broja Gopal

doi:10.22323/1.033.0103

Cited by 6 publications

(10 citation statements)

References 2 publications

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“…In Molla et al (2016), Jana et al (2016) and Chatterjee (2016), we successfully applied this constant normalization method to estimate masses of three MAXI transient compact objects, such as, MAXI J1659-152, MAXI 1836-194, and MAXI J1543-564 respectively. In Molla et al (2016, we also verified estimated mass of MAXI J1659-152 from that obtained by us using propagating oscillatory shock (POS) model (Chakrabarti et al 2005(Chakrabarti et al , 2008Debnath et al 2010Debnath et al , 2013. The successful interpretation of masses of these MAXI objects also motivated us to estimate mass of the well known transient BHC H 1743-322 using the same method.…”

Section: Introductionsupporting

confidence: 64%

Estimation of Mass of Compact Object in H 1743-322 From 2010 and 2011 Outbursts Using Tcaf Solution and Spectral Index–qpo Frequency Correlation

Molla

Chakrabarti

Debnath

et al. 2017

ApJ

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The well known black hole candidate H 1743-322 exhibited temporal and spectral variabilities during several outbursts. Daily variation of the accretion rates and the flow geometry change on a daily basis during each of the outbursts could be understood very well using the recent implementation of two component advective flow (TCAF) solution of the viscous transonic flow equations as an additive table model in XSPEC. This has dramatically improved our understanding about the accretion flow dynamics. Most interestingly, the solution allows to treat mass of the black hole candidate as a free parameter and there mass could be estimated from spectral fits. In this paper, we fit the data of two successive outbursts of H 1743-322 in 2010 and 2011 and studied evolutions of accretion flow parameters, such as, two component (Keplerian and sub-Keplerian) accretion rates, shock location (i.e., size of the Compton cloud), etc. We assume that the model Normalization remains the same accross the states in both these outbursts. We use this to estimate mass of the black hole and found that it comes out in the range of 9.25 − 12.86M ⊙ . For the sake of comparison, we also estimated mass using Photon index vs. QPO frequency correlation method which turns out to be 11.65 ± 0.67M ⊙ using GRO J1655-40 as reference source. Combining these two estimates, the most probable mass of the compact object becomes 11.21 +1.65 −1.96 M ⊙ .

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Section: Introductionsupporting

confidence: 64%

Estimation of Mass of Compact Object in H 1743-322 From 2010 and 2011 Outbursts Using Tcaf Solution and Spectral Index–qpo Frequency Correlation

Molla

Chakrabarti

Debnath

et al. 2017

ApJ

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“…The whole outburst eruption was a ‘double‐peaked’ profile where the first half is dominated by the power‐law emission and the second half is dominated by the soft emission from the Keplerian disc. This outburst behaviour is similar to the outburst behaviour of GRO J1655−40 during 1996 (Sobczak et al 2000a) and 2005 (Chakrabarti et al 2005, 2008; Shaposhnikov et al 2007). A total of 209 pointed observations using Proportional Counter Array (PCA) and High Energy X‐ray Timing Experiment (HEXTE) instruments on board the RXTE spanning 250 d covered the entire outburst of 1998–1999.…”

Section: Introductionsupporting

confidence: 75%

Evidence for two-component flows around the black hole candidate XTE J1550−564 from spectral features during its 1998-1999 outburst

Dutta

Chakrabarti

2010

Monthly Notices of the Royal Astronomical Society

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We study the spectral properties of the accretion disc in the Galactic black hole candidate XTE J1550−564 during the 1998-1999 outburst when the source exhibited double-peaked eruptions. This outburst lasted for 250 d and the 2.5-25.0 keV spectral state varied smoothly from one to another several times. We show that the spectral features of the 1998-1999 outburst could be clearly understood by a two-component (Keplerian and sub-Keplerian) advective flow (TCAF). We concentrate on the spectral data from a Proportional Counter Array instrument on the RXTE satellite for the black hole XTE J1550−564 and fit them quite satisfactorily using TCAF model. From the spectral fit we calculate the disc parameters, such as the Keplerian rate, the sub-Keplerian rate (halo rate), the shock location and the inner edge of the Keplerian disc. This observation points to the presence of two independent components in the accretion flow and that the accretion rate at all radii need not be constant in an evolving disc.

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“…This understanding also generally agrees with the observational results. Recent reporting of the outbursts of GRO 1655−40 showed a clear evidence of the QPO frequencies increasing monotonically from about 90 mHz to 17 Hz (Chakrabarti et al 2005) in a matter of 15 d and this could be easily fitted using the shock propagating at a constant velocity (Chakrabarti et al 2005).…”

Section: Discussionmentioning

confidence: 99%

Dissipative accretion flows around a rotating black hole

Das¹,

Chakrabarti²

2008

Monthly Notices of the Royal Astronomical Society

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We study the dynamical structure of a cooling dominated rotating accretion flow around a spinning black hole. We show that non-linear phenomena such as shock waves can be studied in terms of only three flow parameters, namely, the specific energy (${\cal E}$), the specific angular momentum ($\lambda$) and the accretion rate (${\dot m}$) of the flow. We present all possible accretion solutions. We find that a significant region of the parameter space in the ${\cal E}-\lambda$ plane allows global accretion shock solutions. The effective area of the parameter space for which the Rankine-Hugoniot shocks are possible is maximum when the flow is dissipation free. It decreases with the increase of cooling effects and finally disappears when the cooling is high enough. We show that shock forms further away when the black hole is rotating compared to the solution around a Schwarzschild black hole with identical flow parameters at a large distance. However, in a normalized sense, the flow parameters for which the shocks form around the rotating black holes are produced shocks closer to the hole. The location of the shock is also dictated by the cooling efficiency in that higher the accretion rate (${\dot m}$), the closer is the shock location. We believe that some of the high frequency quasi-periodic oscillations may be due to the flows with higher accretion rate around the rotating black holes.Comment: 9 pages, 7 figures. To appear in MNRA

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Spectral and QPO Properties of GRO J1655-40 in the 2005 Outburst

Cited by 6 publications

References 2 publications

Estimation of Mass of Compact Object in H 1743-322 From 2010 and 2011 Outbursts Using Tcaf Solution and Spectral Index–qpo Frequency Correlation

Estimation of Mass of Compact Object in H 1743-322 From 2010 and 2011 Outbursts Using Tcaf Solution and Spectral Index–qpo Frequency Correlation

Evidence for two-component flows around the black hole candidate XTE J1550−564 from spectral features during its 1998-1999 outburst

Dissipative accretion flows around a rotating black hole

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