Resonance Oscillation of Radiative Shock Waves in Accretion Disks around Compact Objects

Molteni, D.; Sponholz, H.; Chakrabarti, Sandip K.

doi:10.1086/176775

Cited by 266 publications

(288 citation statements)

References 17 publications

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“…While it has been reported that QPOs can also be generated by cooling (Molteni et al 1996b). In realistic disc, both processes are active, and both should produce shock oscillation.…”

Section: Discussion and Concluding Remarksmentioning

confidence: 97%

“…Hot electrons in the post-shock region, abbreviated as CENBOL (CENtrifugal pressure supported Boundary Layer), may explain the power-law tail of the spectrum from black hole candidates in hard states, while a weak or no shock solution produces a dearth of hot electrons which may cause the weaker power-law tail in the soft states (Chakrabarti & Titarchuk 1995;Mandal & Chakrabarti 2010). Moreover, a large number of authors have shown the formation of bipolar outflows from the post-shock accretion flow, both numerically (Molteni et al 1994(Molteni et al , 1996b as well as analytically (Le & Becker 2005;Chattopadhyay & Das 2007;Fukumura & Kazanas 2007;Das & Chattopadhyay 2008;Das et al 2009;Kumar et al , 2014. It is also interesting to note that, by considering a simplified inviscid accretion, and which has the right parameters to form a standing shock, Das et al (2001) qualitatively showed that there would be no jets in no-shock or weak shock condition of the disc, or in other words, when the disc is in the soft spectral state.…”

Section: Introductionmentioning

confidence: 99%

“…Molteni et al (1996b), considered bremsstrahlung cooling of an inviscid flow, and reported there is significant oscillation of the post-shock region. Since the post-shock flow is of higher density and temperature compared to the pre-shock flow, the cooling rates are higher.…”

Section: Introductionmentioning

confidence: 99%

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Periodic mass loss from viscous accretion flows around black holes

Das

Chattopadhyay

Nandi

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We investigate the behaviour of low angular momentum viscous accretion flows around black holes using Smooth Particle Hydrodynamics (SPH) method. Earlier, it has been observed that in a significant part of the energy and angular momentum parameter space, rotating transonic accretion flow undergoes shock transition before entering in to the black hole and a part of the post-shock matter is ejected as bipolar outflows, which are supposed to be the precursor of relativistic jets. In this work, we simulate accretion flows having injection parameters from the inviscid shock parameter space, and study the response of viscosity on them. With the increase of viscosity, shock becomes time dependent and starts to oscillate when the viscosity parameter crosses its critical value. As a result, the in falling matter inside the post-shock region exhibits quasi-periodic variations and causes periodic ejection of matter from the inner disc as outflows. In addition, the same hot and dense post-shock matter emits high energy radiation and the emanating photon flux also modulates quasi-periodically. Assuming a ten solar mass black hole, the corresponding power density spectrum peaks at the fundamental frequency of few Hz followed by multiple harmonics. This feature is very common in several outbursting black hole candidates. We discuss the implications of such periodic variations.

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“…While it has been reported that QPOs can also be generated by cooling (Molteni et al 1996b). In realistic disc, both processes are active, and both should produce shock oscillation.…”

Section: Discussion and Concluding Remarksmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

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Periodic mass loss from viscous accretion flows around black holes

Das

Chattopadhyay

Nandi

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…It has been shown previously that accretion disc shock may launch bipolar jets (Molteni et al 1994(Molteni et al , 1996aDas et al 2014;Lee et al 2016). The jump condition across an accretion shock is obtained by conserving fluxes across the shock front, e.g., mass flux, momentum flux and energy flux (Taub 1948).…”

Section: Shock Waves In Accretion and Bipolar Jetsmentioning

confidence: 99%

Estimation of bipolar jets from accretion discs around Kerr black holes

Kumar

Chattopadhyay

2017

Monthly Notices of the Royal Astronomical Society

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We analyse flows around a rotating black hole and obtain self-consistent accretionejection solutions in full general relativistic prescription. Entire energy-angular momentum parameter space is investigated in the advective regime to obtain shocked and shock-free accretion solutions. Jet equations of motion are solved along the von-Zeipel surfaces computed from the post-shock disc, simultaneously with the equations of accretion disc along the equatorial plane. For a given spin parameter, the mass outflow rate increases as the shock moves closer to the black hole, but eventually decreases, maximizing at some intermediate value of shock location. Interestingly, we obtain all types of possible jet solutions, for example, steady shock solution with multiple critical points, bound solution with two critical points and smooth solution with single critical point. Multiple critical points may exist in jet solution for spin parameter a s 0.5. The jet terminal speed generally increases if the accretion shock forms closer to the horizon and is higher for corotating black hole than the counter-rotating and the non-rotating one. Quantitatively speaking, shocks in jet may form for spin parameter a s > 0.6 and jet shocks range between 6r g and 130r g above the equatorial plane, while the jet terminal speed v j∞ > 0.35c if Bernoulli parameter E 1.01 for a s > 0.99.

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“…This formalism has been used previously by Mondal et al (2009). Though we use the QPO frequency to be equal to the inverse of infall time, as found in Molteni et al (1996b), this relation need not be strictly followed (see also Das 2003 andSukova &Janiuk 2015). pointed out that the resonance condition could be satisfied over a wide band of parameter range.…”

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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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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Resonance Oscillation of Radiative Shock Waves in Accretion Disks around Compact Objects

Cited by 266 publications

References 17 publications

Periodic mass loss from viscous accretion flows around black holes

Periodic mass loss from viscous accretion flows around black holes

Estimation of bipolar jets from accretion discs around Kerr black holes

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

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