Transonic disk accretion onto black holes

Liang, Edison; Thompson, K.A.

doi:10.1086/158231

Cited by 111 publications

(108 citation statements)

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“…We add a further comment on the shock or no shock solutions, since many authors consider the Chakrabarti solutions untenable, as the shock he finds had not been confirmed by their calculations. As has been pointed out in early works (Liang & Thompson 1980), there are many sonic points in the flow solutions. The flow on a BH has no rigid surface, and shock occurs only in solutions passing through the outer sonic point as clearly demonstrated by Chakrabarti (1990) and Chakrabarti & Molteni (1993).…”

Section: Solutionsmentioning

confidence: 89%

Why Canonical Disks Cannot Produce Advection-dominated Flows

Molteni¹,

Gerardi²,

Valenza³

2001

The Astrophysical Journal

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Using simple arguments we show that the canonical thin Keplerian accretion disks cannot smoothly match any plain advection-dominated accretion flow (ADAF) model. By "plain" ADAF models we mean the ones with zero cooling. The existence of sonic points in exact solutions is critical and imposes constraints that cannot be surpassed adopting "reasonable" physical conditions at the hypothetical match point. Only the occurrence of new critical physical phenomena may produce a transition. We propose that exact advection models are a class of solutions that do not necessarily involve the standard thin cool disks and suggest a different scenario in which good ADAF solutions could eventually occur.

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Section: Solutionsmentioning

confidence: 89%

Why Canonical Disks Cannot Produce Advection-dominated Flows

Molteni¹,

Gerardi²,

Valenza³

2001

The Astrophysical Journal

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“…1996;Mukhopadhyay 2003;Chakrabarti & Mondal 2006). Full general relativistic treatment were few and far between (Liang & Thompson 1980;Lu 1985;Fukue 1987;Chakrabarti 1996 . The more favoured model for jet generation in the community is magnetically driven jets (Blandford & Payne 1982;Camezind 1986;Fendt & Greiner 2001).…”

Section: Existence Of the Dominant Power-law Photons In The Lhs And Imentioning

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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“…Therefore, solutions of relativistic equations for transonic accretion discs around BH have been few (for e.g. Liang & Thompson 1980;Lu 1985;Fukue 1987;Chakrabarti 1996) when compared with those in pNp regime and that too in the inviscid limit. The first consistent viscous advective accretion solution in pure GR was obtained by Peitz & Appl (1997).…”

Section: Introductionmentioning

confidence: 99%

Estimation of mass outflow rates from viscous relativistic accretion discs around black holes

Chattopadhyay

Kumar

2016

Mon. Not. R. Astron. Soc.

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We investigated flow in Schwarzschild metric, around a non-rotating black hole and obtained self-consistent accretion -ejection solution in full general relativity. We covered the whole of parameter space in the advective regime to obtain shocked, as well as, shock-free accretion solution. We computed the jet streamline using von -Zeipel surfaces and projected the jet equations of motion on to the streamline and solved them simultaneously with the accretion disc equations of motion. We found that steady shock cannot exist for α > ∼ 0.06 in the general relativistic prescription, but is lower if mass -loss is considered too. We showed that for fixed outer boundary, the shock moves closer to the horizon with increasing viscosity 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. The jet terminal speed increases with stronger shocks, quantitatively speaking, the terminal speed of jets v j∞ > 0.1 if r sh < 20r g . The maximum of the outflow rate obtained in the general relativistic regime is less than 6% of the mass accretion rate.

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Transonic disk accretion onto black holes

Cited by 111 publications

References 0 publications

Why Canonical Disks Cannot Produce Advection-dominated Flows

Why Canonical Disks Cannot Produce Advection-dominated Flows

Estimation of bipolar jets from accretion discs around Kerr black holes

Estimation of mass outflow rates from viscous relativistic accretion discs around black holes

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