Modified Newtonian Potentials for the Description of Relativistic Effects in Accretion Disks around Black Holes

Artemova, I. V.; Bjoernsson, G.; Новиков, И. Д.

doi:10.1086/177084

Cited by 171 publications

(212 citation statements)

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“…Although the advective disc solutions contain features that automatically explain some of the broad observational features (compact corona, compact jet base, spectral state changes), still most of the works were done in the pseudo-Newtonian regime (Paczyński & Wiita 1980;Artemova et. al.…”

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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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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“…The advance to the pseudo-Newtonian imitation of spinning fields mainly followed the proposal by Artemova et al (1996) of two simple potentials for the Kerr black hole. Recently, these have been checked against a slightly different formula (as well as against the "benchmark" of the Paczyński-Wiita potential) on the behaviour of circular-orbit acceleration by Karas & Abramowicz (2015).…”

Section: Previous Results From the Literaturementioning

confidence: 99%

“…Other major simple pseudo-Newtonian substitutes for Schwarzschild were provided by Artemova et al (1996) and quite recently by Wegg (2012). Artemova et al (1996) used several pseudo-potentials in studying disc accretion onto black holes; in the non-rotating case, they considered expressions (we number them according to the original paper)…”

Section: Black Hole With Disc or Ring: A Pseudo-newtonian Descriptionmentioning

confidence: 99%

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Free motion around black holes with discs or rings: between integrability and chaos – IV

Witzany

Semerák

Suková

2015

Monthly Notices of the Royal Astronomical Society

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The dynamical system studied in previous papers of this series, namely a bound time-like geodesic motion in the exact static and axially symmetric space-time of an (originally) Schwarzschild black hole surrounded by a thin disc or ring, is considered to test whether the often employed "pseudo-Newtonian" approach (resorting to Newtonian dynamics in gravitational potentials modified to mimic the black-hole field) can reproduce phase-space properties observed in the relativistic treatment. By plotting Poincaré surfaces of section and using two recurrence methods for similar situations as in the relativistic case, we find similar tendencies in the evolution of the phase portrait with parameters (mainly with mass of the disc/ring and with energy of the orbiters), namely those characteristic to weakly non-integrable systems. More specifically, this is true for the Paczyński-Wiita and a newly suggested logarithmic potential, whereas the Nowak-Wagoner potential leads to a different picture. The potentials and the exact relativistic system clearly differ in delimitation of the phase-space domain accessible to a given set of particles, though this mainly affects the chaotic sea whereas not so much the occurrence and succession of discrete dynamical features (resonances). In the pseudoNewtonian systems, the particular dynamical features generally occur for slightly smaller values of the perturbation parameters than in the relativistic system, so one may say that the pseudo-Newtonian systems are slightly more prone to instability. We also add remarks on numerics (a different code is used than in previous papers), on the resemblance of dependence of the dynamics on perturbing mass and on orbital energy, on the difference between the Newtonian and relativistic Bach-Weyl rings, and on the relation between Poincaré sections and orbital shapes within the meridional plane.

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“…In the present work we would like to study the chaotic motion of test particles under the combined influence of the gravitational field of a Kerr black hole as well as the dipolar halo surrounding it by incorporating the potential proposed by Artemova et al (1996). The same pseudo-Kerr black hole potential has been used by Ying and Xin (2012) to study the non relativistic (for v particle << c, c being the velocity of light in vacuum) chaotic dynamics within the quadruple halo.…”

Section: Introductionmentioning

confidence: 99%

Influence of the black hole spin on the chaotic particle dynamics within a dipolar halo

Nag¹,

Sinha²,

Ananda

et al. 2017

Astrophys Space Sci

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We investigate the role of the spin angular momentum of astrophysical black holes in controlling the special relativistic chaotic dynamics of test particles moving under the influence of a post-Newtonian pseudo-Kerr black hole potential, along with a perturbative potential created by a asymmetrically placed (dipolar) halo. Proposing a Lyapunov-like exponent to be the effective measure of the degree of chaos observed in the system under consideration, it has been found that black hole spin anti-correlates with the degree of chaos for the aforementioned dynamics. Our findings have been explained applying the general principles of dynamical systems analysis.

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Modified Newtonian Potentials for the Description of Relativistic Effects in Accretion Disks around Black Holes

Cited by 171 publications

References 0 publications

Estimation of bipolar jets from accretion discs around Kerr black holes

Estimation of bipolar jets from accretion discs around Kerr black holes

Free motion around black holes with discs or rings: between integrability and chaos – IV

Influence of the black hole spin on the chaotic particle dynamics within a dipolar halo

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