On the development of the Papaloizou–Pringle instability of the black hole–torus systems and quasi-periodic oscillations

Dönmez, Orhan

doi:10.1093/mnras/stt2255

Cited by 14 publications

(25 citation statements)

References 43 publications

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“…The relation among the pressure, rest mass density, and internal energy is defined using the perfect fluid equation of state P = (Γ − 1)ρ with Γ = 4/3. Initially a steady state accreated torus is produced using the appropriate values of the highest density of the torus ρ c = 1.140 x 10 −4 , the mass ratio of the black hole-torus M t /M BH = 0.1, the polytropic constant K = 4.969 x 10 −2 , the constant specific angular momentum 0 = 3.80, inner r in = 4.57 and outer, r out = 15.889, radii of the torus, cusp location r cusp = 4.57, and orbital period t orb = 151.6 at r c = 8.35 (Dönmez 2014a(Dönmez ,b, 2015.…”

Section: Equations Models and Initial Setupsmentioning

confidence: 99%

“…The outflow boundary condition is set up close to or far away from the black hole to avoid the unwanted oscillations. The more details about initial setups as well as boundaries used in our numerical simulation can be found in Dönmez (2014aDönmez ( ,b, 2015.…”

Section: Equations Models and Initial Setupsmentioning

confidence: 99%

“…They found vertical epicyclic frequencies. We have previously found (Dönmez 2014a) the numerical study of the dynamical instability of the torus on the equatorial plane due to perturbation which was represented injecting gas from the outer boundary of the domain. It was shown that the mass accretion rate in the perturbed torus strongly depended on the cusp location and dynamical changes of the torus triggered the PPI.…”

Section: Introductionmentioning

confidence: 99%

“…The instability was occurring when the waves inside the radius are transferring their energy to the waves outside of the corotation radius (Blaes & Glatzel 1986). Besides, the emerging the hydrodynamical instabilities were strongly depended on the physical parameters of the system such as the torus size, angular momentum of the black hole, angular momentum of the torus, and the type of the instability (Villiers & Hawley 2002;Dönmez 2014aDönmez , 2017. The observational evidence of the PPI in Seyfert galaxy N GC 1068 was found by Garcia-Burillo et.al (2017).…”

Section: Introductionmentioning

confidence: 99%

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Angular velocity perturbations inducing the Papaloizou–Pringle instability and QPOs in the torus around the black hole

Dönmez

2017

Mod. Phys. Lett. A

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A numerical study of the dynamic of the nonselfgravitating, unmagnetized, nonaxisymmetric, and rotating the torus around the non-rotating black hole is presented. We investigate the instability of the rotating torus subject to perturbations presented by increasing or decreasing the angular velocity of the stable torus. We have done, for the first time, an extensive analysis of the torus dynamic response to the perturbation of the angular velocity of the stable torus. We show how the high, moderate, and low values of the perturbations affect the torus dynamic and help us to understand the properties of the instability and Quasi-Periodic Oscillation (QPO). Our numerical simulations indicate the presence of Papaloizou-Pringle instability (PPI) with global m = 1 mode and QPOs for the moderate and lower values of the perturbations on the angular velocity of the stable torus. Furthermore, with the lower values of the perturbations, the torus can lead to a wiggling initially and then PPI is produced in it. Finally, the matter of the torus would be dissipated due to the presence of a strong torque.

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Section: Equations Models and Initial Setupsmentioning

confidence: 99%

Section: Equations Models and Initial Setupsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Angular velocity perturbations inducing the Papaloizou–Pringle instability and QPOs in the torus around the black hole

Dönmez

2017

Mod. Phys. Lett. A

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“…The low density atmosphere, ρ atm = 10 the maximum density and pressure values at a well defined radial and angular coordinates for the stable torus, respectively. The numerical evolution of the black hole-torus system without any perturbation showed that the dynamic of steady-state torus was uninfluenced by the presence of the defined atmosphere [10]. The general form of the Kerr metric in Boyer-Lindquist coordinates is used to set up the black hole at the center of computational domain using a uniformly spaced grid along radial r and angular ϕ directions.…”

Section: Initial Setups and Definition Of The Physical Boundariesmentioning

confidence: 99%

Investigating the instability of the torus around the blackhole in the presence of the radial and angular velocity perturbations

Dönmez¹

2017

Turk J Phys

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Abstract:We have performed the numerical simulation of the perturbed relativistic torus around the black hole by solving the general relativistic hydrodynamics equations on the equatorial plane. We have monitored the different simple models by applying the radial and angular velocity perturbations to the steady state torus around the black hole. The instabilities are triggered by adding the subsonic velocity fields over the radial and angular velocities of the stable torus.We have found the disk instability so-called the Papaloizou-Pringle instability and excited modes of the Quasi-Periodic Oscillations (QPOs) in the thin disk approximation case. The significant oscillations and oscillation modes in the mass accretion rates are observed around the rotating black hole with a radial velocity perturbation. The angular velocity perturbation can not create the significant variations and QPOs in the nonselfgravitating relativistic torus around the nonrotating and rotating black holes. The results observed from the radial velocity perturbation might be used to explain the Papaloizou-Pringle instability observed in N GC 1068

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ALMA images the many faces of the NGC 1068 torus and its surroundings

García‐Burillo

Combes

Almeida

et al. 2019

A&A

140

103

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Aims. We investigate the fueling and the feedback of nuclear activity in the nearby (D = 14 Mpc) Seyfert 2 barred galaxy NGC 1068, by studying the distribution and kinematics of molecular gas in the torus and its connections to the host galaxy disk. Methods. We use the Atacama Large Millimeter Array (ALMA ) to image the emission of a set of molecular gas tracers in the circumnuclear disk (CND) and the torus of the galaxy using the CO(2-1), CO(3-2) and HCO + (4-3) lines and their underlying continuum emission with high spatial resolutions (0.03 −0.09 2−6 pc). These transitions, which span a wide range of physical conditions of molecular gas (n(H 2 ) ⊂ 10 3 −10 7 cm −3 ), are instrumental in revealing the density radial stratification and the complex kinematics of the gas in the torus and its surroundings. Results. The ALMA images resolve the CND as an asymmetric ringed disk of D 400 pc-size and mass of 1.4 × 10 8 M sun . The CND shows a marked deficit of molecular gas in its central 130 pc-region. The inner edge of the ring is associated with the presence of edge-brightened arcs of NIR polarized emission, which are identified with the current working surface of the ionized wind of the active galactic nucleus (AGN). ALMA proves the existence of an elongated molecular disk/torus in NGC 1068 of M gas torus 3 × 10 5 M , which extends over a large range of spatial scales D 10 − 30 pc around the central engine. The new observations evidence the density radial stratification of the torus: the HCO + (4-3) torus, with a full size D HCO + (4−3) = 11 ± 0.6 pc, is a factor of 2-3 smaller than its CO(2-1) and CO(3-2) counterparts, which have full-sizes D CO(3−2) = 26 ± 0.6 pc and D CO(2−1) = 28 ± 0.6 pc, respectively. This result brings into light the many faces of the molecular torus. The torus is connected to the CND through a network of molecular gas streamers detected inside the CND ring. The kinematics of molecular gas show strong departures from circular motions in the torus, the gas streamers, and the CND ring. These velocity field distortions are interconnected and are part of a 3D outflow that reflects the effects of AGN feedback on the kinematics of molecular gas across a wide range of spatial scales around the central engine. In particular, we estimate through modeling that a significant fraction of the gas inside the torus ( 0.4 − 0.6 × M gas torus ) and a comparable amount of mass along the gas streamers are outflowing. However, the bulk of the mass, momentum and energy of the molecular outflow of NGC 1068 is contained at larger radii in the CND region, where the AGN wind and the radio jet are currently pushing the gas assembled at the Inner Lindblad Resonance (ILR) ring of the nuclear stellar bar. Conclusions. In our favored scenario a wide-angle AGN wind launched from the accretion disk of NGC1068 is currently impacting a sizable fraction of the gas inside the torus. However, a large gas reservoir ( 1.2 − 1.8 × 10 5 M ), which lies close to the equatorial plane of the torus, remains unaffected by the feedback of...

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On the development of the Papaloizou–Pringle instability of the black hole–torus systems and quasi-periodic oscillations

Cited by 14 publications

References 43 publications

Angular velocity perturbations inducing the Papaloizou–Pringle instability and QPOs in the torus around the black hole

Angular velocity perturbations inducing the Papaloizou–Pringle instability and QPOs in the torus around the black hole

Investigating the instability of the torus around the blackhole in the presence of the radial and angular velocity perturbations

ALMA images the many faces of the NGC 1068 torus and its surroundings

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