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

Dönmez, Orhan

doi:10.1142/s0217732317501085

Cited by 5 publications

(12 citation statements)

References 23 publications

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“…As the bulk of the gas in the torus emits at low velocities and at correspondingly large radii, this behavior is suggestive of the presence of a m = 1-spiral in the gas. This asymmetry is expected if the molecular torus reflects the propagation of the Papaloizou-Pringle instability (PPI) (Papaloizou & Pringle 1984;Kiuchi et al 2011;Korobkin et al 2013;Dönmez 2014;Donmez 2017).…”

Section: Kinematics Of the Molecular Torusmentioning

confidence: 99%

“…Numerical simulations have long predicted the existence of dusty winds coming out from AGN tori with a large variance of geometries, which depend on the different treatment of radiation pressure driven by photons at different wavelengths (IR, X-ray and UV), on the assumed degree of anisotropy of the AGN radiation, and on the details of the particular hydrodynamic code used in these simulations (e.g., Wada 2015;Wada et al 2016;Chan & Krolik 2016, 2017Namekata & Umemura 2016;Williamson et al 2019). Furthermore, as recently argued by Giustini & Proga (2019), theoretical analyses predict that radiation-driven accretion disk winds in AGN can have a fairly large equatorial component in Seyfert galaxies that are characterized by Eddington ratios (Edd ratio ) and black hole masses (M BH ) similar to those of NGC 1068 (Edd ratio 0.5, log 10 (M BH /M ) 7.2; Greenhill et al 1996).…”

Section: An Outflowing Torus?mentioning

confidence: 99%

“…The question of the dynamical status of the torus has also evolved from the first proposed scenario, depicting the torus as a geometrically thick rotating doughnut-like disk in hydrostatic equilibrium (Krolik & Begelman 1988), towards a more dynamical picture, describing the torus as an outflowing structure, where clouds are embedded in a hydro-magnetically or radiatively driven wind (Blandford & Payne 1982;Emmering et al 1992;Bottorff et al 1997;Kartje et al 1999;Elitzur & Shlosman 2006;Wada 2012Wada , 2015Wada et al 2016;Hönig & Kishimoto 2017;Chan & Krolik 2016, 2017Williamson et al 2019;Hönig 2019). This outflowing torus may be part of the obscuring structures that have been identified as polar-like dust components in a notable fraction of Seyferts observed with interferometers in the MIR (Tristram et al 2009;Burtscher et al 2013;Hönig et al 2013;López-Gonzaga et al 2014.…”

Section: Introductionmentioning

confidence: 99%

“…Alternatively, the disturbed kinematics of the torus could be the signature of the Papaloizou-Pringle instability (PPI), predicted to drive the dynamical evolution of AGN tori on scales r ≤ 0.1 pc (Papaloizou & Pringle 1984). This instability has been studied both in isolated tori (Kiuchi et al 2011;Korobkin et al 2013) and also in tori perturbed due to the accretion of gas (Dönmez 2014;Donmez 2017). These simulations show the growth of a long-lasting non-axisymmetric m = 1 mode.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Kinematics Of the Molecular Torusmentioning

confidence: 99%

Section: An Outflowing Torus?mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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

García‐Burillo

Combes

Almeida

et al. 2019

A&A

140

103

View full text Add to dashboard Cite

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“…2004). The perturbation of the black hole torus system can be observed in different types of perturbations such as angular velocity perturbation (Donmez 2017), spherical shell accretion (Donmez 2015), radial velocity perturbation , and Bondi-Hoyle accretion , which are all studied to extract the oscillation properties of the torus' PPI instabilities, and the quasi-periodic frequencies produced during these oscillations. The non-axisymmetric perturbations trigger the PPI instability and cause the excitation of frequencies due to the non-linear coupling of the modes.…”

Section: Introductionmentioning

confidence: 99%

On the dynamics of the torus around the kicked black hole

Donmez,

Al-Kandari,

Seedo

2021

Preprint

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There is a special interest to understand the dynamical properties of the accretion disk created around the newly formed black hole due to the supermassive black hole binaries which merge inside the gaseous disk. The newly formed black hole would have a kick velocity that drives a perturbation on a newly accreted torus around the black hole. In this paper, the effects of the kicked black holes onto the accreted torus are studied by using the general relativistic hydrodyanmical code, focusing on changing the dynamics of the accretion disk during the accretion disk-black hole interaction. We have found the non-axisymmetric global mode m = 1 Papaloizou-Pringle Instability (PPI) produced on the torus due to kicked black hole. The higher the perturbation velocity produced by the kicked black hole, the longer time the torus takes to reach the saturation point. The created funnel walls are also observed from the numerical simulations. These funnels are responsible for accreting matter toward to the black hole. At the later time of evolution, the accretion through the funnel is stopped and PPI is developed on the torus around the black hole.

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Bondi–Hoyle accretion around the non-rotating black hole in 4D Einstein–Gauss–Bonnet gravity

Dönmez

2021

Eur. Phys. J. C

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In this paper, the numerical investigation of a Bondi–Hoyle accretion around a non-rotating black hole in a novel four dimensional Einstein–Gauss–Bonnet gravity is investigated by solving the general relativistic hydrodynamical equations using the high resolution shock capturing scheme. For this purpose, the accreated matter from the wind-accreating X-ray binaries falls towards the black hole from the far upstream side of the domain, supersonically. We study the effects of Gauss–Bonnet coupling constant $$\alpha $$ α in 4D EGB gravity on the accreated matter and shock cones created in the downstream region in detail. The required time having the shock cone in downstream region is getting smaller for $$\alpha > 0$$ α > 0 while it is increasing for $$\alpha < 0$$ α < 0 . It is found that increases in $$\alpha $$ α leads violent oscillations inside the shock cone and increases the accretion efficiency. The violent oscillations would cause increase in the energy flux, temperature, and spectrum of X-rays. So the quasi-periodic oscillations (QPOs) are naturally produced inside the shock cone when $$-5 \le \alpha \le 0.8$$ - 5 ≤ α ≤ 0.8 . It is also confirmed that EGB black hole solution converges to the Schwarzschild one in general relativity when $$\alpha \rightarrow 0$$ α → 0 . Besides, the negative coupling constants also give reasonable physical solutions and increase of $$\alpha $$ α in negative directions suppresses the possible oscillation observed in the shock cone.

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

Cited by 5 publications

References 23 publications

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

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

On the dynamics of the torus around the kicked black hole

Bondi–Hoyle accretion around the non-rotating black hole in 4D Einstein–Gauss–Bonnet gravity

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