The properties of wind and jet from a super-Eddington accretion flow around a supermassive black hole

Yang, Hai; Yuan, Feng; Kwan, Tom M.; Dai, Li‐Xin

doi:10.1093/mnras/stad1444

Cited by 7 publications

(3 citation statements)

References 91 publications

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“…A physical link between the strengthening/weakening of the IC component, and the inclination variation of the disk, is possible, as indicated by the analysis of the early time NICER data. Simulations suggest that, when a massive BH accretes at super-Eddington levels, in the scenario of a powerful disk outflow, the temperature of the inner accretion region reaches 10 6 K (corresponding to 0.09 keV; e.g., Jiang et al 2019;Yang et al 2023). Our results are consistent with the picture that, as the disk inclination decreases, more photons from the hotter accretion region at smaller radii are observed.…”

Section: Discussionsupporting

confidence: 87%

Tidal Disruption Event AT2020ocn: Early Time X-Ray Flares Caused by a Possible Disk Alignment Process

Cao,

Jonker,

Pasham

et al. 2024

ApJ

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A tidal disruption event (TDE) may occur when a star is torn apart by the tidal force of a black hole (BH). Eventually, an accretion disk is thought to form out of stellar debris falling back toward the BH. If the star’s orbital angular momentum vector prior to disruption is not aligned with the BH spin angular momentum vector, the disk will be tilted with respect to the BH equatorial plane. The disk will eventually be drawn into the BH equatorial plane due to a combination of the Bardeen–Petterson effect and internal torques. Here, we analyze the X-ray and UV observations of the TDE AT2020ocn obtained by Swift, XMM-Newton, and Neutron star Interior Composition ExploreR. The X-ray light curve shows strong flares during the first ≈100 days, while, over the same period, the UV emission decays gradually. We find that the X-ray flares can be explained by a model that also explains the spectral evolution. This model includes a slim disk viewed under a variable inclination plus an inverse-Comptonization component processing the slim disk emission. A scenario where the ongoing Lense–Thirring precession during the disk alignment process is responsible for the observed inclination variations is consistent with the data. In later observations, we find that the X-ray spectrum of AT2020ocn becomes harder, while the mass accretion rate remains at super-Eddington levels, suggesting the formation of a corona in line with accretion onto other compact objects. We constrain the BH mass to be ( 7 − 3 + 13 ) × 10 5 M ⊙ at the 1σ (68%) confidence level.

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Section: Discussionsupporting

confidence: 87%

Tidal Disruption Event AT2020ocn: Early Time X-Ray Flares Caused by a Possible Disk Alignment Process

Cao,

Jonker,

Pasham

et al. 2024

ApJ

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“…Due to the presence of the disk wind, the mass inflow rate would reduce inward. Numerical simulations show that the reduction roughly follows a power law within R tr (e.g., X.-H. Yang et al 2014;Kitaki et al 2021;Yoshioka et al 2022;H. Yang et al 2023), so we take the mass inflow rate varying with radius as (Blandford & Begelman 1999)…”

Section: Disk Equationsmentioning

confidence: 99%

Super-Eddington Magnetized Neutron Star Accretion Flows: A Self-similar Analysis

Chen,

Dai

2024

ApJ

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The properties of super-Eddington accretion disks exhibit substantial distinctions from the sub-Eddington ones. In this paper, we investigate the accretion process of a magnetized neutron star (NS) surrounded by a super-Eddington disk. By constructing self-similar solutions for the disk structure, we study in detail an interaction between the NS magnetosphere and the inner region of the disk, revealing that this interaction takes place within a thin boundary layer. The magnetosphere truncation radius is found to be approximately proportional to the Alfvén radius, with a coefficient ranging between 0.34–0.71, influenced by the advection and twisting of a magnetic field, NS rotation, and radiation emitted from an NS accretion column. Under super-Eddington accretion, the NS can readily spin up to become a rapid rotator. The proposed model can be employed to explore the accretion and evolution of NSs in diverse astrophysical contexts, such as ultraluminous X-ray binaries or active galactic nucleus disks.

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“…This accretion regime is neglected in Yuan et al ( 2018 ) but is considered in this work. Specifically, the mass flux and velocity of wind as a function of Ṁ BH and radius will be taken from Yang et al ( 2023 ). In this work, they have performed three-dimensional general relativistic radiation magnetohydrodynamical (RMHD) numerical simulations of a super-Eddington accretion flow around a black hole and analyse the data using the 'virtual particle trajectory' approach, which can loyally reflect the motion of fluid elements and discriminate turbulence and real wind, to obtain the wind properties.…”

Section: Agn Physicsmentioning

confidence: 99%

Active galactic nuclei feedback in an elliptical galaxy (III): the impacts and fate of cosmological inflow

Zhu

Yuan

et al. 2023

Monthly Notices of the Royal Astronomical Society

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The cosmological inflow of a galaxy is speculated to be able to enter the galaxy and enhance the star formation rate (SFR) and black hole accretion rate (BHAR). In this paper, by performing high-resolution hydrodynamic simulations in the framework of MACER, we investigate the fate of the inflow and its impacts on the evolution of a massive elliptical galaxy. The inflow properties are adopted from the cosmological simulation IllustrisTNG. We find that the inflow gas hardly enters but is blocked beyond ∼20 kpc from the central galaxy and becomes part of the circumgalactic medium (CGM). The gas pressure gradient, mainly contributed by the thermalized stellar wind and subdominant contributed by the energy input from the AGN, balances gravity and prevents the inflow from entering the galaxy. The SFR and BHAR are almost not affected by the normal inflow. However, if the rate of cosmological inflow were increased by a factor of 3, a small fraction of the inflow would enter the galaxy and contribute about 10% of the gas in the galaxy. In this case, the gas density in the galaxy would increase by a factor of $\gtrsim $ 20. This increase is not because of the additional gas supply by the inflow but due to the increase of gas density and pressure in the CGM caused by the inflow. Consequently, the SFR and BHAR would increase by a factor of ∼5 and ∼1000, respectively. Finally, AGN feedback can perturb the motion of the inflow and heat the CGM through its intermittent outbursts.

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The properties of wind and jet from a super-Eddington accretion flow around a supermassive black hole

Cited by 7 publications

References 91 publications

Tidal Disruption Event AT2020ocn: Early Time X-Ray Flares Caused by a Possible Disk Alignment Process

Tidal Disruption Event AT2020ocn: Early Time X-Ray Flares Caused by a Possible Disk Alignment Process

Super-Eddington Magnetized Neutron Star Accretion Flows: A Self-similar Analysis

Active galactic nuclei feedback in an elliptical galaxy (III): the impacts and fate of cosmological inflow

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