Comparison Between RHD Simulation of Supercritical Accretion Flows and a Steady Model With Outflows

Jiao, Cheng-Liang; Mineshige, Shin; Takeuchi, Shun; Ohsuga, Ken

doi:10.1088/0004-637x/806/1/93

Cited by 17 publications

(27 citation statements)

References 60 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our results are having the inflow and outflow regions for a certain range of the viscosity parameters and they also depend on other disk parameters. Which is consistent with some analytical (Xu & Chen 1997;Xue & Wang 2005;Jiao & Wu 2011;Gu 2012Gu , 2015 and numerical simulation studies (Ohsuga et al 2005;Okuda et al 2007;Yuan et al 2012a,b;Yang et al 2014;Jiao et al 2015;Yuan et al 2015). Although, our solutions and the disk structure are quite different from the previous analytical studies on 2D disk flow with self-similar conditions, e.g., the size and shape of the disks, behavior of the solutions and supersonic regions.…”

Section: Summary and Discussionsupporting

confidence: 90%

The 2D Disk Structure with Advective Transonic Inflow–Outflow Solutions around Black Holes

Kumar

2018

ApJ

View full text Add to dashboard Cite

We solved analytically viscous two-dimensional (2D) fluid equations for accretion and outflows in spherical polar coordinates (r, θ, φ) and obtained explicitly flow variables in r− and θ−directions around black holes (BHs). We investigated global transonic advection-dominated accretion flow (ADAF) solutions in r−direction on an equatorial plane with using Paczyński-Wiita potential. We used radial flow variables of ADAFs with symmetric conditions on the equatorial plane, as initial values for integration in θ−direction. In the study of 2D disk structure, we used twoazimuthal components of viscous stress tensors namely, τ rφ and τ θφ . Interestingly, we found that the whole advective disk is not participating in outflow generation and the outflows form close to the BHs. Normally, outflow strength increased with increasing viscosity parameter (α 1 ), mass-loss parameter (s) and decreasing gas pressure ratio (β). Outflow region increased with increasing s, α 1 for τ rφ and decreasing α 2 for τ θφ . The τ θφ is effective in angular momentum transportation at high latitude and outflows collimation along an axis of symmetry since it changes polar velocity (v θ ) of the flow. The outflow emission is also affected by the ADAF size and decreased with decreasing it. Transonic surfaces formed for both inflows (v r < 0, very close to BH) and outflows (v r > 0). We also explored no outflows, outflows and failed outflows regions, which mainly depend on the viscosity parameters.

show abstract

Section: Summary and Discussionsupporting

confidence: 90%

The 2D Disk Structure with Advective Transonic Inflow–Outflow Solutions around Black Holes

Kumar

2018

ApJ

View full text Add to dashboard Cite

show abstract

“…In SS433, the much larger Eddington factorṁ w ∼ 10 4 implies a quasi-spherical wind speed close to the observed velocity width ∼1500 km s −1 of the so-called stationary H-α line. Recent numerical simulations (Jiao et al 2015) also find winds with velocities ∼0.1-0.2c except very close to the rotational axis, where the velocity is higher, as expected.…”

Section: H Y P E R -E D D I N G To N B L Ac K H O L E W I N D Ssupporting

confidence: 80%

Black hole winds II: Hyper-Eddington winds and feedback

King

Muldrew

2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We show that black holes supplied with mass at hyper-Eddington rates drive outflows with mildly sub-relativistic velocities. These are ∼0.1-0.2c for Eddington accretion factorsṁ acc ∼ 10-100, and ∼1500 km s −1 forṁ acc ∼ 10 4 . Winds like this are seen in the X-ray spectra of ultraluminous sources (ULXs), strongly supporting the view that ULXs are stellar-mass compact binaries in hyper-Eddington accretion states. SS433 appears to be an extreme ULX system (ṁ acc ∼ 10 4 ) viewed from outside the main X-ray emission cone. For less-extreme Eddington factorsṁ acc ∼ 10-100 the photospheric temperatures of the winds are ∼100 eV, consistent with the picture that the ultraluminous supersoft sources (ULSs) are ULXs seen outside the medium-energy X-ray beam, unifying the ULX/ULS populations and SS433 (actually a ULS but with photospheric emission too soft to detect). For supermassive black holes (SMBHs), feedback from hyper-Eddington accretion is significantly more powerful than the usual near-Eddington ('UFO') case, and if realized in nature would imply M − σ masses noticeably smaller than observed. We suggest that the likely warping of the accretion disc in such cases may lead to much of the disc mass being expelled, severely reducing the incidence of such strong feedback. We show that hyper-Eddington feedback from bright ULXs can have major effects on their host galaxies. This is likely to have important consequences for the formation and survival of small galaxies.Key words: black hole physics -galaxies: active -quasars: general -quasars: supermassive black holes -galaxies: Seyfert -X-rays: binaries. I N T RO D U C T I O NIt is now widely accepted that winds driven by accretion on to black holes have major effects on their surroundings. Wide-angle winds from supermassive black holes (SMBH) in galaxy centres are probably the origin of the SMBH -galaxy scaling relations (for reviews of observations and theory see Kormendy & Ho 2013;King & Pounds 2015). King & Pounds (2003) gave a simple picture of black hole winds for the case when accretion on to the black hole is close to the Eddington value. This paper extends this to cover cases where the hole's mass supply rate is much larger. Shakura & Sunyaev (1973) set out a general theoretical picture of disc winds. They considered accretion discs where the mass supply at the outer edge would be super-Eddington near the black hole. At large distances from the hole, gas spirals inwards through an accretion disc and radiation pressure is unimportant. It first becomes E-mail: ark@astro.le.ac.uk significant in the disc at the spherization radius R sph , where the local energy release GMṀ/R sph is of order the Eddington luminositywith M the black hole mass,Ṁ the instantaneous accretion rate, and κ the electron scattering opacity. Some of the accreting gas is driven out as a wind by radiation pressure, and Shakura & Sunyaev assumed that this occurs at all disc radii R < R sph in such a way that GMṀ(R)/R ∼ L Edd at all R. This means that the accretion rate through the disc decr...

show abstract

“…If the wind is isotropically emitted, it significantly regulates accretion (Wang et al 2021a) and gas dynamical friction (Gruzinov et al 2020). On the other hand, if it is anisotropic, as predicted by numerical simulations (Jiao et al 2015;Kitaki et al 2021), the feedback does not efficiently regulate either accretion (Takeo et al 2020) or dynamical friction (Li et al 2020). Also, when the trapping radius is smaller than the circularization radius, the mass ratio of outflows to inflows is modest (Kitaki et al 2021).…”

Section: A3 Evolution Of Black Hole Mass and Locationmentioning

confidence: 97%

“…The cocoon dynamics may be also influenced by the winds launched in super-Eddington regimes (e.g. Jiao et al 2015;Kitaki et al 2021). To evaluate this influence, we compare the pressure of the wind to that of the cocoon.…”

Section: B2 Influence Of Winds On Cocoon Evolutionmentioning

confidence: 99%

“…However, the wind expected under conditions of super-Eddington accretion is predicted to be launched anisotropically (e.g. Jiao et al 2015;Kitaki et al 2021), and the gas inflow outside the wind opening angle is only modestly suppressed as long as the wind is not decelerated in a shock (Takeo et al 2020). If most of the inflowing gas is ejected as the wind (e.g.…”

mentioning

confidence: 99%

See 1 more Smart Citation

Can stellar-mass black hole growth disrupt disks of active galactic nuclei? The role of mechanical feedback

Tagawa,

Kimura,

Haiman

et al. 2021

Preprint

View full text Add to dashboard Cite

Stellar-mass BHs (sBHs) are predicted to be embedded in active galactic nuclei (AGN) disks due to gravitational drag and in-situ star formation. However, we find that due to a high gas density in an AGN disk environment, compact objects may rapidly grow to intermediate-mass BHs and deplete matter from the AGN disk unless accretion is suppressed by some feedback process(es). These consequences are inconsistent with AGN observations and the dynamics of the Galactic center. Here we consider mechanical feedback mechanisms for the reduction of gas accretion. Rapidly accreting sBHs launch winds and/or jets via the Blandford-Znajek mechanism, which produce high-pressure shocks and cocoons. Such a shock and cocoon can spread laterally in the plane of the disk, eject the outer regions of a circum-sBH disk (CsBD) and puncture a hole in the AGN disk with horizontal size comparable to the disk scale-height. Since the depletion timescale of the bound CsBD is much shorter than the resupply timescale of gas to the sBH, the time-averaged accretion rate onto sBHs is reduced by this process by a factor of ∼ 10-100. This feedback mechanism can therefore help alleviate the sBH over-growth and AGN-disk depletion problems. On the other hand, we find that cocoons of jets can unbind a large fraction of the gas accreting in the disks of less massive SMBHs, which may help explain the dearth of high-Eddington ratio AGNs with SMBH mass 10 5 M ⊙ .

show abstract

Comparison Between RHD Simulation of Supercritical Accretion Flows and a Steady Model With Outflows

Cited by 17 publications

References 60 publications

The 2D Disk Structure with Advective Transonic Inflow–Outflow Solutions around Black Holes

The 2D Disk Structure with Advective Transonic Inflow–Outflow Solutions around Black Holes

Black hole winds II: Hyper-Eddington winds and feedback

Can stellar-mass black hole growth disrupt disks of active galactic nuclei? The role of mechanical feedback

Contact Info

Product

Resources

About