Two-dimensional Models of Hydrodynamical Accretion Flows into Black Holes

By I. Igumenshchev, Marek Abramowicz. 2000

152 citations recorded by the source corpus.

We present a systematic numerical study of two-dimensional axisymmetric accretion flows around black holes. The flows have no radiative cooling and are treated in the framework of the viscous hydrodynamic approximation. The models calculated in this study cover the large range of the relevant parameter space. There are four types of flows, determined by the values of the viscosity parameter α and the adiabatic index γ: convective flows, large-scale circulations, pure inflows, and bipolar outflows. Thermal conduction introduces significant changes to the solutions but does not create a new flow type. Convective accretion flows and flows with large-scale circulations have significant outward-directed energy fluxes, which have important implications for the spectra and luminosities of accreting black holes.

Subfields: Astronomy and Astrophysics, Mechanical Engineering

View Paper: https://www.semanticscholar.org/paper/de1d17be19c2bcf3a1be14075b9719b58da60b55

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Ramesh Narayan
2. F. Yuan
3. J. McKinney
4. A. Sa̧dowski
5. A. Tchekhovskoy
6. E. Quataert
7. B. Metzger
8. Bing Zhang

In Mechanical Engineering

1. Ramesh Narayan
2. F. Yuan
3. A. Merloni
4. A. C. Fabian
5. J. McKinney
6. Pawan Kumar
7. T. Piran
8. A. Sa̧dowski

Citations in the corpus

• Energy, momentum and mass outflows and feedback from thick accretion discs around rotating black holes (2013, background): “Already early works based on pseudo-Newtonian codes with purely hydrodynamic viscosity showed that a significant fraction of the inflowing mass near the equatorial plane can flow out along the poles (Igumenshchev & Abramowicz 1999, 2000; Stone, Pringle & Begelman 1999).”
• Three-dimensional Magnetohydrodynamic Simulations of Radiatively Inefficient Accretion Flows (2003, methodology): “For instance, model A has a relative disk thickness, H=R ’ 0:5, a flattened density profile, and nearly Keplerian rotation, all of which make it similar to the CDAF model shown for instance in Figure 17 of Igumenshchev & Abramowicz (2000).”
• General relativistic magnetohydrodynamic simulations of the jet formation and large-scale propagation from black hole accretion systems (2006, background): “Nonrelativistic outflows were found even in viscous hydrodynamic simulations (Stone et al. 1999; Igumenshchev & Abramowicz 1999, 2000; McKinney & Gammie 2002).”
• Constraining the Accretion Rate onto Sagittarius A* Using Linear Polarization (2000, background): “…flows with small values of the dimensionless viscosity parameter α find that the gas density scales with radius as ρ ∝ r−1/2 rather than the canonical Bondi/ADAF scaling of ρ ∝ r−3/2 (Stone, Pringle, & Begelman 1999; Igumenshchev & Abramowicz 1999, 2000; Igumenshchev, Abramowicz, & Narayan 2000).”
• Coronal outflow dominated accretion discs: a new possibility for low-luminosity black holes? (2001, methodology): “Th problem is inherently 2D (Igumenshchev & Abramowicz 2000), and the simultaneous roles of convection, advection and outflows have to be assessed in order to properly model the expected SED.”
• Accretion Models of Gamma-Ray Bursts (2001, methodology): “The formation of an accretion disk is a natural outcome of most popular models of GRBs, e.g. the mergers of double neutron star binaries (Eichler et al., 1989; Narayan, Paczyński & Piran 1992), neutron star black hole binaries (Paczyński, 1991; Narayan Paczyński & Piran 1992), black hole white dw”
• SUPERNOVA LIGHT CURVES POWERED BY FALLBACK ACCRETION (2012, background): “Such radiatively inefficient accretion flows are expected to produce large-scale outflows (Narayan & Yi 1994; Blandford & Begelman 1999; Igumenshchev & Abramowicz 2000; Pen et al. 2003; Begelman 2012; McKinney et al. 2012) and/or Poynting flux dominated jets (De Villiers et al. 2005; McKinney 2006).”
• Fluorescent iron lines as a probe of astrophysical black hole systems (2002, background): “These suggestions remain controversial [113] and are the subject of active research [172–174], but in any case, such a flow is likely to be extremely hot (electron temperatures of ∼ 10K) and optically-thin.”
• A Magnetohydrodynamic Nonradiative Accretion Flow in Three Dimensions (2001, background): “Most (e.g., Igumenshchev & Abramowicz 1999, 2000, hereafter IA99, IA00; Stone, Pringle, & Begelman 1999, hereafter SPB) have assumed the flow evolves due to a fortified kinematic viscosity, ν.”
• NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. II. NATURE, ORIGIN, AND PROPERTIES OF OUTFLOWS AND THEIR POSSIBLE OBSERVATIONAL APPLICATIONS (2012, background): “Such a prediction has been well confirmed by HD simulations (SPB99; Igumenshchev & Abramowicz 1999, 2000).”
• Radiative efficiency of hot accretion flows (2012, background): “…precisely, the inflow rate; refer to Stone, Pringle & Begelman 1999 for details) decreases with decreasing radius, whether the radiation is weak (Igumenshchev & Abramowicz 1999, 2000; Stone et al. 1999; Stone & Pringle 2001) or strong (Yuan & Bu 2010), following a power-law scaling of radius,…”
• NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH (2015, background): “The study of winds from hot accretion flows can be traced back to Stone, Pringle & Begelman (1999; see also Igumenshchev & Abramowicz 1999, 2000).”
• Hot Accretion Flows Around Black Holes (2014, methodology): “…out without magnetic fields, using 2D hydrodynamic (HD) codes and an α-like prescription for the viscous stress (Igumenshchev et al. 1996, Igumenshchev & Abramowicz 1999, Stone et al. 1999, Igumenshchev & Abramowicz 2000; Igumenshchev et al. 2000, De Villiers & Hawley 2002; Fragile & Anninos 2005).”
• Mass fall-back and accretion in the central engine of gamma-ray bursts (2008, background): “An important feature of an ADAF is that it generally has a strong mass outflow (Stone, Pringle & Begelman 1999; Igumenshchev & Abramowicz 2000), which is believed to be driven by a positive Bernouilli constant (Narayan & Yi 1994, 1995).”
• General relativistic magnetohydrodynamic simulations of magnetically choked accretion flows around black holes (2012, unknown): “For viscous simulations, Igumenshchev & Abramowicz (2000) found ρ ∝ r−1/2 to r−0.7 for Γ = 5/3–4/3, respectively.”
• The Dynamical Structure of Nonradiative Black Hole Accretion Flows (2002, background): “A number of axisymmetric hydrodynamical simulations have been performed (e.g., Igumenshchev & Abramowicz 1999, 2000; Stone, Pringle, & Begelman 1999) that drive accretion by employing an explicit kinematic viscosity, .”
• GRMHD simulations of magnetized advection‐dominated accretion on a non‐spinning black hole: role of outflows (2012, background): “Clear examples of this effect may be seen in the global 1D models of Narayan, Kato & Honma (1997), where the non-self-similar zone extends from the inner boundary to a few tens of gravitational radii.”