GLOBAL STRUCTURE OF THREE DISTINCT ACCRETION FLOWS AND OUTFLOWS AROUND BLACK HOLES FROM TWO-DIMENSIONAL RADIATION-MAGNETOHYDRODYNAMIC SIMULATIONS

By K. Ohsuga, S. Mineshige. 2011

255 citations recorded by the source corpus.

We present the detailed global structure of black hole accretion flows and outflows through newly performed two-dimensional radiation-magnetohydrodynamic simulations. By starting from a torus threaded with weak toroidal magnetic fields and by controlling the central density of the initial torus, ρ0, we can reproduce three distinct modes of accretion flow. In model A, which has the highest central density, an optically and geometrically thick supercritical accretion disk is created. The radiation force greatly exceeds the gravity above the disk surface, thereby driving a strong outflow (or jet). Because of mild beaming, the apparent (isotropic) photon luminosity is ∼22LE (where LE is the Eddington luminosity) in the face-on view. Even higher apparent luminosity is feasible if we increase the flow density. In model B, which has moderate density, radiative cooling of the accretion flow is so efficient that a standard-type, cold, and geometrically thin disk is formed at radii greater than ∼7 RS (where RS is the Schwarzschild radius), while the flow is radiatively inefficient otherwise. The magnetic-pressure-driven disk wind appears in this model. In model C, the density is too low for the flow to be radiatively efficient. The flow thus becomes radiatively inefficient accretion flow, which is geometrically thick and optically thin. The magnetic-pressure force, together with the gas-pressure force, drives outflows from the disk surface, and the flow releases its energy via jets rather than via radiation. Observational implications are briefly discussed.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/7b41e653c1eb547a35ad61c5caeac61b881a69c9

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In Astronomy and Astrophysics

1. Ramesh Narayan
2. A. Sa̧dowski
3. A. Tchekhovskoy
4. F. Yuan
5. J. McKinney
6. Yucong Zhu
7. R. Penna
8. S. Davis

In Nuclear and High Energy Physics

1. Ramesh Narayan
2. A. Sa̧dowski
3. A. Tchekhovskoy
4. F. Yuan
5. J. McKinney
6. R. Penna
7. Yucong Zhu
8. A. Kulkarni

Citations in the corpus

• A GLOBAL THREE-DIMENSIONAL RADIATION MAGNETO-HYDRODYNAMIC SIMULATION OF SUPER-EDDINGTON ACCRETION DISKS (2014, methodology): “Comparison with Previous Simulations Super-Eddington accretion disks for non-spinning black holes have been studied extensively with 2D axisymmetric radiation hydro or MHD simulations (Ohsuga et al. 2005, 2009; Ohsuga & Mineshige 2011, 2013; Sa̧dowski et al. 2014).”
• Hot Accretion Flows Around Black Holes (2014, background): “Ohsuga and collaborators (e.g., Ohsuga et al. 2009, Ohsuga & Mineshige 2011) have carried out simulations with full radiative transfer and have studied a wide range of accretion rates.”
• DRIVING OUTFLOWS WITH RELATIVISTIC JETS AND THE DEPENDENCE OF ACTIVE GALACTIC NUCLEUS FEEDBACK EFFICIENCY ON INTERSTELLAR MEDIUM INHOMOGENEITY (2012, background): “…observational estimates of the energetics of AGN outflows, one would expect this factor to be of order 0.001–0.01 (e.g., McKernan et al. 2007; Moe et al. 2009; Tombesi et al. 2010), which is also found in disk-wind simulations (Kurosawa et al. 2009; Takeuchi et al. 2010; Ohsuga & Mineshige 2011).”
• Semi-implicit scheme for treating radiation under M1 closure in general relativistic conservative fluid dynamics codes (2012, methodology): “…Blaes, Hirose & Krolik 2007; Krolik, Hirose & Blaes 2007; Hirose, Blaes & Krolik 2009a; Hirose, Krolik & Blaes 2009b; Blaes et al. 2011), and even a few full disc simulations have been done with a non-relativistic code using flux-limited diffusion (Ohsuga et al. 2009; Ohsuga & Mineshige 2011).”
• Powerful Outflows and Feedback from Active Galactic Nuclei (2015, background): “Ohsuga & Mineshige (2011) show in detail that winds with these properties (their Models A and B) are a natural outcome of mildly super–Eddington accretion.”
• GRMHD simulations of magnetized advection‐dominated accretion on a non‐spinning black hole: role of outflows (2012, background): “The latter variety of ADAF is referred to as a ‘slim disc’ (Abramowicz et al. 1988) and requires a radiation MHD code to simulate (see Ohsuga et al. 2009; Ohsuga & Mineshige 2011; and references therein). flow (RIAF).”
• Three-dimensional simulations of supercritical black hole accretion discs - luminosities, photon trapping and variability (2015, methodology): “The pioneering initial work was based on Newtonian codes with crude (flux-limited diffusion) radiative transport (Ohsuga et al. 2009; Ohsuga & Mineshige 2011).”
• Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, methodology): “…code and flux-limited diffusion, super-Eddington accretion flows have been simulated and their spectra computed (Ohsuga et al. 2003; Ohsuga et al. 2005; Ohsuga 2006; Ohsuga et al. 2009; Ohsuga & Mineshige 2011; Kawashima et al. 2012; Mineshige et al. 2012; Takeuchi et al. 2013; Yang et al. 2013).”
• Ultraluminous X-ray sources in the Chandra and XMM-Newton era (2011, background): “…mass supply ṁ ≈ 5 can produce a total luminosity≈ 1.7LEdd (in rough agreement with the standard analytical scaling used earlier), and an apparent luminosity≈ 22LEdd for face-on observers, due to mild collimation in the magnetized outflow (Mineshige & Ohsuga 2011; Ohsuga & Mineshige 2011).”
• Global simulations of axisymmetric radiative black hole accretion discs in general relativity with a mean-field magnetic dynamo (2014, background): “The most common approach in the past was to invoke flux limited diffusion (FLD) (e.g., Hirose et al. 2009b; Blaes et al. 2011; Ohsuga et al. 2009; Ohsuga & Mineshige 2011), which assumes that the radiative flux follows the gradient of the radiative energy density.”
• The ultraluminous state revisited: fractional variability and spectral shape as diagnostics of super-Eddington accretion (2013, background): “Such a wind is expected to occur at super-Eddington accretion rates (Poutanen et al. 2007; Dotan & Shaviv 2011; Ohsuga & Mineshige 2011), indeed the supercritical accretion flow simulations of Kawashima et al. (2012) produce such a wind, and find that it takes the form of a funnel.”
• Numerical simulations of super-critical black hole accretion flows in general relativity (2013, methodology): “Our results for a non-rotating BH are in qualitative agreement with models A in Ohsuga et al. (2009) and Ohsuga & Mineshige (2011), which were simulated using a non-relativistic MHD code with flux-limited diffusion.”