GRMHD simulations of magnetized advection‐dominated accretion on a non‐spinning black hole: role of outflows

By Ramesh Narayan, A. Sa̧dowski, R. Penna, A. Kulkarni. 2012

356 citations recorded by the source corpus.

We present results from two long-duration general relativistic magneto-hydrodynamic (GRMHD) simulations of advection-dominated accretion around a non-spinning black hole. The first simulation was designed to avoid significant accumulation of magnetic flux around the black hole. This simulation was run for a time of 200 000 GM/c3 and achieved inflow equilibrium out to a radius ∼90 GM/c2. Even at this relatively large radius, the mass outflow rate is found to be only 60 per cent of the net mass inflow rate into the black hole. The second simulation was designed to achieve substantial magnetic flux accumulation around the black hole in a magnetically arrested disc. This simulation was run for a shorter time of 100 000 GM/c3. Nevertheless, because the mean radial velocity was several times larger than in the first simulation, it reached inflow equilibrium out to a radius ∼170 GM/c2. Here, becomes equal to at r ∼ 160 GM/c2. Since the mass outflow rates in the two simulations do not show robust convergence with time, it is likely that the true outflow rates are lower than our estimates. The effect of black hole spin on mass outflow remains to be explored. Neither simulation shows strong evidence for convection, though a complete analysis including the effect of magnetic fields is left for the future.

Subfields: Astronomy and Astrophysics, Biomedical Engineering

View Paper: https://www.semanticscholar.org/paper/3bf7c428804c9ddeda042cd911fbfbbfc760035a

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In Astronomy and Astrophysics

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

In Biomedical Engineering

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

Citations in the corpus

• Long-term GRMHD simulations of neutron star merger accretion discs: implications for electromagnetic counterparts (2018, result): “Because of these differences, the results of previous work that focused on the sub-relativistic disk outflow (e.g., Narayan et al. 2012; Sa̧dowski et al. 2013) are not directly applicable to the merger problem .”
• First M87 Event Horizon Telescope Results. V. Physical Origin of the Asymmetric Ring (2019, neutral): “Models with 1f ~ are conventionally referred to as Standard and Normal Evolution (SANE; Narayan et al. 2012; Saḑowski et al (2013a)) models; models with maxf f~ are conventionally referred to as Magnetically Arrested Disk (MAD; Igumenshchev et al. 2003; Narayan et al. 2003) models.”
• Semi-implicit scheme for treating radiation under M1 closure in general relativistic conservative fluid dynamics codes (2012, methodology): “…De Villiers-P., Hawley & Krolik 2003; Gammie, McKinney & Tóth 2003; Anninos, Fragile & Salmonson 2005; Del Zanna et al. 2007), and ADAF-like models have been simulated using these (see McKinney, Tchekhovskoy & Blandford 2012; Narayan et al. 2012; Tchekhovskoy & McKinney 2012 for recent work).”
• NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. I. A LARGE RADIAL DYNAMICAL RANGE AND THE DENSITY PROFILE OF ACCRETION FLOW (2012, background): “Narayan et al. (2012) most recently presented two long-duration GRMHD simulations of a hot accretion flow, in which the accumulation of magnetic flux around the black hole does and does not occur (“MAD” and “SANE” models), respectively.”
• Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, methodology): “This is probably an upper limit (see Narayan et al. 2012; Sa̧dowski et al. 2013b).”
• NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. II. NATURE, ORIGIN, AND PROPERTIES OF OUTFLOWS AND THEIR POSSIBLE OBSERVATIONAL APPLICATIONS (2012, background): “13 (see also Igumenshchev, Narayan & Abramowicz 2003; Mckinney, Tchekhovskoy & Blandford 2012; and Narayan et al. 2012).”
• Magnetic Reconnection and Hot Spot Formation in Black Hole Accretion Disks (2020, background): “In the Standard And Normal Evolution (SANE, Narayan et al. 2012; Sadowski et al. 2013) state a fully turbulent accretion disk can develop due to a smaller magnetic flux (see e.g., Porth et al. 2019), and current sheets can ubiquitously form and interact with the turbulent flow.”
• The Event Horizon General Relativistic Magnetohydrodynamic Code Comparison Project (2019, background): “Chael et al. (2019) and Narayan et al. (2012) also included magnetic and radiative contributions.”
• Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers (2014, background): “…(e.g. Fromang & Papaloizou 2007; Sorathia et al. 2012; Hawley et al. 2013), impact of the global magnetic field topology (e.g. Beckwith, Hawley & Krolik 2008), or the relevance of additional instabilities besides the magnetorotational instability (e.g. Narayan et al. 2012; Yuan, Bu & Wu 2012).”
• Global simulations of axisymmetric radiative black hole accretion discs in general relativity with a mean-field magnetic dynamo (2014, methodology): “…accretion flows we performed suggest that the radius outside which outflow in a wind is present (R ≈ 20 and R ≈ 10 for a∗ = 0 and 0.9, respectively) is smaller than for corresponding simulations of radiatively inefficient, optically thin disks (Narayan et al. 2012; Sa̧dowski et al. 2013b).”
• Energy, momentum and mass outflows and feedback from thick accretion discs around rotating black holes (2013, methodology): “Narayan et al. (2012) have shown that for a∗ = 0 models such a magnetically driven wind from the accretion disc itself does not extend all the way towards the BH but stops around r = 40.”
• First Sagittarius A* Event Horizon Telescope Results. V. Testing Astrophysical Models of the Galactic Center Black Hole (2022, background): “…hole equator, ºM mass accretion rate), divides the outcome into two states: the MAD state (e.g., BisnovatyiKogan & Ruzmaikin 1974; Igumenshchev et al. 2003; Narayan et al. 2003; Tchekhovskoy et al. 2011) and the SANE state (e.g., De Villiers et al. 2003; Gammie et al. 2003; Narayan et al. 2012).”
• Numerical simulations of super-critical black hole accretion flows in general relativity (2013, methodology): “…edge of the disk (Shafee et al. 2008; Penna et al. 2010; Noble et al. 2011), jets (e.g., Tchekhovskoy et al. 2010a,b, 2011; Tchekhovskoy & McKinney 2012a; Narayan et al. 2010; Penna et al. 2013b), outflows (e.g., Narayan et al. 2012b; Sa̧dowski et al. 2013b), viscosity (e.g., Penna et al. 2013a).”
• Radiative efficiency of hot accretion flows (2012, methodology): “So, throughout this paper, we adopt a single value for s. Yuan, Bu & Wu (2012a) have investigated the origin of such a profile and have concluded that they are a result of mass loss in the outflow (see Narayan et al. 2012 for an alternative view).”
• Formation of precessing jets by tilted black hole discs in 3D general relativistic MHD simulations (2017, background): “However, the behaviour of jets produced by tilted discs with smaller magnetic fluxes, in the so-called standard and normal evolution (Narayan et al. 2012) regime, and/or smaller radial extents remains completely unexplored.”