Black-Hole Accretion Disks: Towards a New Paradigm

By S. Kato, J. Fukue, S. Mineshige. 2008

486 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/3d0bf85c3a4120e92672bdbdf932d617bf6f874e

How researchers see this paper

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

1. Ramesh Narayan
2. A. Sa̧dowski
3. Bing Zhang
4. J. McKinney
5. Tong Liu
6. Nicholas C. Stone
7. B. Metzger
8. F. Yuan

Citations in the corpus

• THE EVENT HORIZON OF SAGITTARIUS A* (2009, background): “…surface emission to remain undetected would require unphysically large radiative efficiencies, greater than 99.6%, as compared to the typical efficiencies in active galactic nuclei (AGNs) of 10% (Kato et al. 2008) and the meager efficiency implicated in Sgr A*, 0.01%–1% (Narayan & McClintock 2008).”
• Circularization of Tidally Disrupted Stars around Spinning Supermassive Black Holes (2015, background): “While the mass-to-energy conversion efficiency reaches ≈ 42% for an extreme Kerr black hole in a prograde rotation, it is only ≈ 4% for the retrograde case (Kato et al. 2008), suggesting a wide range of bolometric disk luminosities depending on the relative inclination of disk and SMBH spin.”
• GLOBAL STRUCTURE OF THREE DISTINCT ACCRETION FLOWS AND OUTFLOWS AROUND BLACK HOLES FROM TWO-DIMENSIONAL RADIATION-MAGNETOHYDRODYNAMIC SIMULATIONS (2011, background): “…inefficient accretion flow (RIAF) model, which are proposed as models for the accretion flow with higher (∼ LE) and lower luminosities, respectively (Shakura & Sunyaev 1973; Ichimaru 1977; Rees et al. 1982; Abramowicz et al. 1988; Narayan & Yi 1994, see Kato et al. 2008 for an extensive review).”
• Global Radiation-Magnetohydrodynamic Simulations of Black-Hole Accretion Flow and Outflow: Unified Model of Three States (2009, background): “For example, the disk viscosity, the most important key ingredient for the accretion disk theory, is prescribed by a phenomenological α-viscosity model, whereby the viscous torque is proportional to the pressure (Kato et al. 2008), although its physical basis is not clear.”
• Hot Accretion Flows Around Black Holes (2014, background): “…flow with viscous transport of angular momentum — is the celebrated thin disk model developed in the early 1970s (Shakura & Sunyaev 1973, Novikov & Thorne 1973, Lynden-Bell & Pringle 1974; see reviews by Pringle 1981, Frank et al. 2002, Kato et al. 2008, Abramowicz & Fragile 2013, Blaes 2013).”
• Neutrino-dominated accretion flows as the central engine of gamma-ray bursts (2017, background): “Here xms = 3 + Z2 − √ (3 − Z1)(3 + Z1 + 2Z2), where Z1 = 1 + (1 − a2∗)1/3[(1 + a∗)1/3 + (1 − a∗)1/3] and Z2 = √ 3a2∗ + Z 2 1 for 0 < a∗ < 1 (e.g., Bardeen et al. 1972; Kato et al. 2008; Zalamea & Beloborodov 2011; Liu et al. 2015c).”