Hot Accretion Flows Around Black Holes

By F. Yuan, Ramesh Narayan. 2014

1,147 citations recorded by the source corpus.

Black hole accretion flows can be divided into two broad classes: cold and hot. Whereas cold accretion flows consist of cool optically thick gas and are found at relatively high mass accretion rates, hot accretion flows, the topic of this review, are virially hot and optically thin, and occur at lower mass accretion rates. They are described by accretion solutions such as the advection-dominated accretion flow and luminous hot accretion flow. Because of energy advection, the radiative efficiency of these flows is in general lower than that of a standard thin accretion disk. Moreover, the efficiency decreases with decreasing mass accretion rate. Observations show that hot accretion flows are associated with jets. In addition, theoretical arguments suggest that hot flows should produce strong winds. Hot accretion flows are believed to be present in low-luminosity active galactic nuclei and in black hole X-ray binaries in the hard and quiescent states. The prototype is Sgr A*, the ultralow-luminosity supermassive black hole at our Galactic center. The jet, wind, and radiation from a supermassive black hole with a hot accretion flow can interact with the external interstellar medium and modify the evolution of the host galaxy.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/36c2c5741c91e0f97a4c80dcc09e5b01bdead114

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Citations in the corpus

Raining on black holes and massive galaxies: the top-down multiphase condensation model (2016, neutral): “CCA differs from hot models (Bondi, ADAF, etc.; Yuan & Narayan 2014) that all predict a cuspy X-ray profile.”
NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH (2015, methodology): “For example, it has been found that in the MAD state, the power of the BZ jet will dominate the disk jet (Narayan, Igumenshchev & Abramowicz 2003; Tchekhovskoy, Narayan & McKinney 2010; Penna et al.2013a; see review by Yuan & Narayan 2014).”
Active galactic nuclei: what’s in a name? (2017, background): “There is compelling theoretical and observational evidence that the structure of the flow changes with L/LEdd (e.g. Narayan and Yi 1994; Vasudevan and Fabian 2009; Yuan and Narayan 2014), with higher L/LEdd systems producing stronger emission from an optically-thick accretion disk in the optical and”
An Update on Monitoring Stellar Orbits in the Galactic Center (2016, background): “Knowing the mass of and distance to Sgr A* is the reason why the Galactic Center is a unique testbed concerning massive black holes and their vicinities for numerous models in many branches of astrophysics (Yuan & Narayan 2014).”
First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback (2019, background): “General relativistic (GR)MHD simulations explore black hole outflow phenomena including both winds and jets (Blandford & Begelman 1999; McKinney et al. 2014), recently reviewed in Yuan & Narayan (2014).”
Shadows of spherically symmetric black holes and naked singularities (2018, background): “…simplicity, we assume that the gas is a single-temperature plasma, although it is likely that the accreting gas in Sgr A∗ is a two-temperature plasma (Yuan & Narayan 2014) MNRAS 000, 1–15 (2018) gularity with M0 = 0.7 (green) and M0 = 0.6 (blue), and JMN-2 naked singularity with λ = 0.8 (magenta)…”
General relativistic magnetohydrodynamical simulations of the jet in M 87 (2015, background): “The bolometric luminosity of the core is estimated to beL/LEdd ≈ 10−7, which suggests that the powerful (the jet power isP j ≈ 1045erg s−1, de Gasperin et al. 2012) kpc-scale jet emerges from a radiatively inefficient accretion flow (RIAF) onto the supermassive BH (Yuan & Narayan 2014).”
Simulating galaxy formation with black hole driven thermal and kinetic feedback (2016, background): “However, there are also theoretical indications pointing to the existence of kinetic winds in the low-accretion state (Igumenshchev & Abramowicz 1999; Stone et al. 1999; Yuan & Narayan 2014; Yuan et al. 2015; Bu et al. 2016; Sa̧dowski et al. 2016).”
First Sagittarius A* Event Horizon Telescope Results. V. Testing Astrophysical Models of the Galactic Center Black Hole (2022, background): “…form of a radiatively inefficient/advection-dominated accretion flow (RIAF/ADAF, as proposed by Ichimaru 1977; Rees et al. 1982; Narayan & Yi 1994, 1995a, 1995b; Narayan et al. 1996, 1998; Yuan & Narayan 2014) rather than in the form of a radiatively efficient thin disk (Shakura & Sunyaev 1973).”
The Event Horizon General Relativistic Magnetohydrodynamic Code Comparison Project (2019, background): “In both cases, the accretion flow is believed to form an optically thin disk that is geometrically thick and therefore has temperature comparable to the virial temperature (see Yuan & Narayan 2014 for a review).”
Testing the rotational nature of the supermassive object M87* from the circularity and size of its first image (2019, background): “[22] F.”
On the charge of the Galactic centre black hole (2018, background): “…(10) where the ratio of the thickness of the accretion flow to the radial length-scale is expected to be of the order of unity since the accretion flow around Sgr A* is generally considered to be optically thin and geometrically thick as for hot accretion flows in general (Yuan & Narayan 2014).”
Black holes with scalar hair in light of the Event Horizon Telescope (2020, methodology): “The ADAF model is believed to accurately describe the accretion flow around low-redshift supermassive BHs, including M87* and SgrA* [215].”
The Shadow of a Spherically Accreting Black Hole (2019, background): “The hot accretion flow in Sagittarius A∗, M87, and most other galactic nuclei consists of a geometrically thick, quasi-spherical disk (Yuan & Narayan 2014), whose characteristics lie somewhere between the pure spherical model considered here and the geometrically thin disks considered in earlier…”