Accretion Power in Astrophysics: Contents

By J. Frank, A. King, D. Raine. 2002

1,271 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/c44225b0615cd3b3bac3a062c7127aa844efa957

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In Astronomy and Astrophysics

1. Ramesh Narayan
2. J. E. McClintock
3. A. Tchekhovskoy
4. F. Yuan
5. A. Sa̧dowski
6. J. McKinney
7. P. Hopkins
8. J. Steiner

In Atomic and Molecular Physics, and Optics

1. Ramesh Narayan
2. A. Tchekhovskoy
3. F. Yuan
4. A. Sa̧dowski
5. R. Penna
6. G. Lodato
7. A. Kulkarni
8. Harvard

Citations in the corpus

• Hot Accretion Flows Around Black Holes (2014, methodology): “The most convenient way to investigate this is by plotting the locus of accretion solutions in the two-dimensional plane of accretion rate Ṁ and surface density Σ ≡ 2ρH (e.g., Frank et al. 2002).”
• GRMHD simulations of magnetized advection‐dominated accretion on a non‐spinning black hole: role of outflows (2012, background): “…Novikov & Thorne 1973; Frank, King & Raine 2002), and (2) an advectiondominated accretion flow (ADAF; Narayan & Yi 1994, 1995b; Abramowicz et al. 1995; Ichimaru 1977; see Narayan, Mahadevan & Quataert 1998; Frank et al. 2002; Kato, Fukue & Mineshige 2008; Narayan & McClintock 2008 for reviews).”
• Multidimensional modelling of X-ray spectra for AGN accretion disc outflows (2008, background): “The cooling rate for a population of non-relativistic electrons due to Compton up-scattering of low-energy photons (hν << kTe) can be estimated from the local energy density of such photonsUγ via CCp = 4σTUγ kTe mec (15) whereσT is the Thomson cross-section (see Frank et al. (2002), p. 180).”
• Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. IX. 10 New Observations of Reverberation Mapping and Shortened Hβ Lags (2018, methodology): “Equation (4) is derived from the thin accretion disk model (Shakura & Sunyaev 1973; Frank et al. 2002; see more details in Paper II), and can be used as a substitute for the traditional estimate of the Eddington ratio (e.g., =L L L L10bol Edd 5100 Edd, where Lbol is the bolometric luminosity and…”
• Accretion disc viscosity: how big is alpha? (2007, background): “For a typical dwarf nova in outburst, we find the equipartition field in the outer disc regions to be (Shakura & Sunyaev 1973; Frank et al. 2002) Beq 5.2 × 104 ( α 0.1 )−9/10( Ṁ 1018 g s−1 )17/40( M M )7/16 × ( R 1010 cm )−21/16 G. (4) Here Ṁ is the accretion rate, M is the mass of the central…”
• Formation of millisecond pulsars with CO white dwarf companions – II. Accretion, spin-up, true ages and comparison to MSPs with He white dwarf companions (2012, background): “…Davidson & Ostriker (1973); Ghosh & Lamb (1979a,b); Shapiro & Teukolsky (1983); Ghosh & Lamb (1992); Spruit & Taam (1993); Campana et al. (1998); Frank et al. (2002); Rappaport et al. (2004); Bozzo et al. (2009); D’Angelo & Spruit (2010); Ikhsanov & Beskrovnaya (2012) and references therein.”
• Ultra-stripped supernovae: progenitors and fate (2015, background): “This depends on, for example, whether or not an accretion disk is formed, and whether or not propeller effects are important (e.g. Frank et al. 2002).”
• The Spin of the Near-Extreme Kerr Black Hole GRS 1915+105 (2006, methodology): “The flux emitted by a thin accretion disk around a BH with zero torque at the inner edge is given by (e.g., Frank et al. 2002) F (R) = 3GMṀ 8πR3 [ 1− ( Rin R )1/2 ] , (1) where M is the mass of the BH, Ṁ is the mass accretion rate, R is the cylindrical radius, and Rin is the radius of the inner…”