Direct numerical simulations of the Blandford–Znajek effect

By Serguei Komissarov. 2001

137 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/440dfa4b026832b0bb01dd17f406486712017c37

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In Astronomy and Astrophysics

1. Ramesh Narayan
2. J. McKinney
3. A. Tchekhovskoy
4. F. Yuan
5. A. Sa̧dowski
6. Bing Zhang
7. T. Johannsen
8. Pawan Kumar

In Nuclear and High Energy Physics

1. Ramesh Narayan
2. A. Tchekhovskoy
3. J. McKinney
4. A. Sa̧dowski
5. F. Yuan
6. Bing Zhang
7. J. Dexter
8. R. Penna

Citations in the corpus

• BLACK HOLE SPIN AND THE RADIO LOUD/QUIET DICHOTOMY OF ACTIVE GALACTIC NUCLEI (2009, methodology): “Numerical simulations by Komissarov (2001) showed that the BZ77 effect achieves maximum efficiency when Ω ≈ ΩH/2.”
• Total and Jet Blandford-Znajek Power in the Presence of an Accretion Disk (2005, methodology): “Forcefree numerical models agree with the above BZ model (Komissarov 2001).”
• EFFICIENCY OF MAGNETIC TO KINETIC ENERGY CONVERSION IN A MONOPOLE MAGNETOSPHERE (2009, background): “…consider the limit of infinitely high magnetization,ρ → 0, i.e. the force-free limit (Goldreich & Julian 1969; Okamoto 1974; Blandford 1976; Lovelace 1976; Blandford & Znajek 1977; MacDonald & Thorne 1982; Fendt et al. 1995; Komissarov 2001, 2002a,b; McKinney 2006a; Narayan et al. 2007; TMN08).”
• NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH (2015, background): “…to the disk jet, a Poynting flux-dominated jet (BZ jet) will be produced through the black hole horizon, powered by the black hole spin (Blandford & Znajek 1976; Komissarov 2001; McKinney 2005; Hawley & Krolik 2006; Tchekhovskoy, Narayan & McKinney 2010, 2011; Penna, Narayan & Sadowski 2013a).”
• Prograde and retrograde black holes: whose jet is more powerful? (2012, unknown): “Here rg = GM/c2, M, and a are BH gravitational radius, mass, and dimensionless spin, ΩH = ac/2rH is BH angular frequency, f (ΩH) ≈ 1 + 1.38(ΩHrg/c)2 − 9.2(ΩHrg/c)4 is a high-spin correction, dAθϕ = √−g dθdϕ is an area element in θ−ϕ plane, and g is the metric determinant (Tchekhovskoy et al. 2010, s”
• Energy, momentum and mass outflows and feedback from thick accretion discs around rotating black holes (2013, methodology): “The main predictions of the Blandford– Znajek (BZ) jet model are supported by general relativistic magnetohydrodynamic (GRMHD) simulations (Komissarov 2001; Hirose et al. 2004; De Villiers et al. 2005; McKinney 2005; Hawley & Krolik 2006; Beckwith, Hawley & Krolik 2008; Tchekhovskoy, Narayan &…”
• First Sagittarius A* Event Horizon Telescope Results. V. Testing Astrophysical Models of the Galactic Center Black Hole (2022, methodology): “We model the plasma flow around Sgr A* using ideal, nonradiative GRMHD in the Kerr metric, with a* a free parameter (see, e.g., Koide et al. 1999; Komissarov 2001; Gammie et al. 2003; De Villiers & Hawley 2003; Anninos et al. 2005; Del Zanna et al. 2007).”
• Spacetime approach to force-free magnetospheres (2014, background): “Thus one effectively solves the stream equation through time-dependent evolution (e.g., Komissarov 2001; McKin-ney 2006; Spitkovsky 2006; Komissarov & McKinney 2007).”
• ECHO: a Eulerian conservative high-order scheme for general relativistic magnetohydrodynamics and magnetodynamics (2007, methodology): “…of these applications include the validation of the Blandford-Znajek mechanism for the extraction of rotational energy from a Kerr black hole (Komissarov 2001; Koide 2003; Komissarov 2004; McKinney & Gammie 2004; Komissarov 2005; McKinney 2005), the spin evolution of a black hole under the…”
• Time‐dependent, force‐free, degenerate electrodynamics (2002, methodology): “In fact, we have already constructed a 2D scheme for the Kerr space-time and used it (Komissarov 2001) to study the Blandford-Znajek mechanism (Blandford & Znajek 1977) for the extraction of rotational energy from black holes.”
• Hot Accretion Flows Around Black Holes (2014, methodology): “This enforces strict mass, momentum and total energy conservation, as exemplified by the pioneering relativistic MHD code of Komissarov (1999, 2001), the GRMHD codes HARM (Gammie et al. 2003) and COSMOS++ (Anninos et al. 2005), and the Newtonian MHD code ATHENA (Stone et al. 2008).”
• A Measurement of the Electromagnetic Luminosity of a Kerr Black Hole (2004, methodology): “See sections 3.2 and 3.3 for a discussion. a, but Komissarov (2001) has integrated the equations of force-free electrodynamics for a monopolar field geometry and at a = 0.5 finds that ω rises from ≈ 0.495ΩH at the pole to ≈ 0.51ΩH at the equator, so this seems unlikely.”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “…relativistic MHD have led to significant progress in our understanding of the magnetic jet launching mechanism, propagation and acceleration (e.g. Komissarov, 2001, 2004; McKinney, 2006; Komissarov, 2007; Komissarov et al., 2007; McKinney and Narayan, 2007; Tchekhovskoy et al., 2008; Komissarov…”
• Simulations of the axisymmetric magnetospheres of neutron stars (2006, result): “The very first numerical simulations of this kind, of the monopole magnetospheres of black holes, seemed to confirm the suitability of this approach (Komissarov 2001).”
• Beyond ideal MHD: towards a more realistic modelling of relativistic astrophysical plasmas (2008, background): “…the last decade to study a number of phenomena in relativistic astrophysics and in fully nonlinear regimes (Komissarov 1999b; Koide et al. 1999; Komissarov 2001; Koldoba et al. 2002; Gammie et al. 2003; Del Zanna et al. 2003; Anninos et al. 2005; Duez et al. 2005; Shibata & Sekiguchi 2005;…”
• Electrodynamics of black hole magnetospheres (2004, methodology): “Given the fact that, in such a degenerate regime, the full system of relativistic MHD presents a real challenge for numerical methods (see Komissarov 2001a; Gammie, McKinney & Tóth 2003), it is difficult not to conclude that the electrodynamic approach is more suitable.”
• Simulations of ultrarelativistic magnetodynamic jets from gamma‐ray burst engines (2008, background): “…& Julian 1969; Okamoto 1974; Blandford 1976; Lovelace 1976; Blandford & Znajek 1977; MacDonald & Thorne 1982; Fendt, Camenzind & Appl 1995; Komissarov 2001, 2002; McKinney 2006a), which corresponds to a magnetically dominated plasma in which particle rest mass and temperature are…”
• Electromagnetic Extraction of Energy from Kerr Black Holes (2005, background): “It seems that almost the same situation can be seen in recent FFDE numerical simulations by Komissarov (2001, 2002a, 2004).”
• Relativistic MHD simulations of core-collapse GRB jets: 3D instabilities and magnetic dissipation (2015, background): “It is commonly agreed that these jets are powered electromagnetically, most likely by the winding of magnetic field lines that thread a rotating central compact object (Blandford & Znajek 1977; Komissarov 2001; Tchekhovskoy et al. 2010a).”