Magnetically Driven Accretion in the Kerr Metric. III. Unbound Outflows

By Jean-Pierre De Villiers, J. Hawley, Julian Krolik, Shigenobu Hirose. 2004

212 citations recorded by the source corpus.

We have carried out fully relativistic numerical simulations of accretion disks in the Kerr metric. In this paper we focus on the unbound outflows that emerge self-consistently from the accretion flow. These outflows are found in the axial funnel region and consist of two components: a hot, fast, tenuous outflow in the axial funnel proper and a colder, slower, denser jet along the funnel wall. The funnel-wall jet is excluded from the axial funnel by elevated angular momentum and is also pressure-confined by a magnetized corona. Inside the funnel, a large-scale poloidal magnetic field spontaneously arises from the coupled dynamics of accretion and outflow, although there was no large-scale field in the initial state. Black hole rotation is not required to produce these unbound outflows, but their strength is enhanced by black hole spin. When the black hole spins rapidly, the energy ejected can be tens of percent of the accreted rest mass. At low spin, kinetic energy and enthalpy of the matter dominate the outflow energetics; at high spin, the balance shifts to Poynting flux. We compare the outflows observed in our simulations with those seen in other simulations.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/61b9498fdd4257194cda4529f2d77f90e544548c

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In Astronomy and Astrophysics

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

Citations in the corpus

• Magnetic acceleration of relativistic AGN jets (2007, methodology): “This picture finds support in recent numerical simulations (e.g McKinney & Gammie 2004; De Villiers et al. 2005).”
• Long-term GRMHD simulations of neutron star merger accretion discs: implications for electromagnetic counterparts (2018, background): “The physics of the polar unbound outflows in threedimensional GRMHD simulations of accretion disks around spinning black holes has been studied by De Villiers et al. (2005) and Hawley & Krolik (2006).”
• The Influence of Magnetic Field Geometry on the Evolution of Black Hole Accretion Flows: Similar Disks, Drastically Different Jets (2007, methodology): “For example, De Villiers et al. (2005) simulated the evolution of a torus with an initial toroidal field around a Schwarzschild black hole and noted the lack of any resulting jet, but did not consider why no jet formed.”
• ASSESSING QUANTITATIVE RESULTS IN ACCRETION SIMULATIONS: FROM LOCAL TO GLOBAL (2011, background): “…mechanisms by which a large-scale field magnetic field can be attached to a black hole, either inward transport of truly large-scale field (Beckwith et al. 2009) or spontaneous, if temporary, inflation of field loops within the accretion flow (McKinney & Gammie 2004; De Villiers et al. 2003, 2005).”
• Short-hard gamma-ray bursts (2007, methodology): “…Mineshige & Shibata, 2004) to GR simulations using a Kerr metric in two dimensions (McKinney & Gammie, 2004; McKinney, 2005, 2006) and in three dimensions (De Villiers, Hawley & Krolik, 2003; De Villiers et al. , 2005; Hirose et al. , 2004; Krolik, Hawley & Hirose, 2005; Hawley & Krolik, 2006).”
• SUPERNOVA LIGHT CURVES POWERED BY FALLBACK ACCRETION (2012, background): “Such radiatively inefficient accretion flows are expected to produce large-scale outflows (Narayan & Yi 1994; Blandford & Begelman 1999; Igumenshchev & Abramowicz 2000; Pen et al. 2003; Begelman 2012; McKinney et al. 2012) and/or Poynting flux dominated jets (De Villiers et al. 2005; McKinney 2006).”
• Jet-regulated cooling catastrophe (2010, result): “…is also in good agreement with the average value obtained by general relativistic magnetohydrodynamic numerical simulations of the accretion-ejection mechanism in accretion discs around spinning BHs (e.g. De Villiers et al. 2005, Hawley & Krolik 2006 or Benson & Babul 2009 and references therein).”
• Grand unification of AGN activity in the ΛCDM cosmology (2009, background): “Embedding such calculations in a fully general relativistic framework produces relativistic jets from the accretion flow, and the collima- c© 0000 RAS tion and jet power depend on the BH spin (McKinney & Gammie 2004; De Villiers et al. 2005; Hawley & Krolik 2006).”
• No evidence for black hole spin powering of jets in X-ray binaries (2010, background): “McKinney (2005) however arrived at theopposite conclusion, deriving a very strong dependence of jet power on black hole spin (see also De Villiers et al. 2005 for parallelwork on the influence of spin on jets from numerical simulations).”
• Going with the Flow: Can the Base of Jets Subsume the Role of Compact Accretion Disk Coronae? (2005, result): “…model presented here is consistent with the physical picture seen in relativistic MHD simulations (Meier & Nakamura 2004; McKinney & Gammie 2004; De Villiers et al. 2005), where the corona is not static but instead is a windy hot material blowing away from the inner regions of the accretion flow.”
• Efficient Generation of Jets from Magnetically Arrested Accretion on a Rapidly Spinning Black Hole (2011, background): “Recent timedependent general relativistic magnetohydrodynamic (GRMHD) numerical simulations have found a rather low efficiency, ηBZ 20 per cent, even when the central BH is nearly maximally spinning (De Villiers et al. 2005; McKinney 2005; Hawley & Krolik 2006; Barkov & Baushev 2011).”
• Hot Accretion Flows Around Black Holes (2014, methodology): “Representative results from 3D GRMHD simulations can be found in the series of early papers by De Villiers and collaborators (De Villiers et al. 2003, 2005; Hirose et al. 2004; Krolik et al. 2005) and Gammie and collaborators (Gammie et al. 2004, McKinney & Gammie 2004, McKinney 2006).”
• Simulations of ultrarelativistic magnetodynamic jets from gamma‐ray burst engines (2008, background): “…the framework of GRMHD, of magnetized accretion discs around spinning BHs naturally produce mildly relativistic jets (McKinney & Gammie 2004; De Villiers et al. 2005; McKinney 2005b; Hawley & Krolik 2006; Beckwith et al. 2008; Barkov & Komissarov 2008a) as well as relativistic jets with…”
• ECHO: a Eulerian conservative high-order scheme for general relativistic magnetohydrodynamics and magnetodynamics (2007, background): “…of jet formation in a black hole-accretion disk system (Koide et al. 2000; De Villiers et al. 2003; Mizuno et al. 2004; Nishikawa et al. 2005; De Villiers et al. 2005; McKinney 2006b; Hawley & Krolik 2006; Koide et al. 2006), the time evolution of a neutron star magnetosphere, in both the MHD…”
• Magnetically Driven Jets in the Kerr Metric (2005, methodology): “The boost factor W is then computed using S , but because the definition of the inertia used in the code includesW, it is found from the solution to a quartic equation derived from 4-normalization (De Villiers et al. 2005b).”
• GRMHD simulations of magnetized advection‐dominated accretion on a non‐spinning black hole: role of outflows (2012, background): “The jets on the other hand were relativistic and escaped easily, though carrying very little mass. Jets have been studied in detail by a number of authors (McKinney & Gammie 2004; De Villiers et al. 2005; McKinney 2006).”