Magnetically Driven Jets in the Kerr Metric

By J. Hawley, Julian Krolik. 2005

283 citations recorded by the source corpus.

We compute a series of three-dimensional general relativistic magnetohydrodynamic simulations of accretion flows in the Kerr metric and investigate the properties of the resulting unbound outflows. The strength of the outflows increases sharply with increasing black hole rotation rate. Several generic features are observed. The mass in the outflow in concentrated in a hollow cone whose opening angle is largely determined by the effective potential for matter with specific angular momentum comparable to that of the innnermost stable circular orbit. The pressure in the accretion disk's corona provides the dominant force accelerating the matter outward. The principle element shaping the outflow is therefore the centrifugal barrier preventing accreting matter from coming close to the rotation axis. The funnel inside the centrifugal barrier contains very little matter and is dominated by electromagnetic fields that rotate at a rate tied closely to the rotation of the black hole, even when the black hole spins in a sense opposite to the rotation of the accretion flow. These fields carry an outward-going Poynting flux whose immediate energy source is the rotating spacetime of the Kerr black hole. When the spin parameter a/M of the black hole exceeds ≃0.9, the energy carried to infinity by these outflows can be comparable to the nominal radiative efficiency predicted in the Novikov-Thorne model. Similarly, the expelled angular momentum can be comparable to that accreted by the black hole. Both the electromagnetic and the matter outflows contribute significantly to the energy and angular momentum of the outflow.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/038b404c85ab6e6625515952bdb3e80491f9f7f9

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Citations in the corpus

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).”
Stability of relativistic jets from rotating, accreting black holes via fully three-dimensional magnetohydrodynamic simulations (2008, background): “…jet from an unresolved Keplerian disc (e.g., Tchekhovskoy et al. 2008), and to evolving both the disc and jet (e.g., Hawley et al. 2001; McKinney & Gammie 2002, 2004; Kigure & Shibata 2005; McKinney 2005; Hawley & Krolik 2006; McKinney 2006a; McKinney & Narayan 2007a,b; Komissarov & McKinney 2007).”
The electromagnetic signals of compact binary mergers (2012, background): “There are several mechanisms by which this could be achieved (e.g. Blandford & Znajek 1977; Piran 2004; Hawley & Krolik 2006; Lee & Ramirz-Ruiz 2007; Nakar 2007).”
Mechanical feedback from active galactic nuclei in galaxies, groups and clusters (2012, background): “Spinning black holes launch Poynting flux jets along the black hole’s spin axis (Nakamura et al 2008) that carry very little matter with them (Hawley and Krolik 2006).”
Global Radiation-Magnetohydrodynamic Simulations of Black-Hole Accretion Flow and Outflow: Unified Model of Three States (2009, background): “…1991), multi-dimensional global magneto-hydrodynamics (MHD) simulations are being rather extensively performed recently as a model for the disks with low luminosities (Matsumoto 1999; Machida et al. 2000; Hawley & Krolik 2001; Koide et al. 2001; De Villiers et al. 2003; Hawley & Krolik 2006) .”
Self-regulated growth of supermassive black holes by a dual jet-heating active galactic nucleus feedback mechanism: methods, tests and implications for cosmological simulations (2011, unknown): “High values of f,r ∼ 1 for the radio mode of AGN feedback are consistent with relativistic magnetohydrodynamic simulations of BH accretion discs (De Villiers et al. 2005; Hawley & Krolik 2006) for maximally spinning BHs.”
BLACK HOLE SPIN AND THE RADIO LOUD/QUIET DICHOTOMY OF ACTIVE GALACTIC NUCLEI (2009, background): “Any mechanism that enhances the total magnetic flux threading the horizon would lead to a larger BH power output (McKinney 2005b; Hawley & Krolik 2006; Komissarov & McKinney 2007; Reynolds et al. 2006; Garofalo 2009).”
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).”
General relativistic magnetohydrodynamic simulations of magnetically choked accretion flows around black holes (2012, methodology): “…not reach the MCAF state (for GRMHD simulations, e.g., see De Villiers et al. 2003; McKinney & Gammie 2004; McKinney 2005; De Villiers et al. 2005; Hawley & Krolik 2006; McKinney 2006b; Komissarov & McKinney 2007; Komissarov et al. 2007; McKinney & Narayan 2007a,b; Fragile et al. 2007; Beckwith…”
Cool outflows in galaxies and their implications (2020, background): “(2014) in the study by Heckman and Borthakur (2016) extends the range of SFR and ΣSFR over the previous studies and therefore provides more leverage for the fits.”
Spitzer Reveals Hidden Quasar Nuclei in Some Powerful FR II Radio Galaxies (2006, background): “Models that tie jet production to accretion onto a spinning black hole are particularly promising (e.g., Meier 1999; Hawley & Krolik 2006).”
Simulations of magnetized discs around black holes: Effects of black hole spin, disc thickness and magnetic field geometry (2010, methodology): “N10 make use of an older set of simulations from a different non-energy-conserving code (Hawley & Krolik 2006; Beckwith et al. 2008a) to investigate the effect of other field geometries.”
Simulations of ultrarelativistic magnetodynamic jets from gamma‐ray burst engines (2008, background): “…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 Lorentz factors of ∼10 (McKinney 2006b).”
ECHO: a Eulerian conservative high-order scheme for general relativistic magnetohydrodynamics and magnetodynamics (2007, background): “…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 regime (Komissarov 2006b) and the…”
The Influence of Magnetic Field Geometry on the Evolution of Black Hole Accretion Flows: Similar Disks, Drastically Different Jets (2007, methodology): “As described in Hawley & Krolik (2006), energy for the Poynting flux comes from the rotation of the black hole, in a manner closely related to the classical Blandford-Znajek mechanism.”
Grand unification of AGN activity in the ΛCDM cosmology (2009, background): “…outflows of matter in the form of jets may have strong implications for the upper spin limit, since these outflows are ccelerated by magnetic fields that are powered by the extraction of c© 0000 RAS, MNRAS000, 000–000 the rotational energy of the BH (Hawley & Krolik 2006; Benson& Babul 2009).”
Long-term GRMHD simulations of neutron star merger accretion discs: implications for electromagnetic counterparts (2018, methodology): “Concurrent with the onset of accretion, a relativistic outflow is launched around the rotation axis due the magnetic pressure gradient generated by field winding in the vicinity of the black hole (e.g., Hawley & Krolik 2006).”