Total and Jet Blandford-Znajek Power in the Presence of an Accretion Disk

By J. McKinney. 2005

213 citations recorded by the source corpus.

Rotating black holes probably power ultrarelativistic jets in gamma-ray bursts, relativistic jets from some active galactic nuclei, and jets from some black hole X-ray binaries. Prior estimates of the power output of a black hole have assumed an infinitely thin disk and a magnetic field based upon a slowly rotating black hole and have not self-consistently determined the geometry or magnitude of the magnetic field for a realistic accretion disk. We provide useful formulae for the total and jet Blandford-Znajek (BZ) power and efficiency as determined self-consistently from general relativistic magnetohydrodynamic numerical models. Of all jet mechanisms, we suggest that only the BZ mechanism is able to produce an ultrarelativistic jet.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d6438591e5dfef1d56501488560c91f939698a04

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Citations in the corpus

ECHO: a Eulerian conservative high-order scheme for general relativistic magnetohydrodynamics and magnetodynamics (2007, background): “…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 effect of different physical processes (Gammie et al. 2004), the problem of jet…”
EFFICIENCY OF MAGNETIC TO KINETIC ENERGY CONVERSION IN A MONOPOLE MAGNETOSPHERE (2009, background): “We point out that the magnetic flux in accreting black hole systems is non-uniformly concentrated in the polar region of the BH (e.g., McKinney 2005, due to ambient pressure of the accretion flow), and therefore the total energy losses of the spinning black hole are actually dominated by the losses…”
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).”
Spacetime approach to force-free magnetospheres (2014, background): “…discussions of different field line types in black hole magnetospheres can be found in (Thorne, Price & MacDonald 1986; Blandford 2002; Hirose et al. 2004; McKinney 2005). intersection is necessary for establishing that conductors determine the rotation frequency of their field lines (see Sec.”
Simulations of ultrarelativistic magnetodynamic jets from gamma‐ray burst engines (2008, methodology): “If the collapsar system forms an accreting BH, then the ultrarelativistic jet may be accompanied by a moderately relativistic disc wind that may provide additional collimation for the jet (McKinney 2005b,2006b).”
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).”
Equation of state in relativistic magnetohydrodynamics: variable versus constant adiabatic index (2007, background): “For all models, the field geometries allowed are similar to that found in McKinney (2005).”
Mass fall-back and accretion in the central engine of gamma-ray bursts (2008, methodology): “We then estimate the relativistic jet luminosity from the mass accretion rate and the BH spin, using a prescription proposed by McKinney (2005).”
Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r‐process nuclei (2010, methodology): “…(Eγ,iso ∼ 2.4 × 10 48 ergs; Kann et al. 2008): even ignoring geometric beaming corrections, only an accreted mass ∼ 10−5M⊙ is necessary to produce a relativistic jet with energy Eγ,iso assuming that the efficiency for converting rest-mass energy to γ−ray power is ∼ 10 per cent (e.g. McKinney 2005).”
Hot Accretion Flows Around Black Holes (2014, background): “Many studies have been published over the years, providing estimates of the jet power as a function of black hole spin (e.g., Hawley & Balbus 2002; De Villers et al. 2005; McKinney 2005, 2006; Hawley & Krolik 2006).”
Magnetically Driven Jets in the Kerr Metric (2005, methodology): “McKinney (2005) expanded on these results and proposed an analytic fitting function for the electromagnetic efficiency of the jet as a function of black hole rotation rate, suggesting that this efficiency scales / 5H , where H is the rotation rate of the black hole.”
Energy, momentum and mass outflows and feedback from thick accretion discs around rotating black holes (2013, methodology): “…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 & McKinney 2010, 2011; Tchekhovskoy, McKinney & Narayan…”
Measuring the spins of accreting black holes (2011, background): “For low spins, the black hole contributes very little power; in fact, for a∗ < 0.4, the accretion disk apparently provides more power than the black hole (McKinney 2005).”
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).”
A Reconnection Switch to Trigger gamma-Ray Burst Jet Dissipation (2010, background): “The magnetization μ could be limited by neutron diffusion (Levinson & Eichler 2003), which still leads to quite high magnetizations of μ ∼ 103–104 (McKinney 2005a) (corresponding to ζ ∼ 103–104).”
Black Hole Spin via Continuum Fitting and the Role of Spin in Powering Transient Jets (2013, background): “GRMHD simulations of accreting black holes have found MHD jets forming spontaneously from generic initial conditions (e.g., Koide et al. 2002; McKinney & Gammie 2004; McKinney 2005; Beckwith et al. 2008; McKinney & Blandford 2009).”
A Unified Model for Tidal Disruption Events (2018, background): “If these jets are produced through the Blandford-Znajek process, this can be because the host SMBHS of those events have very large spins, since the jet power generally depends on black hole spin as Pj ∝ a2−4 (McKinney 2005).”
AFTERGLOW OBSERVATIONS OF FERMI LARGE AREA TELESCOPE GAMMA-RAY BURSTS AND THE EMERGING CLASS OF HYPER-ENERGETIC EVENTS (2010, background): “Both analytic models (e.g., Lee et al. 2000) and numerical simulations (e.g., McKinney 2005) suggest that as much as 5–10% of this rotational energy can be made available to power a collimated outflow, easily within the requirements of hyperenergetic events.”