Three-Dimensional Simulations of Magnetized Thin Accretion Disks around Black Holes: Stress in the Plunging Region

By Rebecca Shafee, J. McKinney, Ramesh Narayan, A. Tchekhovskoy, Charles F. Gammie, J. E. McClintock. 2008

147 citations recorded by the source corpus.

We describe three-dimensional general relativistic magnetohydrodynamic simulations of a geometrically thin accretion disk around a nonspinning black hole. The disk has a thickness h/r ∼ 0.05–0.1 over the radial range (2–20) GM/c2. In steady state, the specific angular momentum profile of the inflowing magnetized gas deviates by less than 2% from that of the standard thin disk model of Novikov and Thorne. Also, the magnetic torque at the radius of the innermost stable circular orbit (ISCO) is only ~2% of the inward flux of angular momentum at this radius. Both results indicate that magnetic coupling across the ISCO is relatively unimportant for geometrically thin disks.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8b0d8bf12ee7a93b688c5674d49ebe2cc96c3f06

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Citations in the corpus

The spin of the black hole microquasar XTE J1550−564 via the continuum-fitting and Fe-line methods (2010, methodology): “Theoretical support for identifying Rin with RISCO is provided by magnetohydrodynamic simulations of thin accretion discs (Reynolds & Fabian 2008; Shafee et al. 2008; Penna et al. 2010; Kulkarni et al. 2011; but see Noble, Krolik & Hawley 2009, 2010).”
Measuring the spins of accreting black holes (2011, methodology): “Their argument, which was based on a hydrodynamical description of the disk, was confirmed by detailed calculations carried out by Shafee et al (2008b).”
Observational evidence for a correlation between jet power and black hole spin (2011, background): “As most clearly demonstrated for the prototype microquasar GRS 1915+105 (Fender & Belloni 2004), this stage appears to correspond to the inward-moving inner edge of the accretion disc reaching the ISCO, which results in a shock or some other violent event that launches the large-scale relativistic j”
Black Hole Spin via Continuum Fitting and the Role of Spin in Powering Transient Jets (2013, methodology): “To answer this question, geometrically thin accretion disks around black holes have been simulated by a number of authors (Shafee et al. 2008a; Noble & Krolik 2009; Penna et al. 2010) using state-of-the-art GRMHD codes.”
Energy, momentum and mass outflows and feedback from thick accretion discs around rotating black holes (2013, background): “All GRMHD simulations of thin discs performed so far (e.g. Shafee et al. 2008; Penna et al. 2010; Noble et al. 2011; Zhu et al. 2012) are based on an artificial cooling function which drives discs to an arbitrarily chosen entropy corresponding to a required given disc thickness.”
THE CONSTANT INNER-DISK RADIUS OF LMC X-3: A BASIS FOR MEASURING BLACK HOLE SPIN (2010, background): “…provide support for identifying the inner-disk radius Rin with the radius of the innermost stable circular orbit RISCO (Reynolds & Fabian 2008; Shafee et al. 2008; Penna et al. 2010; but see Noble et al. 2009), a proposition that has a long history of theoretical and observational support…”
Semi-implicit scheme for treating radiation under M1 closure in general relativistic conservative fluid dynamics codes (2012, background): “…of thin discs have been computed so far, and all are based on an ad hoc (although physically motivated) local cooling function which artificially removes excess heat to keep the disc geometrically thin (Shafee et al. 2008; Penna et al. 2010; Noble et al. 2011; see also Reynolds & Fabian 2008).”
Simulations of magnetized discs around black holes: Effects of black hole spin, disc thickness and magnetic field geometry (2010, background): “In either case, these hydrodynamic models clearly show that, as |h/r| → 0, i.e. as cs/vK → 0, the solution always tends towards the NT model (Shafee et al. 2008b).”
THE EXTREME SPIN OF THE BLACK HOLE IN CYGNUS X-1 (2011, methodology): “RISCO is a monotonic function of the dimensionless spin parameter a∗, decreasing from 6 GM/c2 to 1 GM/c2 as spin increases from a∗ = 0 to a∗ = 1 (Bardeen et al. 1972)9.”
Three-dimensional simulations of supercritical black hole accretion discs - luminosities, photon trapping and variability (2015, background): “The latter is treated 1 A number of groups (e.g., Shafee et al. 2008a; Schnittman et al. 2013; Avara et al. 2015) have performed simulations of thin disks in pure hydrodynamical setup implementing arbitrary cooling function. in the “blackbody” Comptonization approximation as described in Sądowski…”
Stability of relativistic jets from rotating, accreting black holes via fully three-dimensional magnetohydrodynamic simulations (2008, background): “At the inner torus edge, cells have aspect ratio 1:5:10 and the fastest-growing magnetorota ional mode is resolved with 6 cells, as sufficient (Shafee et al. 2008).”
A Reconnection Switch to Trigger gamma-Ray Burst Jet Dissipation (2010, background): “…applicable to a neutrino-dominated accretion disc that takes on a quite thin geometry near a rotating BH where the jet is launched [see e.g. Kohri et al. (2005) and Chen & Beloborodov (2007), and for simulations of such magnetized thin discs, see e.g. Shafee et al. (2008) and Penna et al. (2010)].”
Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, background): “Simulations have only so-far included an ad hoc cooling function that leads to |H/R| ∼ 0.05–0.1 (Shafee et al. 2008; Reynolds & Fabian 2008; Reynolds & Miller 2009; Noble et al. 2009; Penna et al. 2010; Noble et al. 2010; Sorathia et al. 2010; Noble et al. 2011b; Beckwith et al. 2011).”
STELLAR-MASS BLACK HOLE SPIN CONSTRAINTS FROM DISK REFLECTION AND CONTINUUM MODELING (2009, methodology): “Based on the results summarized in Reynolds & Fabian (2008) and related work by Shafee et al. (2008), a conservative estimate of the uncertainty in the ISCO based on this and other simulations is 0.5 rg for low spin parameters (an uncertainty of about 20% for very low spin; see Miniutti & Fabian…”
GRMHD simulations of magnetized advection‐dominated accretion on a non‐spinning black hole: role of outflows (2012, unknown): “Similarly, Hawley & Balbus (2002) observed outflows for all radii outside the innermost stable circular orbit (ISCO), though they used a definition of inflow and outflow based on cyclindrical coordinates (all other authors use spherical coordinates) which makes their outflow estimates somewhat ambig”
ASSESSING QUANTITATIVE RESULTS IN ACCRETION SIMULATIONS: FROM LOCAL TO GLOBAL (2011, background): “…from pseudo-Newtonian dynamics (Hawley & Krolik 2001; Machida & Matsumoto 2003) to full three-dimensional general relativistic physics (De Villiers & Hawley 2003; Gammie et al. 2003; Anninos et al. 2005), most recently including toy-model thermodynamics (Noble et al. 2009; Shafee et al. 2008).”
DIRECT CALCULATION OF THE RADIATIVE EFFICIENCY OF AN ACCRETION DISK AROUND A BLACK HOLE (2008, methodology): “2Concurrent with our effort, Shafee et al. (2008) have also developed a 3D version of the HARM code.”
Numerical simulations of super-critical black hole accretion flows in general relativity (2013, methodology): “…radiation have been described in the literature (e.g., De Villiers et al. 2003; Gammie et al. 2003; Anninos et al. 2005; Del Zanna et al. 2007; Shafee et al. 2008; Penna et al. 2010; Tchekhovskoy et al. 2010a,b; Narayan et al. 2010; Noble et al. 2011; Tchekhovskoy et al. 2011; Tchekhovskoy &…”