HARM: A Numerical Scheme for General Relativistic Magnetohydrodynamics

By Charles F. Gammie, J. McKinney, G. T'oth. 2003

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We describe a conservative, shock-capturing scheme for evolving the equations of general relativistic magnetohydrodynamics. The fluxes are calculated using the Harten, Lax, & van Leer scheme. A variant of constrained transport, proposed earlier by Tóth, is used to maintain a divergence-free magnetic field. Only the covariant form of the metric in a coordinate basis is required to specify the geometry. We describe code performance on a full suite of test problems in both special and general relativity. On smooth flows we show that it converges at second order. We conclude by showing some results from the evolution of a magnetized torus near a rotating black hole.

Subfields: Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/d25b953be0b4a9413189d9695117c120cf72ebe5

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In Computational Mechanics

Citations in the corpus

Long-term GRMHD simulations of neutron star merger accretion discs: implications for electromagnetic counterparts (2018, methodology): “To evolve the torus in GRMHD, we use HARMPI2, an enhanced version of the serial open-source code HARM (Gammie et al. 2003; Noble et al. 2006).”
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).”
Magnetic acceleration of relativistic AGN jets (2007, methodology): “This distinguishes it from most other schemes for relativistic MHD, including those that are based on HLL, KT and similar ﬂux prescriptions (e.g. Gammie et al. 2003; Duez et al. 2005; Koide et al. 1999; Anninos et al. 2006; Shibata & Sekuguchi 2005; Anderson et al. 2006a; Del Zanna et al. 2003;…”
Stability of relativistic jets from rotating, accreting black holes via fully three-dimensional magnetohydrodynamic simulations (2008, methodology): “We us the conservative unsplit 3D GRMHD code HARM (Gammie et al. 2003), Kerr-Schild coordinates, 4th-order interpolationa d 4thorder Runge-Kutta (McKinney 2006a), a robust inversion scheme (Mignone & McKinney 2007), a staggered field scheme (McKinney et al., in prep.)”
THE SUBMILLIMETER BUMP IN Sgr A* FROM RELATIVISTIC MHD SIMULATIONS (2010, methodology): “For comparison, we have also run a set of axisymmetric simulations using the publicly available HARM code (Gammie et al. 2003; Noble et al. 2006) at black hole spins a/M = 0.00, 0.50, 0.75, 0.90, 0.92, and 0.94 (G = c = 1 is used throughout this paper).”
General relativistic magnetohydrodynamic simulations of magnetically choked accretion flows around black holes (2012, methodology): “The initial mass for the thick disk models is an isentropic hydro-equilibrium torus (Fishbone & Moncrief 1976; Gammie et al. 2003) with inner edge at rin = 10rg and pressure maximum at rmax = 100rg.”
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).”
Total and Jet Blandford-Znajek Power in the Presence of an Accretion Disk (2005, methodology): “HARM (Gammie et al. 2003) was used to evolve a series of otherwise identical GRMHD models with spina/M from 0.999 to 0.999 andH/R of 0.1, 0.2, 0.5, and 0.9 to determine the total BZ power (Ptot), jet BZ power (Pjet), and field strength (Br).”
Prograde and retrograde black holes: whose jet is more powerful? (2012, methodology): “We carried out time-dependent 3D general relativistic non-radiative MHD simulations using a high-order version of Godunov-type shock-capturing code HARM (Gammie et al. 2003; McKinney & Gammie 2004; Tchekhovskoy et al. 2007, 2009; McKinney & Blandford 2009) in modified spherical polar coordinates.”
BLACK HOLE SPIN AND THE RADIO LOUD/QUIET DICHOTOMY OF ACTIVE GALACTIC NUCLEI (2009, methodology): “We performed the simulations using the GR MHD code HARM (Gammie et al. 2003; McKinney & Gammie 2004; McKinney 2006a, 2006b; Noble et al. 2006) using Kerr– Schild coordinates in the Kerr metric; the code includes a number of recent improvements (Mignone & McKinney 2007; Tchekhovskoy et al. 2007,…”
Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, methodology): “No explicit viscosity or resistivity are included, but we use the energy conserving HARM scheme so all dissipation is captured (Gammie et al. 2003; McKinney 2006).”
DIRECT CALCULATION OF THE RADIATIVE EFFICIENCY OF AN ACCRETION DISK AROUND A BLACK HOLE (2008, methodology): “Explicitly, these are U (P) = √−g [ ρut, T tt + ρu t, T tj , B k ]T (8) 3We follow Gammie et al. (2003) in our definition of the electromagnetic field tensor and magnetic field variables.”
GENERAL RELATIVISTIC HYDRODYNAMIC SIMULATION OF ACCRETION FLOW FROM A STELLAR TIDAL DISRUPTION (2015, methodology): “We use the fully conservative general relativistic magnetohydrodynamics code HARM3D for our global simulation (Gammie et al. 2003; Noble et al. 2009); there is, however, no magnetic field in the simulation reported here.”
Global General Relativistic Magnetohydrodynamic Simulation of a Tilted Black Hole Accretion Disk (2007, background): “Many simulations of black hole accretion flows have been carried out over the past three decades, both in the hydrodynamic (e.g., Wilson 1972; Hawley et al. 1984; Hawley 1991) and magnetohydrodynamic (MHD; e.g., Koide et al. 1999; Gammie et al. 2003; DeVilliers &Hawley 2003b) regimes.”