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

Abstract

We describe three-dimensional general relativistic magnetohydrodynamic simulations of a geometrically thin accretion disk around a non-spinning black hole. The disk has a thickness $h/r\sim 0.05-0.1$ over the radial range $(2-20)GM/c^2$. 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 & Thorne (1973). Also, the magnetic torque at the radius of the innermost stable circular orbit (ISCO) is only $\sim 2$ 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.

4 pages, 4 figures, ApJL accepted

References in corpus (9)

• The Influence of Magnetic Field Geometry on the Evolution of Black Hole Accretion Flows: Similar Disks, Drastically Different Jets
• Testing Accretion Disk Theory in Black Hole X-ray Binaries
• Equation of State in Relativistic Magnetohydrodynamics: variable versus constant adiabatic index
• Broad iron K-alpha emission lines as a diagnostic of black hole spin
• WHAM: A WENO-based general relativistic numerical scheme I: Hydrodynamics
• Disk-Jet Coupling in Black Hole Accretion Systems I: General Relativistic Magnetohydrodynamical Models
• General Relativistic Force-Free Electrodynamics: A New Code and Applications to Black Hole Magnetospheres
• Disk-Jet Coupling in Black Hole Accretion Systems II: Force-Free Electrodynamical Models
• Viscous Torque and Dissipation in the Inner Region of a Thin Accretion Disk: Implications for Measuring Black Hole Spin

Cited by in corpus (13)

• Stability of Relativistic Jets from Rotating, Accreting Black Holes via Fully Three-Dimensional Magnetohydrodynamic Simulations
• The Submillimeter Bump in Sgr A* from Relativistic MHD Simulations
• Quasar Accretion Disks Are Strongly Inhomogeneous
• Semi-implicit scheme for treating radiation under M1 closure in general relativistic conservative fluid dynamics codes
• A Determination of the Spin of the Black Hole Primary in LMC X-1
• The Origin of Black Hole Spin in Galactic Low-Mass X-ray Binaries
• Development of General Relativistic Magnetohydrodynamic Code and its Application to Central Engine of Long Gamma-Ray Bursts
• GRMHD prediction of coronal variability in accreting black holes
• Relativistic thick accretion disks: morphology and evolutionary parameters
• Black hole spin inferred from 3:2 epicyclic resonance model of high-frequency quasi-periodic oscillations
• The Race Between Stars and Quasars in Reionizing Cosmic Hydrogen
• Black Hole Spin Evolution Affected by Magnetic Field Decay
• The thickness of a weakly-magnetized accretion flow inside the last stable orbit of a Kerr black hole