Resolution analysis of magnetically arrested disc simulations

Resolution analysis of magnetically arrested disc simulations

ABSTRACT Polarization measurements by the Event Horizon Telescope from M87* and Sgr A* suggest that there is a dynamically strong, ordered magnetic field, typical of what is expected of a magnetically arrested accretion disc (MAD). In such discs, the strong poloidal magnetic field can suppress the a...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society Vol. 533; no. 1; pp. 254 - 267
Main Authors: Salas, L D S, Musoke, G, Chatterjee, K, Markoff, S B, Porth, O, Liska, M T P, Ripperda, B
Format: Journal Article
Language:English
Published: London Oxford University Press 01-09-2024
Subjects:
Accretion disks
Angular momentum
Emission
Energy dissipation
Event horizon
Magnetic fields
Magnetic flux
Magnetic properties
Magnetohydrodynamic turbulence
Sheaths
Simulation
Tubes
black hole physics
(magnetohydrodynamics) MHD
accretion, accretion discs
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Summary:ABSTRACT Polarization measurements by the Event Horizon Telescope from M87* and Sgr A* suggest that there is a dynamically strong, ordered magnetic field, typical of what is expected of a magnetically arrested accretion disc (MAD). In such discs, the strong poloidal magnetic field can suppress the accretion flow and cause episodic flux eruptions. Recent work shows that general relativistic magnetohydrodynamic (GRMHD) MAD simulations feature dynamics of turbulence and mixing instabilities that are becoming resolved at higher resolutions. We perform a convergence study of MAD states exceeding the status quo by an order of magnitude in resolution. We use existing 3D simulations performed with the H-AMR code, up to a resolution of 5376 × 2304 × 2304 in a logarithmic spherical-polar grid. We find consistent time-averaged disc properties across all resolutions. However, higher resolutions reveal signs of inward angular momentum transport attributed to turbulent convection, particularly evident when mixing instabilities occur at the surfaces of flux tubes during flux eruptions. Additionally, we see wave-like features in the jet sheath, which become more prominent at higher resolutions, that may induce mixing between the jet and disc. At higher resolutions, we observe the sheath to be thinner, resulting in increased temperature, reduced magnetization, and greater variability. Those differences could affect the dissipation of energy, which would eventually result in distinct observable radiative emission from high-resolution simulations. With higher resolutions, we can delve into crucial questions about horizon-scale physics and its impact on the dynamics and emission properties of larger-scale jets.
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stae1834