The Effects of Resolution on Black Hole Accretion Simulations of Jets

Abstract

We perform three general-relativistic magnetohydrodynamic simulations of black hole accretion designed to test how sensitive results are to grid resolution in the jet region. The cases differ only in numerics, modelling the same physical scenario of a radiatively inefficient, geometrically thick, magnetically arrested flow onto a rapidly spinning black hole. Properties inferred with the coarsest grid generally agree with those found with higher resolutions, including total jet power and its decomposition into different forms, velocity structure, nonaxisymmetric structure, and the appearance of resolved millimetre images. Some measures of variability and magnetization are sensitive to resolution. We conclude that most results obtained by limiting resolution near the jet for computational expediency should still be reliable, at least insofar as they would not be improved with a finer grid.

Accepted by MNRAS

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Cited by in corpus (4)

• Jets in Magnetically Arrested Hot Accretion Flows: Geometry, Power and Black Hole Spindown
• Numerical simulation of hot accretion flows (IV): effects of black hole spin and magnetic field strength on the wind and the comparison between wind and jet properties
• Modeling the inner part of the jet in M87: Confronting jet morphology with theory
• Yet Another Modification of Relativistic Magnetohydrodynamic Waves: Electron Thermal Inertia