Abstract
Abstract We present high-resolution 2D and 3D simulations of magnetized decaying turbulence in relativistic, resistive magnetohydrodynamics. The simulations show dynamic formation of large-scale intermittent long-lived current sheets being disrupted into plasmoid chains by the tearing instability. These current sheets are locations of enhanced magnetic-field dissipation and heating of the plasma. We find magnetic energy spectra ∝k −3/2, together with strongly pronounced dynamic alignment of Elsässer fields and of velocity and magnetic fields, for strong guide-field turbulence, whereas we retrieve spectra ∝k −5/3 for the case of a weak guide-field.
Highlights
Turbulence provides a route for the energy cascade and dissipation in a wide range of astrophysical plasmas
These astrophysical systems are typically relativistic, meaning that the magnetization σ = B2/(4πωρc2) ≥ 1, where B is the magnetic field strength, ρ is the plasma density, and ω is the relativistic enthalpy density, indicating that the magnetic energy density is larger than the plasma energy density
In order to ensure that the resistive length scales are resolved, and results are converged with numerical resolution, we develop a novel adaptive mesh refinement (AMR) strategy
Summary
Turbulence provides a route for the energy cascade and dissipation in a wide range of astrophysical plasmas. This is relevant for astrophysical systems like black hole accretion disk-jet systems (e.g., Ripperda et al 2020, 2021; Mahlmann et al 2020), magnetar magnetospheres (Beloborodov 2020) and pulsar wind nebulae (e.g., Lyubarsky 1992; Begelman 1998) These astrophysical systems are typically relativistic, meaning that the magnetization σ = B2/(4πωρc2) ≥ 1, where B is the magnetic field strength, ρ is the plasma density, and ω is the relativistic enthalpy density, indicating that the magnetic energy density is larger than the plasma energy density. Most turbulence studies have been in the realm of nonrelativistic magnetohydrodynamics (MHD) when the Alfven speed, vA, is much lower than the speed of light, c. Iroshnikov (1963); Kraichnan (1965) showed that the energy cascade from large to small scales is caused by the mutual shear of counter-propagating Alfven waves
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