Numerical viscosity and resistivity in MHD turbulence simulations
arXiv:2311.10350 · doi:10.1093/mnras/staf160
Abstract
Accurate magnetohydrodynamical (MHD) turbulence simulations require understanding numerical dissipation. We quantify numerical viscosity and resistivity in subsonic (M=0.1) and supersonic (M=10) turbulence regimes. The hydrodynamic (Re) and magnetic Reynolds numbers (Rm) on the turbulence driving scale l_turb in a cubic domain of side length L with N^3 resolution elements are well-described by Re=[2(N/N_Re)(l_turb/L)]^p_Re and Rm=[2(N/N_Rm)(l_turb/L)]^p_Rm. We provide two sets of fit values of (N_Re,p_Re,N_Rm,p_Rm): one with p_Re & p_Rm fixed at their theoretical values, and the other one allowing all 4 parameters to vary. The sets for M=0.1 are (1.57_{-0.12}^{+0.10},4/3,1.55_{-0.14}^{+0.45},4/3) and (0.83_{-0.08}^{+0.09},1.20_{-0.02}^{+0.02},4.19_{-4.05}^{+2.95},1.60_{-0.33}^{+0.18}), respectively. For M=10, they are (3.55_{-0.56}^{+0.78},3/2,1.03_{-0.11}^{+0.12},3/2) and (10.46_{-0.85}^{+0.96},1.90_{-0.04}^{+0.04},0.44_{-0.23}^{+0.61},1.32_{-0.09}^{+0.17}). The resulting magnetic Prandtl numbers (Pm=Rm/Re) are consistent with constant values of 1.0_{-0.2}^{+0.3} for M=0.1, and 6.2_{-4.8}^{+5.6} for M=10. These apply when the magnetic energy (E_mag) is <10% of the kinetic energy (E_kin). When E_mag/E_kin~0.1-1, Rm is reduced by a factor~3 (increase in N_Rm by a factor~2) for M=0.1, while Rm for M=10 and Re (for any M) remain largely unaffected. We compare our Re-N relation with 14 other simulations from the literature, employing various numerical methods (with & without Riemann solvers, different reconstruction schemes & orders, and smoothed particle hydrodynamics), and find agreement within a factor of 3. Additionally, we compare these results to target Re and Rm values from simulations with explicit dissipation. These comparisons and our relations help users determine the Re and Rm achievable at a given N, ensuring physical dissipation dominates over numerical dissipation.
25 pages, 13 figures, accepted by MNRAS, comments welcome
References in corpus (59)
- Theory of Star Formation
- Control of star formation by supersonic turbulence
- Astrophysical magnetic fields and nonlinear dynamo theory
- Interstellar Turbulence I: Observations and Processes
- The Interstellar Environment of our Galaxy
- Origin of Galactic and Extragalactic Magnetic Fields
- Comparing the statistics of interstellar turbulence in simulations and observations: Solenoidal versus compressive turbulence forcing
- The Statistics of Supersonic Isothermal Turbulence
- Simulations of small-scale turbulent dynamo
- On the Origin of Cosmic Magnetic Fields
- Turbulent molecular clouds
- Simulations of nonhelical hydromagnetic turbulence
- Simulations of Magnetized Disks Around Black Holes: Effects of Black Hole Spin, Disk Thickness, and Magnetic Field Geometry
- A new Jeans resolution criterion for (M)HD simulations of self-gravitating gas: Application to magnetic field amplification by gravity-driven turbulence
- On the universality of supersonic turbulence
- Inefficient star formation through turbulence, magnetic fields and feedback
- Mach Number Dependence of Turbulent Magnetic Field Amplification: Solenoidal versus Compressive Flows
- 3D Turbulent Reconnection: Theory, Tests and Astrophysical Implications
- Dynamo theories
- The generation of strong magnetic fields during the formation of the first stars
- A robust numerical scheme for highly compressible magnetohydrodynamics: Nonlinear stability, implementation and tests
- SCALING AND INTERMITTENCY IN BURGERS' TURBULENCE
- Fluctuation dynamo and turbulent induction at low magnetic Prandtl numbers
- Magnetic field amplification in turbulent astrophysical plasmas
- The sonic scale revealed by the world's largest supersonic turbulence simulation
- Magnetic fields in the early universe
- Magnetic fields of M dwarfs
- Comparing Numerical Methods for Isothermal Magnetized Supersonic Turbulence
- The onset of a small-scale turbulent dynamo at low magnetic Prandtl numbers
- A comparison between grid and particle methods on the statistics of driven, supersonic, isothermal turbulence
- The Turbulent Dynamo in Highly Compressible Supersonic Plasmas
- Magnetic Field Amplification by Small-Scale Dynamo Action: Dependence on Turbulence Models and Reynolds and Prandtl Numbers
- Generation of Magnetic Fields in the Multi-phase ISM with Supernova-Driven Turbulence
- Critical Magnetic Prandtl Number for Small-Scale Dynamo
- Algorithmic comparisons of decaying, isothermal, supersonic turbulence
- Mach number dependence of the onset of dynamo action
- Energy Flux and Bottleneck Effect in Turbulence
- The turbulent formation of stars
- A Fluid-Dynamical Subgrid Scale Model for Highly Compressible Astrophysical Turbulence
- The Star Formation Rate of Molecular Clouds
- A divergence-free semi-implicit finite volume scheme for ideal, viscous and resistive magnetohydrodynamics
- Turbulence from localized random expansion waves
- Turbulent dynamo in the two-phase interstellar medium
- Magnetic field amplification in accretion discs around the first stars: implications for the primordial IMF
- Fluctuation Dynamo in a Collisionless, Weakly Magnetized Plasma
- Seed magnetic fields in turbulent small-scale dynamos
- Suppression of small scale dynamo action by an imposed magnetic field
- On the measurements of numerical viscosity and resistivity in Eulerian MHD codes
- Turbulent magnetic field amplification from the smallest to the largest magnetic Prandtl numbers
- Fundamental scales in the kinematic phase of the turbulent dynamo
- Efficient highly-subsonic turbulent dynamo and growth of primordial magnetic fields
- As a matter of dynamical range -- scale dependent energy dynamics in MHD turbulence
- Reversed dynamo at small scales and large magnetic Prandtl number
- A finite-volume scheme for modeling compressible magnetohydrodynamic flows at low Mach numbers in stellar interiors
- Magnetic fields in elliptical galaxies: an observational probe of the fluctuation dynamo action
- Dissipative magnetic structures and scales in small-scale dynamos
- Growth or Decay -- I: universality of the turbulent dynamo saturation
- Lagrangian statistics of a shock-driven turbulent dynamo in decaying turbulence
- Critical magnetic Reynolds number of the turbulent dynamo in collisionless plasmas
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