Constrained hyperbolic divergence cleaning in smoothed particle magnetohydrodynamics with variable cleaning speeds

Abstract

We present an updated constrained hyperbolic/parabolic divergence cleaning algorithm for smoothed particle magnetohydrodynamics (SPMHD) that remains conservative with wave cleaning speeds which vary in space and time. This is accomplished by evolving the quantity $\psi /c_h$ instead of $\psi$. Doing so allows each particle to carry an individual wave cleaning speed, $c_h$, that can evolve in time without needing an explicit prescription for how it should evolve, preventing circumstances which we demonstrate could lead to runaway energy growth related to variable wave cleaning speeds. This modification requires only a minor adjustment to the cleaning equations and is trivial to adopt in existing codes. Finally, we demonstrate that our constrained hyperbolic/parabolic divergence cleaning algorithm, run for a large number of iterations, can reduce the divergence of the field to an arbitrarily small value, achieving $\nabla \cdot B=0$ to machine precision.

23 pages, 16 figures, accepted for publication in Journal of Computational Physics

References in corpus (28)

• Athena: A New Code for Astrophysical MHD
• Cosmological SPH simulations: The entropy equation
• Smoothed Particle Hydrodynamics and Magnetohydrodynamics
• The impact of magnetic fields on single and binary star formation
• High Order Upwind Schemes for Multidimensional Magnetohydrodynamics
• SPH compressible turbulence
• Accurate, Meshless Methods for Magneto-Hydrodynamics
• An MHD Gadget for cosmological simulations
• Smoothed Particle Magnetohydrodynamics II. Variational principles and variable smoothing length terms
• The effect of magnetic fields on star cluster formation
• Can non-ideal magnetohydrodynamics solve the magnetic braking catastrophe?
• Collapse of a molecular cloud core to stellar densities: stellar core and outflow formation in radiation magnetohydrodynamics simulations
• Smoothed Particle Magnetohydrodynamics III. Multidimensional tests and the div B = 0 constraint
• Inefficient star formation: The combined effects of magnetic fields and radiative feedback
• Smoothed Particle Magnetohydrodynamics I. Algorithms and tests in one dimension
• Constrained Hyperbolic Divergence Cleaning for Smoothed Particle Magnetohydrodynamics
• Collimated jets from the first core
• Smoothed Particle Magnetohydrodynamics IV - Using the Vector Potential
• Magnetic field structure due to the global velocity field in spiral galaxies
• Magnetic fields and the dynamics of spiral galaxies
• Ambipolar diffusion in smoothed particle magnetohydrodynamics
• Magnetic field evolution in simulations with Euler potentials
• A switch to reduce resistivity in smoothed particle magnetohydrodynamics
• Smoothed particle magnetohydrodynamic simulations of protostellar outflows with misaligned magnetic field and rotation axes
• An explicit scheme for ohmic dissipation with smoothed particle magneto-hydrodynamics
• Protostellar outflows with Smoothed Particle Magnetohydrodynamics (SPMHD)
• A Vector Potential implementation for Smoothed Particle Magnetohydrodynamics
• Simulating Astrophysical Magnetic Fields with Smoothed Particle Magnetohydrodynamics

Cited by in corpus (42)

• Dedalus: A Flexible Framework for Numerical Simulations with Spectral Methods
• There is no magnetic braking catastrophe: Low-mass star cluster and protostellar disc formation with non-ideal magnetohydrodynamics
• Ideal GLM-MHD: About the entropy consistent nine-wave magnetic field divergence diminishing ideal magnetohydrodynamics equations
• The collapse of a molecular cloud core to stellar densities using radiation non-ideal magnetohydrodynamics
• A 3D Simulation of a Neutrino-Driven Supernova Explosion Aided By Convection and Magnetic Fields
• Magnetic field evolution in tidal disruption events
• Disc formation and fragmentation using radiative non-ideal magnetohydrodynamics
• The impact of non-ideal magnetohydrodynamics on binary star formation
• High-order Magnetohydrodynamics for Astrophysics with an Adaptive Mesh Refinement Discontinuous Galerkin Scheme
• Non-ideal magnetohydrodynamics vs turbulence I: Which is the dominant process in protostellar disc formation?
• The impact of non-ideal magnetohydrodynamic processes on discs, outflows, counter-rotation and magnetic walls during the early stages of star formation
• Hall effect-driven formation of gravitationally unstable discs in magnetized molecular cloud cores
• The effect of extreme ionisation rates during the initial collapse of a molecular cloud core
• On the origin of magnetic fields in stars
• 3D Simulations of Oxygen Shell Burning with and without Magnetic Fields
• 3D Simulations of Strongly Magnetised Non-Rotating Supernovae: Explosion Dynamics and Remnant Properties
• A geometric multigrid library for quadtree/octree AMR grids coupled to MPI-AMRVAC
• On the fragmentation boundary in magnetised self-gravitating discs
• The dependence of protostar formation on the geometry and strength of the initial magnetic field
• Non-ideal magnetohydrodynamics vs turbulence II: Which is the dominant process in stellar core formation?
• The role of initial magnetic field structure in the launching of protostellar jets
• Do we need non-ideal magnetohydrodynamics to model protostellar discs?
• On the origin of magnetic fields in stars II: The effect of numerical resolution
• Shaken and stirred: the effects of turbulence and rotation on disc and outflow formation during the collapse of magnetised molecular cloud cores
• A Comparison of 2D Magnetohydrodynamic Supernova Simulations with the CoCoNuT-FMT and Aenus-Alcar Codes
• Magnetorotational instability with smoothed particle hydrodynamics
• The properties of clusters, and the orientation of magnetic fields relative to filaments, in magnetohydrodynamic simulations of colliding clouds
• Simulating the magnetorotational instability on a moving mesh with the shearing box approximation
• Divergence cleaning for weakly compressible smoothed particle hydrodynamics
• Smoothed particle magnetohydrodynamics with the geometric density average force expression
• What can the SEDs of first hydrostatic core candidates reveal about their nature?
• Simulating the LOcal Web (SLOW) -- III: Synchrotron emission from the local cosmic web
• Slurm: fluid particle-in-cell code for plasma modeling
• Numerical dependencies of the galactic dynamo in isolated galaxies with SPH
• Monolithic parabolic regularization of the MHD equations and entropy principles
• Axisymmetric smoothed particle magneto-hydrodynamics
• Cosmological Zoom-In Simulation of Odd Radio Circles as Merger-Driven Shocks in Galaxy Groups
• Coupling Smoothed Particle Hydrodynamics with Multi-Agent Deep Reinforcement Learning for Cooperative Control of Point Absorbers
• Magnetic Fields in the Shapley Supercluster Core with POSSUM: Challenging Model Predictions
• Clumpy shocks as the driver of velocity dispersion in molecular clouds: the effects of self-gravity and magnetic fields
• Kinematic dynamos and resolution limits for Smoothed Particle Magnetohydrodynamics
• OpenGadget3 GPU solver tests