A Runge-Kutta-Gegenbauer super-time-stepping method for stable, efficient handling of anisotropic non-ideal MHD diffusion.
Journal of Computational Physics , year = 2005, month = sep, volume =
12 Pith papers cite this work, alongside 706 external citations. Polarity classification is still indexing.
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Cellular Sheaf Neural Operators use cell complexes, learned restriction maps, and structure-aware message passing to create discretization-aware neural surrogates that preserve constraints in multiphysics PDEs such as MHD.
libyt provides a bidirectional C-Python interface for in-situ analysis of patch-based AMR simulations using yt and Jupyter with minimal workflow changes.
In idealised driven subsonic MHD boxes, Arepo, Athena and Ramses all show dynamo amplification whose residual differences are explained by numerical diffusion, with no systematic advantage of constrained transport.
A spectral-multigrid Poisson solver for spherical and cylindrical coordinates achieves second-order accuracy on uniform and logarithmic radial grids with vacuum boundary handling via screening mass and scales to 4096 cores.
Dedner's mixed divergence cleaning produces substantial artifacts for strongly localized magnetic fields or sudden timestep changes; constrained transport is more accurate, and some prior early-Universe amplification claims may be affected.
In cool-core cluster simulations, mixing with pre-existing cold gas, not direct radiative cooling, dominates condensation; magnetic fields stretch the pre-condensation history to ~150 Myr and brake infalling clouds through tension.
Presents 24 AREPO+IllustrisTNG zoom-in simulations of clusters above 10^15 solar masses showing converged magnetic fields with volume-averaged plasma beta approximately 100 inside R200 after z~1.2, declining Faraday rotation profiles, and intermittent Braginskii heating approaching cooling rates in
An a posteriori framework implemented in PyMHD estimates numerical dissipation in Alfvénic, dynamo, and MRI-driven MHD turbulence, showing it has distinct spectral and anisotropic properties from physical dissipation.
Jet feedback in centrally concentrated clouds reduces star formation efficiency to 12-16% and yields cluster structures more consistent with observations than models without jets.
Oblique filament collisions lead to gravitational collapse of the compressed cloud when post-collision |gravitational energy| exceeds kinetic plus thermal plus magnetic energies, with lower angles and lower velocities favoring hub-filament formation.
3D MHD simulations of young massive star clusters find proton acceleration to hundreds of TeV near O-star termination shocks, with even faster acceleration to over 100 TeV in under 100 years when a supernova remnant expands inside the core.
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A robust super-time-stepping scheme for Ohmic and ambipolar diffusion
A Runge-Kutta-Gegenbauer super-time-stepping method for stable, efficient handling of anisotropic non-ideal MHD diffusion.
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Cellular Sheaf Neural Operators for Structure-Preserving Surrogate Modeling of Constrained PDEs
Cellular Sheaf Neural Operators use cell complexes, learned restriction maps, and structure-aware message passing to create discretization-aware neural surrogates that preserve constraints in multiphysics PDEs such as MHD.
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libyt: an In Situ Interface Connecting Simulations with yt, Python, and Jupyter Workflows
libyt provides a bidirectional C-Python interface for in-situ analysis of patch-based AMR simulations using yt and Jupyter with minimal workflow changes.
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A comparison of numerical schemes for driven subsonic MHD turbulence
In idealised driven subsonic MHD boxes, Arepo, Athena and Ramses all show dynamo amplification whose residual differences are explained by numerical diffusion, with no systematic advantage of constrained transport.
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A fast spectral-multigrid Poisson solver in non-Cartesian geometries
A spectral-multigrid Poisson solver for spherical and cylindrical coordinates achieves second-order accuracy on uniform and logarithmic radial grids with vacuum boundary handling via screening mass and scales to 4096 cores.
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Systematic Comparison between Constrained Transport and Mixed Divergence Cleaning Methods for Astrophysical Magnetohydrodynamic Simulations
Dedner's mixed divergence cleaning produces substantial artifacts for strongly localized magnetic fields or sudden timestep changes; constrained transport is more accurate, and some prior early-Universe amplification claims may be affected.
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XMAGNET -- Stir before serving: a Lagrangian perspective on mixing-driven condensation in the intracluster medium
In cool-core cluster simulations, mixing with pre-existing cold gas, not direct radiative cooling, dominates condensation; magnetic fields stretch the pre-condensation history to ~150 Myr and brake infalling clouds through tension.
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The PICO-Cluster Project: presenting the galaxy cluster sample and studying magnetic field growth, Faraday rotation and Braginskii heating
Presents 24 AREPO+IllustrisTNG zoom-in simulations of clusters above 10^15 solar masses showing converged magnetic fields with volume-averaged plasma beta approximately 100 inside R200 after z~1.2, declining Faraday rotation profiles, and intermittent Braginskii heating approaching cooling rates in
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Characterization of Numerical Dissipation in Simulations of Magnetohydrodynamic Turbulence
An a posteriori framework implemented in PyMHD estimates numerical dissipation in Alfvénic, dynamo, and MRI-driven MHD turbulence, showing it has distinct spectral and anisotropic properties from physical dissipation.
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Centrally concentrated star formation in young clusters II: Jet feedback
Jet feedback in centrally concentrated clouds reduces star formation efficiency to 12-16% and yields cluster structures more consistent with observations than models without jets.
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Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions
Oblique filament collisions lead to gravitational collapse of the compressed cloud when post-collision |gravitational energy| exceeds kinetic plus thermal plus magnetic energies, with lower angles and lower velocities favoring hub-filament formation.
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Direct simulations of very high energy cosmic ray acceleration in 3D MHD model of a compact star cluster
3D MHD simulations of young massive star clusters find proton acceleration to hundreds of TeV near O-star termination shocks, with even faster acceleration to over 100 TeV in under 100 years when a supernova remnant expands inside the core.