The 3D MHD code GOEMHD3 for large-Reynolds-number astrophysical plasmas

Abstract

The numerical simulation of turbulence and flows in almost ideal, large-Reynolds-number astrophysical plasmas motivates the implementation of almost conservative MHD computer codes. They should efficiently calculate, use highly parallelized schemes scaling well with large numbers of CPU cores, allows to obtain a high grid resolution over large simulation domains and which can easily be adapted to new computer architectures as well as to new initial and boundary conditions, allow modular extensions. The new massively parallel simulation code GOEMHD3 enables efficient and fast simulations of almost ideal, large-Reynolds-number astrophysical plasma flows, well resolved and on huge grids covering large domains. Its abilities are validated by major tests of ideal and weakly dissipative plasma phenomena. The high resolution ($2048^3$ grid points) simulation of a large part of the solar corona above an observed active region proved the excellent parallel scalability of the code using more than 30.000 processor cores.

The revised version

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Cited by in corpus (5)

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• Sub-Grid-Scale Description of Turbulent Magnetic Reconnection in Magnetohydrodynamics
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• Electron acceleration by turbulent plasmoid reconnection
• A resolution criterion based on characteristic timescales for MHD simulations of molecular clouds