Non-ideal MHD star formation simulations show stronger magnetic fields, resolved magnetic walls, and density-B offsets only at highest resolution, while ideal MHD results are largely resolution-independent.
Resolving high Reynolds numbers in smoothe d particle hydrodynamics simulations of subsonic turbulence,
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Resolving numerical star formation: A cautionary tale
Non-ideal MHD star formation simulations show stronger magnetic fields, resolved magnetic walls, and density-B offsets only at highest resolution, while ideal MHD results are largely resolution-independent.