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https://stockholmuniversity.zoom.us/j/940229961
In several astrophysical contexts, from planets to binary neutron star mergers, the computational feasibility of MHD simulations is orders of magnitude away from being able to cover the whole range of scales of physical interest. In these cases large eddy simulations are used to partially compensate the lack of numerical resolution, via an implicit or explicit sub-grid-scale model, based on physical/mathematical guess. I present our compressible MHD extension of the so-called gradient sub-grid-scale model, previously used mostly in non-magnetic incompressible cases. I show how it can help capturing magnetic field amplification in the general relativistic scenario at a relatively low computational cost, and future possible applications to planetary dynamos.