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Solar modelling has long been split into ''internal'' and ''surface''modelling, because of the lack of tools to connect the very different scales inspace and time, as well as the widely different environments and dominatingphysical effects involved. Significant efforts have recently been put intoresolving this disconnect. We address the outstanding bottlenecks in connectinginternal convection zone and dynamo simulations to the surface of the Sun, andconduct a proof-of-concept high resolution global simulation of the convectionzone of the Sun, using the task-based DISPATCH code framework. We present a new`volleyball' mesh decomposition, which has Cartesian patches tessellated on asphere with no singularities. We use our new entropy based HLLS approximateRiemann solver to model magneto-hydrodynamics in a global simulation, rangingbetween 0.655 -- 0.995 R$_\odot$, with an initial ambient magnetic field set to0.1 Gauss. The simulations develop convective motions with complex, turbulentstructures. Small-scale dynamo action twists the ambient magnetic field andlocally amplifies magnetic field magnitudes by more than two orders ofmagnitude within the initial run-time.

Global MHD simulations of the solar convective zone using a volleyball mesh decomposition. I. Pilot