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Hydrodynamical simulations are very efficient tools to study the internal structure of stars but the wide range of time and length scales that characterize it makes it difficult to model. To cope this difficulty a common practice when modelling stellar convection is to artificially increase luminosity and thermal diffusivity by several order of magnitude. The reasons for using this artefact is for numerical stability and/or for achieving thermal relaxation We perform fully compressible 2Ddoi:10.5281/zenodo.4566077 fatcat:3gslabastjerlokqgasduuzmnu