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Fig. 6

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Metal abundance profiles as a function of depth (expressed by the Lagrangian mass m) for Saturn a) and Jupiter b) for different numbers of layers. The abundance increases with the number of layers, to keep the density profile unchanged when convection becomes inefficient. The extreme cases (105.4 layers for Saturn and 104.5 layers for Jupiter) correspond to the semiconvective profiles portrayed in Fig. 4.

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