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The internal structure of gas giant planets may be more complex than thecommonly assumed core-envelope structure with an adiabatic temperature profile.Different primordial internal structures as well as various physical processescan lead to non-homogenous compositional distributions. A non-homogenousinternal structure has a significant impact on the thermal evolution and finalstructure of the planets. In this paper, we present alternative structure andevolution models for Jupiter and Saturn allowing for non-adiabatic primordialstructures and the mixing of heavy elements by convection as these planetsevolve. We present the evolution of the planets accounting for various initialcomposition gradients, and in the case of Saturn, include the formation of ahelium-rich region as a result of helium rain. We investigate the stability ofregions with composition gradients against convection, and find that the heliumshell in Saturn remains stable and does not mix with the rest of the envelope.In other cases, convection mixes the planetary interior despite the existenceof compositional gradients, leading to the enrichment of the envelope withheavy elements. We show that non-adiabatic structures (and cooling histories)for both Jupiter and Saturn are feasible. The interior temperatures in thatcase are much higher that for standard adiabatic models. We conclude that theinternal structure is directly linked to the formation and evolution history ofthe planet. These alternative internal structures of Jupiter and Saturn shouldbe considered when interpreting the upcoming Juno and Cassini data.

The Evolution and Internal Structure of Jupiter and Saturn with Compositional Gradients