Alternative Evolution and Internal Structure for Jupiter and Saturn

The internal structure of gas giant planets may be more complex than the commonly assumed core-envelope structure with an adiabatic temperature profile. Different primordial internal structures as well as various physical processes can lead to non-homogenous compositional distributions. A non-homogenous internal structure has a significant impact on the thermal evolution and final structure of the planets. Here we present alternative structure and evolution models for Jupiter and Saturn allowing for both adiabatic and non-adiabatic evolution. In convective regions we calculate the mixing of heavy elements by convection, as these planets evolve. We present the thermal and structural evolution of the planets accounting for various initial composition gradients, and in the case of Saturn, include the formation of a helium-rich region as a result of helium rain. We investigate the stability of the structure against convection, and find that the helium shell in Saturn remains stable and does not mix with the rest of the envelope. In other cases, convection mixes the planetary interior despite the existence of compositional gradients, leading to enrichment of the envelope with metals. We show that non-adiabatic structures (and cooling histories) for both Jupiter and Saturn are feasible, and the interior temperatures in that case are much higher that for standard adiabatic models. Moreover, we show that non-adiabatic evolution can suggest more than one mechanism to explain the current structures, including Saturn's high luminosity. We conclude that the internal structure is directly linked to the formation and evolution history of the planet. These alternative internal structures of Jupiter and Saturn should be considered when interpreting the upcoming Juno and Cassini data.