Evidence for a Dichotomy in the Interior Structures of Jupiter and Saturn from Helium Phase Separation

Abstract

Abstract We examine the comparative thermal evolution of Jupiter and Saturn, applying recent theoretical results for helium’s immiscibility in fluid metallic hydrogen. The redistribution of helium in their interiors proceeds very differently for the two planets. We confirm that, based on Jupiter’s atmospheric helium depletion as observed in situ by the Galileo entry probe, Jupiter’s interior helium has differentiated modestly, and we present models reconciling Jupiter’s helium depletion, radius, and heat flow at the solar age. Jupiter’s recently revised Bond albedo implies a higher intrinsic flux for the planet, accommodating more luminosity from helium differentiation, such that mildly superadiabatic interiors can satisfy all constraints. The same phase diagram applied to the less massive Saturn predicts dramatic helium differentiation, to the degree that Saturn inevitably forms a helium-rich shell or core, an outcome previously proposed by Stevenson & Salpeter and others. The luminosity from Saturn’s helium differentiation is sufficient to extend its cooling time to the solar age, even for adiabatic interiors. This model predicts Saturn’s atmospheric helium to be depleted to Y = 0.07 ± 0.01, corresponding to a He/H2 mixing ratio 0.036 ± 0.006. We also show that neon differentiation may have contributed to both planets’ luminosity in the past. These results demonstrate that Jupiter and Saturn’s thermal evolution can be explained self-consistently with a single physical model, and emphasize that nontrivial helium distributions should be considered in future models for Saturn’s internal structure and dynamo.