Stable stratification of the helium rain layer yields vastly different interiors and magnetic fields for Jupiter and Saturn

TL;DR

This paper explores how helium rain layers in Jupiter and Saturn influence their internal structures and magnetic fields, revealing significant differences in the extent and effects of helium phase separation.

Contribution

It provides new insights into the impact of helium rain layers on planetary interiors and magnetic fields, highlighting differences between Jupiter and Saturn based on phase separation dynamics.

Findings

Jupiter's helium rain layer is limited to a few tens of kilometers.

Saturn's helium rain occurs much deeper, affecting its heat flux.

Helium condensation significantly influences magnetic field characteristics.

Abstract

At sufficiently high pressures (~Mbar) and low temperatures (~1e3-1eK), hydrogen and helium become partly immiscible. Interpretations of Jupiter and Saturn's magnetic fields favor the existence of a statically stable layer near the Mbar pressure level. From experimental and computational data for the hydrogen-helium phase diagram we find that moist convection and diffusive convection are inhibited, implying a stable helium rain layer in both Jupiter and Saturn. However, we find a significant difference in terms of structure and evolution: In Jupiter, helium settling leads to a stable yet super-adiabatic temperature gradient that is limited by conductive heat transport. The phase separation region should extend only a few tens of kilometers instead of thousands in current-day models, and be characterized by a sharp increase of the temperature of about 500K for standard phase separation diagrams. In Saturn, helium rains occurs much deeper, implying a larger helium flux relative to planetary mass. We find that the significant latent heat associated with helium condensation implies that a large fraction, perhaps close to 100%, of the planet's intrinsic heat flux may be locally transported by the sinking helium droplets. This implies that Saturn may possess a much more extended helium-rain region. This also accounts, at least qualitatively, for the differences in strength and characteristics of the magnetic fields of the two planets. Dedicated models of magnetic field generation in both planets may offer observational constraints to further refine these findings.