A new vision on giant planet interiors: the impact of double diffusive convection

TL;DR

This paper introduces new models of giant planet interiors incorporating double-diffusive convection due to compositional gradients, leading to revised estimates of heavy element distribution, core size, and thermal profiles.

Contribution

It develops an analytical framework for layered double-diffusive convection and applies it to Jupiter and Saturn, challenging traditional adiabatic models.

Findings

Models show increased metal enrichment by 30-60%.

Predict smaller or no cores in Jupiter and Saturn.

Models align with observational constraints.

Abstract

While conventional interior models for Jupiter and Saturn are based on the simplistic assumption of a solid core surrounded by a homogeneous gaseous envelope, we derive new models with an inhomogeneous distribution of heavy elements, i.e. a gradient of composition, within these planets. Such a compositional stratification hampers large scale convection which turns into double-diffusive convection, yielding an inner thermal profile which departs from the traditionally assumed adiabatic interior, affecting these planet heat content and cooling history. To address this problem, we develop an analytical approach of layered double-diffusive convection and apply this formalism to Solar System gaseous giant planet interiors. These models satisfy all observational constraints and yield a metal enrichment for our gaseous giants up to 30 to 60% larger than previously thought. The models also constrain the size of the convective layers within the planets. As the heavy elements tend to be redistributed within the gaseous envelope, the models predict smaller than usual central cores inside Saturn and Jupiter, with possibly no core for this latter. These models open a new window and raise new challenges on our understanding of the internal structure of giant (solar and extrasolar) planets, in particular on the determination of their heavy material content, a key diagnostic for planet formation theories.