Superadiabaticity in Jupiter and giant planet interiors

TL;DR

This paper challenges traditional models of Jupiter's interior by demonstrating that non-adiabatic, superadiabatic stratification with shallower density gradients than the outer adiabat is possible and stable, affecting our understanding of giant planet interiors.

Contribution

It clarifies the correct application of the Schwarzschild-Ledoux criterion and shows that superadiabatic stratification with lower density gradients than the outer adiabat can be stable in giant planets.

Findings

Superadiabatic stratification can have lower density gradients than the outer adiabat.

Such structures are stable against non-adiabatic perturbations.

This challenges traditional models of Jupiter's interior and impacts planetary evolution theories.

Abstract

Interior models of giant planets traditionally assume that at a given radius (i.e. pressure) the density should be larger than or equal to the one corresponding to a homogeneous, adiabatic stratification throughout the planet (referred to as the 'outer adiabat'). The observations of Jupiter's gravity field by Juno combined with the constraints on its atmospheric composition appear to be incompatible with such a profile. In this letter, we show that the above assumption stems from an incorrect understanding of the Schwarzschild-Ledoux criterion, which is only valid on a local scale. In order to fulfil the buoyancy stability condition, the density gradient with pressure in a non-adiabatic region must indeed rise more steeply than the {\it local} adiabatic density gradient. However, the density gradient can be smaller than the one corresponding to the outer adiabat at the same pressure because of the higher temperature in an inhomogeneously stratified medium. Deep enough, the density can therefore be lower than the one corresponding to the outer adiabat. We show that this is permitted only if the slope of the local adiabat becomes shallower than the slope of the outer adiabat at the same pressure, as found in recent Jupiter models due to the increase of both specific entropy and adiabatic index with depth. We examine the dynamical stability of this structure and show that it is stable against non-adiabatic perturbations. The possibility of such unconventional density profile in Jupiter complicates further our understanding of the internal structure and evolution of (extrasolar) giant planets.