Conditions for radiative zones in the molecular hydrogen envelope of Jupiter and Saturn: The role of alkali metals

TL;DR

This study investigates the conditions under which stable radiative zones can form in the molecular hydrogen envelopes of Jupiter and Saturn, emphasizing the role of alkali metals and updated opacity data.

Contribution

It provides new radiative opacity tables including key molecules and atomic species, and identifies specific alkali metal abundance thresholds for radiative zone formation in gas giants.

Findings

Radiative zones depend on low K and Na abundances in atmospheres.

Jupiter's radiative zone requires K and Na less than ~10^-3 times solar.

Saturn's radiative zone requires K and Na less than ~10^-4 times solar.

Abstract

Interior models of gas giants in the Solar System traditionally assume a fully convective molecular hydrogen envelope. However, recent observations from the Juno mission suggest a possible depletion of alkali metals in Jupiter's molecular hydrogen envelope, indicating that a stable radiative layer could exist at the kilobar level. Recent studies propose that deep stable layers help reconcile various Jupiter observations, including its atmospheric water and CO abundances and the depth of its zonal winds. However, opacity tables used to infer stable layers are often outdated and incomplete, leaving the precise molecular hydrogen envelope composition required for a deep radiative zone uncertain. In this paper, we determine atmospheric compositions that can lead to the formation of a radiative zone at the kilobar level in Jupiter and Saturn today. We computed radiative opacity tables covering pressures up to $10^5$ bar, including the most abundant molecules present in the gas giants of the Solar System, as well as contributions from free electrons, metal hydrides, oxides, and atomic species, using the most up-to-date line lists published in the literature. These tables were used to calculate Rosseland-mean opacities for the molecular hydrogen envelopes of Jupiter and Saturn, which were then compared to the critical mean opacity required to maintain convection. We find that the presence of a radiative zone is controlled by the existence of K, Na, and NaH in the atmosphere of Jupiter and Saturn. For Jupiter, the elemental abundance of K and Na must be less than $\sim 10^{-3}$ times solar to form a radiative zone. In contrast, for Saturn, the required abundance for K and Na is below $\sim 10^{-4}$ times solar.