Evolution of Jupiter with a radiative zone

Traditionally, interior models of gas giants assume convection as the dominant heat transport mechanism in the hydrogen-dominated 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 might exist at the kilobar level. Deep stable layers have been proposed to reconcile key observations of Jupiter, including its atmospheric water and CO abundances and the depth of its zonal winds. In this study, we present the most comprehensive opacity tables to date, enabling us to determine the alkali depletion required to develop a radiative zone in Jupiter, both at present and throughout its evolution. Using evolutionary models, we explore how deep radiative zones influence key observational constraints, such as Jupiter's effective temperature and its current atmopsheric helium abundance.