Dix Planetary Science Seminar

For about a decade, Jupiter's interior structure has been modeled using H/He-EOS data derived from first principles. A common finding in such models, even before the advent of Juno, is a rather low atmospheric metallicity and an enhanced deep envelope metallicity or dilute core. Meanwhile, three of such H/He-EOS are in use (MH13, REOS, and CMS19). The latter and most recent one, however, predicts the opposite behavior of an enhanced atmospheric metallicity and metal-poor deep interior. While the first group of models would therefore like to see a super-adiabatic region far out in the planet at ~0.95 RJ, the latter group of models suggest a strongly super-adiabatic region deep and below the H/He immiscibility region. The need for super-adiabatic regions may
indicate stable stratification here or there. In this work, we rely on the idea of stable stratification and discuss deep interior differential rotation as a possibility to rescue Jupiter.