2022MNRAS.517.2714M

Turbulent transport driven by secular shear instabilities can lead to enhanced vertical mixing in hot Jupiter atmospheres, impacting their cloudiness, chemistry, and overall vertical structure. We discuss the turbulent regime expected and evaluate theoretical uncertainties on the strength of the vertical mixing (i.e. K_zz values). We focus our work on three well-studied hot Jupiters with a hierarchy of atmospheric temperatures: HD189733b (T_eq ≃ 1200 K), HD209458b (T_eq ≃ 1450 K), and Kepler7b (T_eq ≃ 1630 K). K_zz uncertainties are large. They are dominated by (i) the poorly understood magnitude of turbulent transport and (ii) the semitransparent nature of shear turbulence near the planetary photosphere. Using a specific Moore-Spiegel instability threshold, we infer that the cooler HD189733b is not subject to enhanced mixing from semitransparent shear turbulence, while the daysides of the hotter Kepler7b and (marginally so) HD209458b are. Enhanced vertical mixing is generally expected to manifest on hot enough exoplanets, with T_eq > 1500-1600 K. On a given planet, day and night K_zz profiles can differ by an order of magnitude or more. Vertical mixing is slightly favoured in equatorial regions, where the atmospheric zonal shear is strongest. In all three planetary cases studied, momentum feedback on the atmospheric mean flow is minor to negligible.