Jupiter's Temperate Belt/Zone Contrasts Revealed at Depth by Juno Microwave Observations

Juno microwave radiometer (MWR) observations of Jupiter's midlatitudes reveal a strong correlation between brightness temperature contrasts and zonal winds, confirming that the banded structure extends throughout the troposphere. However, the microwave brightness gradient is observed to change sign with depth: the belts are microwave‐bright in the p10 bar range. The transition level (which we call the “jovicline”) is evident in the MWR 11.5 cm channel, which samples the 5–14 bar range when using the limb‐darkening at all emission angles. The transition is located between 4 and 10 bars, and implies that belts change with depth from being NH3‐depleted to NH3‐enriched, or from physically warm to physically cool, or more likely a combination of both. The change in character occurs near the statically stable layer associated with water condensation. The implications of the transition are discussed in terms of ammonia redistribution via meridional circulation cells with opposing flows above and below the water condensation layer, and in terms of the “mushball” precipitation model, which predicts steeper vertical ammonia gradients in the belts versus the zones. We show via the moist thermal wind equation that both the temperature and ammonia interpretations can lead to vertical shear on the zonal winds, but the shear is ∼50× weaker if only NH3 gradients are considered. Conversely, if MWR observations are associated with kinetic temperature gradients then it would produce zonal winds that increase in strength down to the “jovicline”, consistent with Galileo probe measurements; then decay slowly at higher pressures. Plain Language Summary One of the core scientific questions for NASA's Juno mission was to explore how Jupiter's famous banded structure might change below the top‐most clouds. Did the alternating bands of temperatures, winds, composition, and clouds simply represent the top of a much deeper circulation pattern? Juno's microwave radiometer is capable of peering through the clouds to reveal structures extending to great depths, and has revealed a surprise: belts and zones do persist to pressures of 100 bars or more, but they flip their character at a level which we call the “jovicline,” coinciding with the depths at which water clouds are expected to form and generate a stable layer. This transition from microwave‐bright belts (ammonia depleted and/or physically warm) in the upper layers, to microwave‐dark belts (