Jupiter’s oxygen content is inextricably tied to its formation history and the evolution of the early Solar System. Recent one-dimensional thermochemical modelling of CO showed that the planet’s bulk water content could be subsolar, in stark contrast to the water enrichment determined near the equator using the Juno spacecraft. Here we use a hydrodynamic model to study Jupiter’s atmospheric dynamics at and below the water cloud level with simplified thermochemistry to show the effect of hydrodynamics on the abundance of disequilibrium species CO, PH₃ and GeH₄ in the troposphere. If PH₃ and GeH₄ provide only an upper limit for the oxygen abundance (≤5 times solar), our results suggest an oxygen enrichment range of 2.5–5 times solar using updated CO thermochemistry. Using the conventional CO chemical timescale, we further reveal a correlation between moist convection and the CO abundance at the water cloud level. If such a correlation is found observationally, it would favour the formation of Jupiter near the snow line, which harbours a supersolar oxygen abundance.

木星的氧含量与其形成历史和早期太阳系的演化密不可分。最近对 CO 的一维热化学模型表明，这颗行星的体水含量可能是亚太阳的，这与使用朱诺号宇宙飞船在赤道附近确定的水富集形成鲜明对比。在这里，我们使用水动力学模型来研究木星在水云层及其以下的大气动力学，并简化热化学来展示流体动力学对对流层中不平衡物质 CO、PH₃ 和 GeH₄ 丰度的影响。如果 PH₃ 和 GeH₄ 仅提供氧丰度的上限（≤5 倍太阳能），我们的结果表明，使用更新的 CO 热化学，氧富集范围为 2.5-5 倍太阳能。使用常规的 CO 化学时间尺度，我们进一步揭示了湿对流与水云层 CO 丰度之间的相关性。如果通过观测发现这种相关性，它将有利于木星在雪线附近形成，雪线拥有超太阳的氧丰度。