Until recently, observations of the giant planets of our Solar System were confined to sampling relatively shallow regions of their atmospheres, leaving many uncertainties as to the dynamics of deeper layers. The Cassini and Juno missions to Saturn and Jupiter, however, have begun to address these issues, for example, by measuring their gravity and magnetic fields. The results show that the zonally coherent jets and cloud bands extend to levels where the electrical conductivity of the fluid becomes significant, whereas large-scale vortices, such as the Great Red Spot, are relatively shallow but may have deep-seated roots. The polar regions also exhibit intense cyclonic vortices that, on Jupiter, arrange themselves into remarkably regular “vortex crystals.” Numerical models seem able to capture some of this complexity, but many issues remain unresolved, suggesting a need for models that can represent both deep and shallow processes sufficiently realistic ally to compare with observations.

中文翻译：

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木星和土星天气层的动力学：卡西尼号和朱诺号之后的综合


直到最近，对太阳系巨行星的观测还仅限于对其大气中相对较浅的区域进行采样，这给更深层的动力学留下了许多不确定性。然而，卡西尼号和朱诺号对土星和木星的任务已经开始解决这些问题，例如，通过测量它们的引力和磁场。结果表明，纬向相干的射流和云带延伸到流体的电导率变得显着的水平，而大尺度的漩涡，如大红斑，相对较浅，但可能具有深根。极地地区还表现出强烈的气旋涡旋，在木星上，这些涡旋会自行排列成非常规则的“涡旋晶体”。数值模型似乎能够捕捉到这种复杂性，但许多问题仍未解决，这表明需要能够代表深层和浅层过程的模型，这些过程足够真实，可以与观测进行比较。