气态巨行星大气极涡的深层模式模拟
Deep model simulation of polar vortices in gas giant atmospheres
摘要：
卡西尼号和朱诺号探测器在土星和木星的极地地区发现了大型连贯的气旋漩涡，这与低纬度地区看到的东西带状喷流结构形成了鲜明的对比。争论的焦点是喷流是浅的，还是延伸到行星包络线的更深处。最近的实验和观测表明，深对流模式的相关性，以成功地解释喷流结构和气旋相干涡远离极地地区最近已经模拟，包括一个额外的分层浅层。在这里，我们提出了新的对流模型能够产生长寿命的极涡。使用模拟参数相关的巨大的行星大气，我们发现流动制度，是在与地转湍流（GT）理论在旋转对流形成大规模的相干结构，通过一个高档的能量转移完全三维的。我们的模拟生成的极地特征在质量上与朱诺号和卡西尼号所看到的相似：它们与木星上看到的气旋涡旋结构相匹配;或者可以解释存在一个向下延伸到低纬度的强烈极地涡旋，具有显着的螺旋形态和土星上看到的六边形图案。我们的研究结果表明，这些漩涡可以在行星内部深处产生。区分这两个极流制度的过渡描述，解释在不同的力平衡方面，并与以前的浅大气模型，其特点是极涡动力学在巨行星。此外，热传输性能的调查确认最近的标度律的背景下，减少模型的GT。
英文摘要：
The Cassini and Juno probes have revealed large coherent cyclonic vortices in the polar regions of Saturn and Jupiter, a dramatic contrast from the east-west banded jet structure seen at lower latitudes. Debate has centered on whether the jets are shallow, or extend to greater depths in the planetary envelope. Recent experiments and observations have demonstrated the relevance of deep convection models to a successful explanation of jet structure and cyclonic coherent vortices away from the polar regions have been simulated recently including an additional stratified shallow layer. Here we present new convective models able to produce long-lived polar vortices. Using simulation parameters relevant for giant planet atmospheres we find flow regimes that are in agreement with geostrophic turbulence (GT) theory in rotating convection for the formation of large scale coherent structures via an upscale energy transfer fully three-dimensional. Our simulations generate polar characteristics qualitatively similar to those seen by Juno and Cassini: they match the structure of cyclonic vortices seen on Jupiter; or can account for the existence of a strong polar vortex extending downwards to lower latitudes with a marked spiral morphology and the hexagonal pattern seen on Saturn. Our findings indicate that these vortices can be generated deep in the planetary interior. A transition differentiating these two polar flows regimes is described, interpreted in terms of different force balances and compared with previous shallow atmospheric models which characterised polar vortex dynamics in giant planets. In addition, the heat transport properties are investigated confirming recent scaling laws obtained in the context of reduced models of GT.
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