Equatorial superrotation in shallow atmospheres
Equatorial superrotation in shallow atmospheres
复制标题
浅层大气中的赤道超自转
DOI：
10.1029/2008gl036060
复制
发表时间：
2008
影响因子：
5.2
通讯作者：
L. M. Polvani
中科院分区：
文献类型：
--
作者：
Richard K. Scott;L. M. Polvani
简单的浅水模型已经成功地再现了巨行星大气中的两个关键观测结果：强劲且完全湍流的纬向急流的形成以及纬向风振幅随纬度的减小。然而，迄今为止，它们始终未能重现在此类行星上经常观察到的强烈顺行（超级旋转）赤道风。在本文中，我们表明，只要考虑到辐射弛豫引起的大规模能量耗散的物理过程，浅水模型不仅可以产生超级旋转风，而且可以非常稳健地产生。当能量被线性摩擦消除时，赤道超自转就不会发展；当通过辐射弛豫消除能量时，显然在任何变形半径处都会发生超旋转。
Simple, shallow‐water models have been successful in reproducing two key observables in the atmospheres of the giant planets: the formation of robust, and fully turbulent, latitudinal jets and the decrease of the zonal wind amplitude with latitude. However, they have to date consistently failed in reproducing the strong prograde (superrotating) equatorial winds that are often observed on such planets. In this paper we show that shallow water models not only can give rise to superrotating winds, but can do so very robustly, provided that the physical process of large‐scale energy dissipation by radiative relaxation is taken into account. When energy is removed by linear friction, equatorial superrotation does not develop; when energy is removed by radiative relaxation, superrotation develops at apparently any deformation radius.