Rhines Peter B.
School of Oceanography, WB-10, University of Washington, Seattle, Washington 98195.
Chaos. 1994 Jun;4(2):313-339. doi: 10.1063/1.166011.
This is a discussion of concentrated large-scale flows in planetary atmospheres and oceans, argued from the viewpoint of basic geophysical fluid dynamics. We give several elementary examples in which these flows form jets on rotating spheres. Jet formation occurs under a variety of circumstances: when flows driven by external stress have a rigid boundary which can balance the Coriolis force, and at which further concentration can be caused by the beta effect; when there are singular lines like the line of vanishing windstress or windstress-curl, or the Equator; when compact sources of momentum, heat or mass radiate jet-like beta plumes along latitude circles; when random external stirring of the fluid becomes organized by the beta effect into jets; when internal instability of the mass field generates zonal flow which then is concentrated into jets; when bottom topographic obstacles radiate jets, and when frontogenesis leads to shallow jet formation. Essential to the process of jet formation in stratified fluids is the baroclinic life cycle described in geostrophic turbulence studies; there, conversion from potential to kinetic energy generates eddy motions, and these convert to quasibarotropic motions which then radiate and induce jet-like large-scale circulation. Ideas of potential vorticity stirring by eddies generalize the notion of Rossby-wave radiation, showing how jets embedded in an ambient potential vorticity gradient (typically due to the spherical geometry of the rotating planet) gain eastward momentum while promoting broader, weaker westward circulation. Homogenization of potential vorticity is an important limit point, which many geophysical circulations achieve. This well-mixed state is found in subdomains of the terrestrial midlatitude oceans, the high-latitude circumpolar ocean, and episodically in the middle atmosphere. Homogenization expels potential vorticity gradients vertically to the top and bottom of the fluid, and sideways to the edges of flow domains or gyres; in both these ways is jet formation enhanced.
本文从基础地球物理流体动力学的角度,探讨了行星大气和海洋中的集中大规模流动。我们给出了几个基本例子,说明这些流动在旋转球体上如何形成急流。急流的形成发生在多种情况下:当由外部应力驱动的流动具有能平衡科里奥利力的刚性边界,且β效应可导致进一步集中时;当存在诸如风应力或风应力旋度消失线或赤道等奇异线时;当紧凑的动量、热量或质量源沿纬度圈辐射出类似急流的β羽流时;当流体的随机外部搅拌通过β效应组织成急流时;当质量场的内部不稳定性产生纬向流,然后集中成急流时;当底部地形障碍物辐射出急流时,以及当锋生导致浅急流形成时。分层流体中急流形成过程的关键是地转湍流研究中描述的斜压生命周期;在那里,从势能到动能的转换产生涡旋运动,这些涡旋运动转换为准正压运动,然后辐射并诱导出类似急流的大规模环流。涡旋对位涡的搅拌概念推广了罗斯比波辐射的概念,展示了嵌入环境位涡梯度(通常由于旋转行星的球形几何形状)中的急流如何在促进更广泛、更弱的向西环流的同时获得向东动量。位涡的均匀化是一个重要的极限点,许多地球物理环流都能达到这一状态。在地球中纬度海洋的子区域、高纬度环极海洋以及中层大气中偶尔会发现这种充分混合的状态。均匀化将位涡梯度垂直地排向流体的顶部和底部,并横向排向流动区域或涡旋的边缘;通过这两种方式,急流的形成都得到了增强。