Shallow models The first attempts to explain Jovian atmospheric dynam ics date back to the 1960s.   They were partly based on terrestrial meteorology , which was well developed at that time. Those shallow models assumed that the jets on Jupiter are driven by small scale turbulence , which is in turn maintained by moist convection in the outer layer of the atmosphere (above the water clouds).   The moist convection is a phenomenon related to the condensation and evaporation of water and is one of the major drivers of terrestrial weather.  The production of the jets in this model is related to a well-known property of two dimensional turbulence—the so-called inverse cascade, in which small turbulent structures (vortices) merge to form larger ones.  The finite size of the planet means that the cascade can not produce structures larger than some characteristic scale, which for Jupiter is called the Rhines scale. Its existence is connected to production of Rossby waves
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This note was uploaded on 12/15/2011 for the course AST AST1002 taught by Professor Emilyhoward during the Fall '10 term at Broward College.