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Convection zones comprise hot, light, upwelling fluid; and cold, dense, downwelling fluid. Ergo, convection zones are characterized by two types of fluids, having (two) separate temperatures, at every altitude / depth. Convection zones must be mathematically modeled accordingly. The following figure sketches a star's temperature profile (T vs. r), qualitatively indicating a convection zone, with steep (supra-adiabatic) overall average temperature gradient, spanning the distance between an interior, and another exterior, region wherein the temperature profile is shallow (sub-adiabatic), and so stable against convection. Upon reaching the convection zone, fluid rises along the "hot" adiabat to the top of the zone, whereat it cools, and then sinks along the "cold" adiabat to the bottom of the zone, whereat it (re-)heats, etc. Convection zones form natural heat engines. Their two-fluid character defines their properties; they must be mathematically modeled commensurately. Temperature-dependent density contrast (δρ) determines the relative buoyancy force, counteracted by viscosity between the cells, which depends upon velocity contrast (δv) and characteristic cell size; mass continuity (δ(ρv)=0) helps solve the system for the unknown variables.
A Wikipedia talk page is not the place to publish original research or synthesis. If this model has been published in a reliable peer-reviewed journal, then it can be added to the article with the appropriate cite, assuming of course that it is not given undue weight. --Yaush (talk) 14:48, 22 October 2012 (UTC)