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• W2011343693 endingPage "113" @default.
• W2011343693 startingPage "97" @default.
• W2011343693 abstract "The ice giant planets, Uranus and Neptune, have magnetic fields, atmospheric circulation patterns, and thermal emissions that are distinct from other planets in our Solar System. However, no self-consistent dynamical model has been able to reproduce all of these observations. We hypothesize that the dynamos and surface winds are dynamically coupled and argue that their characteristics are a consequence of three-dimensional turbulence that may be excited in planetary-scale water layers. Here we present dynamo models with thick and thin spherical shell geometries consistent with the range of possible internal structures of Uranus and Neptune. The style of convection is chosen a priori to yield small-scale and disorganized turbulence. In agreement with ice giant observations, both simulations (i) generate multipolar magnetic fields by fluctuating dynamo action, (ii) produce zonal jets with retrograde flow at the equator through angular momentum mixing, and (iii) predict local equatorial peaks in internal heat fluxes due to equatorial upwellings induced primarily by Hadley-like circulation cells. Thus, we argue that three-dimensional convective turbulence can explain the first-order geophysical observations of the ice giants." @default.
• W2011343693 created "2016-06-24" @default.
• W2011343693 creator A5025479795 @default.
• W2011343693 creator A5041389413 @default.
• W2011343693 creator A5063834115 @default.
• W2011343693 creator A5072256015 @default.
• W2011343693 date "2013-05-01" @default.
• W2011343693 modified "2023-09-27" @default.
• W2011343693 title "Turbulent models of ice giant internal dynamics: Dynamos, heat transfer, and zonal flows" @default.
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