The zonal flow in Jupiter's upper troposphere is organized into alternatingretrograde and prograde jets, with a prograde (superrotating) jet at theequator. Existing models posit as the driver of the flow either differentialradiative heating of the atmosphere or intrinsic heat fluxes emanating from thedeep interior; however, they do not reproduce all large-scale features ofJupiter's jets and thermal structure. Here it is shown that the difficulties inaccounting for Jupiter's jets and thermal structure resolve if the effects ofdifferential radiative heating and intrinsic heat fluxes are consideredtogether, and if upper-tropospheric dynamics are linked to amagnetohydrodynamic (MHD) drag that acts deep in the atmosphere. Barocliniceddies generated by differential radiative heating can account for theoff-equatorial jets; meridionally propagating equatorial Rossby waves generatedby intrinsic convective heat fluxes can account for the equatorialsuperrotation. The zonal flow extends deeply into the atmosphere, with itsspeed changing with depth, up to depths at which the MHD drag acts. The theoryis supported by simulations with an energetically consistent generalcirculation model of Jupiter's outer atmosphere. A simulation that incorporatesdifferential radiative heating and intrinsic heat fluxes reproduces Jupiter'sobserved jets and thermal structure and makes testable predictions about as-yetunobserved aspects thereof. A control simulation that incorporates onlydifferential radiative heating but not intrinsic heat fluxes producesoff-equatorial jets but no equatorial superrotation; another control simulationthat incorporates only intrinsic heat fluxes but not differential radiativeheating produces equatorial superrotation but no off-equatorial jets.
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