Abstract
The dynamics of a thin atmospheric layer (1–340 bar) below the cloud tops of Jupiter is simulated with a three‐dimensional, nonlinear transformed spectral model. The gas is compressible and stratified. Commensurate with the observed emitted radiation from Jupiter's atmosphere, the transport of the planet's internal energy in the lower region is taken to be convective, but solar heating is not accounted for. In qualitative agreement with observations, the model produces alternating wind bands and a dominant prograde equatorial jet. The zonal wind speed at the equator is within a factor of 2 of the observed values.
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