Zonal (eastward) wind in a simulation of Jupiter with a 3D general circulation model. This simulation was part of a paper published in 2009. Here we used slightly different dissipation parameters (which are poorly constrained by data) than in the simulation in a later (2010) paper. This leads to weaker and narrower jets than in the later simulations.
As in the later simulations, the equatorial (Rossby) waves responsible for the generation of superrotation are clearly recognizable.
References: Schneider, T., and J. Liu, 2009: Formation of jets and equatorial superrotation on Jupiter. Journal of the Atmospheric Sciences, 66, 579–601.
Liu, J., and T. Schneider, 2010: Mechanisms of jet formation on the giant planets. Journal of the Atmospheric Sciences, 67, 3652–3672.
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