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The atmospheric circulation in the upper atmosphere of hot Jupiter planets isstrongly influenced by the incoming stellar radiation. In this work we explorethe results from a 3D atmospheric model and revisit the main processes drivingthe circulation in hot Jupiter planets. We use the angular momentum transportas a diagnostic and carry out a Fourier analysis to identify the atmosphericwaves involved. We find that the coupling between the angular momentumtransported horizontally by the semi-diurnal tide and the mean circulation isthe mechanism responsible for producing the strong jet at low latitudes. Oursimulations indicate the possible formation of atmospheric indirect cells atlow latitudes. The formation of these cells is induced by the presence of thesemi-diurnal tide that is driven by the stellar irradiation. The tropicalcirculation has an important impact transporting heat and momentum from theupper towards the lower atmosphere. One of the consequences of this heat andmomentum transport is a global increase of the temperature. We show that theinitial conditions do not affect the output of the reference simulation.However, when the period of rotation of the planet was increased ($P_{rot} > 5$Earth days), vertical transport by stationary waves became stronger, transientwaves became non-negligible, and Coriolis influence less dominant, whichallowed a steady state with a strong retrograde jet to be stable. We found thatat least two statically steady state solutions exist for the same planetparameters.

Angular Momentum and Heat Transport on Tidally Locked Hot Jupiter Planets