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Three-dimensional equatorial trapped waves excited by stellar isolation andthe resulting equatorial superrotating jet in a vertical stratified atmosphereof a tidally-locked hot Jupiter are investigated. Taking the hot Jupiter HD189733b as a fiducial example, we analytically solve a set of linear equationssubject to stationary stellar heating with a uniform zonal-mean flow included.We also extract wave information in the final equilibrium state of theatmosphere from the radiative hydrodynamical simulation for HD 189733b byDobbs-Dixon & Agol (2013). We find that the analytic wave solutions are able toqualitatively explain the three-dimensional simulation results. Studying thevertical structure of waves allows us to explore new wave features such as thewestward tilt of wavefronts related to the Rossby-wave resonance as well asdouble gyres of dispersive Rossby waves. We also make an attempt to apply ourlinear wave analysis to explain some numerical features associated with theequatorial jet development seen in the GCM by Showman & Polvani (2011). Duringthe spin-up phase of the equatorial jet, the acceleration of the jet as aresult of the divergence of the wave momentum flux can be in principle boostedby the Rossby-wave resonance as the superrotating jet speed is close to thephase speed of the Rossby waves. However, we also find that as the jet speedincreases, the Rossby-wave structure shifts eastward, while the Kelvin-wavestructure remains approximately stationary, leading to the decline of theacceleration rate. Our analytic model of jet evolution implies that thereexists only one stable equilibrium state of the atmosphere, possibly implyingthat the final state of the atmosphere is independent of initial conditions inthe linear regime. Limitations and future improvements are also discussed.

3D Structures of equatorial waves and the resulting superrotation in the atmosphere of a tidally locked hot Jupiter