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Atmospheric tides can have a strong impact on the rotational dynamics ofplanets. They are of most importance for terrestrial planets located in thehabitable zone of their host star, where their competition with solid tides islikely to drive the body towards non-synchronized rotation states ofequilibrium, as observed in the case of Venus. Contrary to other planetarylayers, the atmosphere is sensitive to both gravitational and thermal forcings,through a complex dynamical coupling involving the effects of Coriolisacceleration and characteristics of the atmospheric structure. These keyphysics are usually not taken into account in modelings used to compute theevolution of planetary systems, where tides are described with parametrisedprescriptions. In this work, we present a new ab initio modeling of atmospherictides adapting the theory of the Earth's atmospheric tides (Chapman & Lindzen1970) to other terrestrial planets. We derive analytic expressions of the tidaltorque, as a function of the tidal frequency and parameters characterizing theinternal structure (e.g. the Brunt-V\"ais\"al\"a frequency, the radiativefrequency, the pressure heigh scale). We show that stratification plays a keyrole, the tidal torque being strong in the case of convective atmospheres (i.e.with a neutral stratification) and weak in case of atmosphere convectivelystable. In a second step, the model is used to determine the non-synchronizedrotation states of equilibrium of Venus-like planets as functions of thephysical parameters of the system. These results are detailed inAuclair-Desrotour et al. (2017a) and Auclair-Desrotour et al. (2017b).

Atmospheric tides and their consequences on the rotational dynamics of terrestrial planets