  Atmospheric tides can have a strong impact on the rotational dynamics of
planets. They are of most importance for terrestrial planets located in the
habitable zone of their host star, where their competition with solid tides is
likely to drive the body towards non-synchronized rotation states of
equilibrium, as observed in the case of Venus. Contrary to other planetary
layers, the atmosphere is sensitive to both gravitational and thermal forcings,
through a complex dynamical coupling involving the effects of Coriolis
acceleration and characteristics of the atmospheric structure. These key
physics are usually not taken into account in modelings used to compute the
evolution of planetary systems, where tides are described with parametrised
prescriptions. In this work, we present a new ab initio modeling of atmospheric
tides adapting the theory of the Earth's atmospheric tides (Chapman & Lindzen
1970) to other terrestrial planets. We derive analytic expressions of the tidal
torque, as a function of the tidal frequency and parameters characterizing the
internal structure (e.g. the Brunt-V\"ais\"al\"a frequency, the radiative
frequency, the pressure heigh scale). We show that stratification plays a key
role, the tidal torque being strong in the case of convective atmospheres (i.e.
with a neutral stratification) and weak in case of atmosphere convectively
stable. In a second step, the model is used to determine the non-synchronized
rotation states of equilibrium of Venus-like planets as functions of the
physical parameters of the system. These results are detailed in
Auclair-Desrotour et al. (2017a) and Auclair-Desrotour et al. (2017b).
