  The competition between the torques induced by solid and thermal tides drives
the rotational dynamics of Venus-like planets and super-Earths orbiting in the
habitable zone of low-mass stars. The tidal responses of the atmosphere and
telluric core are related to their respective physical properties and strongly
depend on the tidal frequency. The resulting torque determines the possible
equilibrium states of the planet's spin. We compute here an analytic expression
for the total tidal torque exerted on a Venus-like planet. This expression is
used to characterize the equilibrium rotation of the body. Close to the star,
the solid tide dominates. Far from it, the thermal tide drives the rotational
dynamics of the planet. The transition regime corresponds to the habitable
zone, where prograde and retrograde equilibrium states appear. We demonstrate
the strong impact of the atmospheric properties and of the rheology of the
solid part on the rotational dynamics of Venus-like planets, highlighting the
key role played by dissipative mechanisms in the stability of equilibrium
configurations.
