  Atmospheric tides can strongly affect the rotational dynamics of planets. In
the family of Earth-like planets, such as Venus, this physical mechanism
coupled with solid tides makes the angular velocity evolve over long timescales
and determines the equilibrium configurations of their spin. Contrary to the
solid core, the atmosphere is submitted to both tidal gravitational potential
and insolation flux coming from the star. The complex response of the gas is
intrinsically linked to its physical properties. This dependence has to be
characterized and quantified to study the large variety of extrasolar planetary
systems. We develop a theoretical global model where radiative losses, which
are predominant in slowly rotating atmospheres, are taken into account. We
analytically compute the tidal perturbation of pressure, density, temperature
and velocity field from which we deduce the expressions of atmospheric Love
numbers and tidal torque exerted by the star. The dynamics of atmospheric tides
depends on the frequency regime of the tidal perturbation: the thermal regime
near synchronization and the dynamical regime characterizing fast-rotating
planets. The dependence of the torque on the tidal frequency is quantified for
Earth-like and Venus-like exoplanets and is in good agreement with the results
given by Global Climate Models (GCM) simulations. Introducing dissipative
processes such as radiation regularizes the tidal response of the atmosphere,
otherwise it is singular at synchronization. We demonstrate the important role
played by the physical and dynamical properties of a super-Earth atmosphere
(e.g. Coriolis, stratification, background pressure, density, temperature,
radiative emission) and point out the key parameters defining tidal regimes
(e.g. inertia, Brunt-V\"ais\"al\"a, radiative frequencies, tidal frequency) and
characterize the behaviour of the fluid shell with dissipation.
