  Hot Jupiters are submitted to an intense stellar heating. The resulting
thermal tides can torque their atmospheres into asynchronous rotation, while
these planets are usually assumed to be locked into spin-orbit synchronization
with their host star. Particularly, the thermal atmospheric torque can be
greatly enhanced by the dynamical component of the tidal response, that is the
component associated with the propagation of internal waves. Owing to the
involved complex dynamics, semi-analytical approaches are crucial to understand
the physical mechanisms that are responsible for the frequency-resonant
behavior of thermal tides, and quantify the atmospheric tidal torque. In this
work, we revisit the early works by Arras \& Socrates (2010) and present an
improved modeling of thermal tides taking into account rotation and radiative
cooling. Using this new modeling, we compute analytically the atmospheric tidal
response of hot Jupiters and show that resonances associated with low-frequency
internal gravity waves are able to drive asynchronous zonal flows in the range
1-30 days.
