  Internal gravity waves propagate in stellar radiative zones and transport
angular momentum throughout the evolution of stars, shaping the internal
rotation pro le of these regions. We use the analytical study of Andre\'e et
al. (2018) to assess the impact of rotation and differential rotation on the
thermal dissipation of internal gravity waves near the equatorial plane,
without making any assumption on the relative strength of rotation relative to
that of the background stable stratification. This dissipation is one of the
mechanisms allowing a wave-induced deposition/extraction of angular momentum.
Here, we apply the analysis to a 3 solar mass star of which we have computed
the one-dimensional evolution, from the pre-main sequence to the end of the
main sequence. We show that rotation and differential rotation do not
significantly modify the efficiency of the damping of internal gravity waves by
thermal diffusion, except very close to their excitation region.
