  Layered semi-convection could operate in giant planets, potentially
explaining the constraints on the heavy elements distribution in Jupiter
deduced recently from Juno observations, and contributing to Saturn's
luminosity excess or the abnormally large radius of some hot Jupiters. This is
a state consisting of density staircases, in which convective layers are
separated by thin stably stratified interfaces. The efficiency of tidal
dissipation in a planet depends strongly on its internal structure. It is
crucial to improve our understanding of the mechanisms driving this
dissipation, since it has important consequences to predict the long-term
evolution of any planetary system. In this work, our goal is to study the
resulting tidal dissipation when internal waves are excited by other bodies
(such as the moons of giant planets) in a region of layered semi-convection. We
find that the rates of tidal dissipation can be significantly enhanced in a
layered semi-convective medium compared to a uniformly convective medium,
especially in the astrophysically relevant sub-inertial frequency range. Thus,
layered semi-convection is a possible candidate to explain high tidal
dissipation rates recently observed in Jupiter and Saturn.
