  Gas giant planets are differentially rotating magnetic objects that have
strong and complex interactions with their environment. In our Solar system,
they interact with their numerous moons while exoplanets with very short
orbital periods (hot Jupiters), interact with their host star. The dissipation
of waves excited by tidal forces in their interiors shapes the orbital
architecture and the rotational dynamics of these systems. Recently,
astrometric observations of Jupiter and Saturn systems have challenged our
understanding of their formation and evolution, with stronger tidal dissipation
in these planets than previously predicted, in contrast to what appears to be
weaker in gas giant exoplanets. These new constraints are motivating the
development of realistic models of tidal dissipation inside these planets. At
the same time, the Juno and Cassini space missions have revolutionised our
knowledge of the interiors of Jupiter and Saturn, whose structure is a
combination of stably stratified zones and convective regions. In this work, we
present results of hydrodynamical calculations modelling tidal waves and their
dissipation in Jupiter, taking for the first time the latest, state-of-the-art
interior model of the planet. We performed 2D numerical simulations of linear
tidal gravito-inertial waves that propagate and dissipate within Jupiter
interior by taking into account viscous, thermal and chemical diffusions. This
new model allows us to explore the properties of the dissipation and the
associated tidal torque as a function of all the key hydrodynamical and
structural parameters.
