Tidal dissipation is known as one of the main drivers of the secular
evolution of planetary systems. It directly results from dissipative mechanisms
that occur in planets and stars' interiors and strongly depends on the
structure and dynamics of the bodies. This work focuses on the mechanism of
viscous friction in stars and planetary layers. A local model is used to study
tidal dissipation. It provides general scaling laws that give a qualitative
overview of the different possible behaviors of fluid tidal waves. Furthermore,
it highlights the sensitivity of dissipation to the tidal frequency and the
roles played by the internal parameters of the fluid such as rotation,
stratification, viscosity and thermal diffusivity that will impact the
spins/orbital architecture in planetary systems.Comment: 4 pages, 3 figures, IAU 310 symposium proceedings, Complex planetary
system
