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Tidal dissipation is known as one of the main drivers of the secularevolution of planetary systems. It directly results from dissipative mechanismsthat occur in planets and stars' interiors and strongly depends on thestructure and dynamics of the bodies. This work focuses on the mechanism ofviscous friction in stars and planetary layers. A local model is used to studytidal dissipation. It provides general scaling laws that give a qualitativeoverview of the different possible behaviors of fluid tidal waves. Furthermore,it highlights the sensitivity of dissipation to the tidal frequency and theroles played by the internal parameters of the fluid such as rotation,stratification, viscosity and thermal diffusivity that will impact thespins/orbital architecture in planetary systems.

Scaling laws to understand tidal dissipation in fluid planetary layers and stars