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Tidal dissipation in planetary interiors is one of the key physicalmechanisms that drive the evolution of star-planet and planet-moon systems.Tidal dissipation in planets is intrinsically related to their internalstructure. In particular, fluid and solid layers behave differently under tidalforcing. Therefore, their respective dissipation reservoirs have to becompared. In this work, we compute separately the contributions of thepotential dense rocky/icy core and of the convective fluid envelope of gaseousgiant planets, as a function of core size and mass. We demonstrate that ingeneral both mechanisms must be taken into account.

Understanding tidal dissipation in gaseous giant planets from their core to their surface