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Tidal dissipation, which is directly linked to internal structure, is one ofthe key physical mechanisms that drive systems evolution and govern theirarchitecture. A robust evaluation of its amplitude is thus needed to predictevolution time for spins and orbits and their final states. The purpose of thispaper is to refine recent model of the anelastic tidal dissipation in thecentral dense region of giant planets, commonly assumed to retain a largeamount of heavy elements, which constitute an important source of dissipation.The previous paper evaluated the impact of the presence of the static fluidenvelope on the tidal deformation of the core and on the associated anelastictidal dissipation, through the tidal quality factor Qc. We examine here itsimpact on the corresponding effective anelastic tidal dissipation, through theeffective tidal quality factor Qp. We show that the strength of this mechanismmainly depends on mass concentration. In the case of Jupiter- and Saturn-likeplanets, it can increase their effective tidal dissipation by, around, a factor2.4 and 2 respectively. In particular, the range of the rheologies compatiblewith the observations is enlarged compared to the results issued from previousformulations. We derive here an improved expression of the tidal effectivefactor Qp in terms of the tidal dissipation factor of the core Qc, withoutassuming the commonly used assumptions. When applied to giant planets, theformulation obtained here allows a better match between the an elastic core'stidal dissipation of a two-layer model and the observations.

The surface signature of the tidal dissipation of the core in a two-layer planet