Schematic representation of our tidal and thermal model. Left: internal structure for the planet, composed of water ice I (white), high-pressure ice polymorphs (HPP, gray), rock (dark gray), and iron (black). The volume fractions of each constituent material were calculated based on the mean density of each planet (see Sect. 2). Middle: to calculate the response of each planet to tidal forcing, we constructed a volume-weighted average viscosity and rigidity for the planet based on the ϕ values and the rheology of each constituent material. A value of the imaginary part of the k₂ Love number, and the tidal heat flux F_tidal were calculated. Right: the temperature in the planet’s interior (T_eq) was governed by a balance between heat generation by tides and transport by solid-state convection; the efficiency of both processes depends sensitively on the viscosity and rigidity of the planet. The net global heat flux was calculated from the tidal heat flux and the incident sunlight from the star, F_⋆.