Rotational evolution due to tides in a Kepler-38-like CB planet (see Table 1), considering different values of planetary relaxation factor γ₂, illustrated here with different colours (see legend in the upper left panel). The evolution was calculated by direct numerical integration of Eqs. (7) and (14). The evolution of the planetary spin rate Ω₂ is shown in the upper left panel (zoomed around Ω₂ ~ n₂ in a secondary plot), the lag-angle δ₂ in the upper right panel, the equatorial flattening in the lower left panel and the polar flattening in the lower right panel. The dashed black line in the upper left panel shows the stationary solution predicted by Zoppetti et al. (2019) with a CTL-based model.