Tidal evolution of a Jupiter-mass planet around a fast-rotating 0.1 M_⊙ star with a high dissipation factor. Top panel: evolution of semi-major axis of Jupiter-mass planets (full line) beginning at different initial semi-major axis and of the corresponding corotation distance (dashed line). The red dashed line corresponds to the corotation radius of a star with no planet. Middle panel: evolution of the eccentricity of the planets. Bottom panel: evolution of the rotation period of the planets (full line) and of the corresponding star (dashed line). In both cases, the stellar spin initially increases to reach the spin period of the planet (we consider planets in pseudo-synchronization). Later in the evolution, either the spin-up due to contraction or the spin-down due to stellar wind leads the spin of the star to differentiate from the spin of the planet.