Upper panel: evolution of the surface equatorial velocity for various 2 M_⊙ models with and without planets. The continuous black curves are for models without planets. The lower curve is for the models with Ω_ini/ Ω_crit = 0.1, the upper curve for Ω_ini/ Ω_crit = 0.5. The coloured curves are for models with planets. The evolution is shown only until the engulfment. The continuous (dashed) curves correspond to Ω_ini/ Ω_crit = 0.1 (Ω_ini/ Ω_crit = 0.5) models. The planets have a mass equal to 15 M_J. From left to right, we show the case for an initial distance between the star and the planet equal to 0.5, 1.0 and 1.5 au. Lower panel: evolution of the semi-major axis of the planetary orbit (coloured continuous and dashed curves) and the evolution of the stellar radii (black lower curves). The long-short dashed (magenta) curve shows the evolution of the corotation radius for the 2 M_⊙ with Ω_ini/ Ω_crit = 0.5 without planet, the dotted line for the same model with a tidal interaction with a 15 M_j planet beginning its orbital evolution at a distance of 1 au from the star. The curve stops at engulfment.