Secular evolution of a star–planet system formed by a median rotating solar twin (M_⋆ = 1 M_⊙,  P_rot,ini = 5 days) orbited by a magnetized planet (a_ini = 0.02 AU,  B_p = 1 G) for three different planetary masses: M_p = {0.01,  0.1,  1} M_Jup (dark to light colors). Top panel: semi-major axis (solid lines). In shades of red: wind braking + tides, in shades of blue: wind braking + tides + magnetic effects, in shades of purple: Roche limit, defined as in Benbakoura et al. (2019). In dashed-dotted black: stellar radius. Middle panel: time evolution of the rotation rate of the stellar envelope (solid line) and of the stellar core (dashed line). Bottom panel: departure of the rotation period of the planet-hosting star compared to an isolated star.