Strength of the stellar wind-planet interactions computed in this work. Top: magnetospheric size of the planet, assuming a planetary magnetic field strength of 2 G at the pole (i.e., 1 G at the equator). Middle: maximum dissipated power of Alfvén waves travelling towards the star (Saur et al. 2013). Bottom: maximum dissipated power from the star-planet magnetic reconnection scenario (Lanza 2009). The solid lines are for Model I, and the dashed lines for Model II. The colour scheme follows the one adopted in Fig. 3. The grey arrows in the upper horizontal axes indicate approximate times of mid-transits.