Evolution of the CoRoT-2 system in the presence of tides, as a function of age expressed in billion years. From top to bottom, the five panels are: a) planet’s transit radius; b) planet’s orbital eccentricity; c) planet’s orbital period in days; d) planet’s spin period in days; e) star’s spin period in days. The observational constraints are indicated by colored areas (see Fig. 12). For visibility purposes, the constraint on the orbital period has been increased by a factor 10⁵. Three models are shown: Black lines: a model with , , e_ini = 0.4, a_ini = 0.04 AU, corresponding to a preferred model of Gillon et al. (2010). Purple lines: a model including migration for the first 10 Ma, and , , e_ini = 0.4, a_ini = 0.13 AU. Blue lines: a close-encounter model, for which the eccentricity is suddenly raised to e ~ 0.77 after 300 Ma, presumably due to close encounters with another planet. This assumes , , a_ini = 0.1 AU. The thick parts of the lines corresponds to epochs for which the eccentricity and orbital periods are in agreement with the observations (see text).