the present values of their orbital parameters, contrarily to what has been claimed in previous calculations based on truncated eccentricity models [@ISB09]. Finally, in §\[sec:global\], we apply our model to the case of some of the discovered bloated planets. We show that, although tidal heating can explain the presently observed radius of some [*moderately bloated*]{} hot Jupiters, as indeed suggested in some previous studies, tidal heating alone cannot explain [*all*]{} the anomalously large radii. Indeed, in these cases, eccentricity damping occurs too early in the system’s tidal evolution (assuming a genuine two-body planetary system) to lead to the present state of the planet’s contraction.

Model Description {#sec:hyp}
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Internal evolution {#sec:intevolution}
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The main physics inputs (equations of state, internal composition, irradiated atmosphere models, boundary conditions) used in the present calculations have been described in details in previous papers devoted to the evolution of extrasolar giant planets [@BCB03; @BCB08; @LBC09] and are only briefly outlined below. The evolution of the planet is based on a consistent treatment between the outer non-grey irradiated atmospheric structure and the inner structure. The interior is composed primarily of a gaseous H/He envelope whose thermodynamic properties are described by the Saumon-Chabrier-VanHorn equation of state (EOS, 