Evolution of irradiated HJs with no additional heating, ε_j = 0, for models with M = 1 M_j, ρ_c = 10 g cm⁻³ (top row) or M = 4 M_j, ρ_c = 45 g cm⁻³ (bottom row). Left panels: p(T) profiles at ages t ~ 0.1, 1 and 5 Gyr (dots, dashes, solid lines, respectively), comparing the cases without (black) and with irradiation, T_eq = 1500 K (blue) and 2000 K (orange), all with solar composition. The thicker lines correspond to the convective zone, which extends from the RCB (p ~ 1 - 10³ bar) to the outer core (p > 10⁷ bar). Central panels: Radius evolution of planets with T_eq = 1500 K and different core masses (M_c = 0,10 (M/M_j), 50 (M/M_j) M_e, increasing for darker shades, all with solar composition) and composition of the envelope: pure hydrogen (purple), solar (black) and higher helium and heavier elements content, (Y, Z) = (0.35,0.035) (purple, black and red, respectively, all with M_c = 10 M_φ). In the top central panel we also show the effects of variation of ρ_c = 5 g cm⁻³ (dashes) and ρ_c = 20 g cm⁻³ (dot-dashed lines) for the representative M_c = 10 M_e, solar composition case: since the effect is rather small compared to varying other parameters, we show it only in that particular panel. Right panels: Same as the central panels, but for T_eq = 2000 K.