Effects of the feedback of B_atm. We take into account two representative models, both with M = 1 M_j, T_eq = 1750 K and υ_avg = 793 m/s: one with an evolving B_atm (grey) and the other with a fixed B_atm = 5 G. Left: evolution of the pressure values delimiting the deep (solid) and shallow (if any, dashes) convective regions. Middle: evolution of the internal luminosity, evaluated as L_int = L(p_dyn) (solid), Ohmic luminosity $L_{\mathrm{j}}={\int }_M{ϵ}_{\mathrm{j}}dm$ (dashes), and irradiation power L_irr = 4πR² F_irr (dots). Right: evolution of the planetary radius (solid) and the dynamo radius (dashes).