Top: magnetic field amplitude at the base of the convective envelope along the evolution of a M_⋆ = 1 M_⊙ star, with solar metallicity (Z = 0.0134), uniformly rotating with an initial rotation rate during the disk-locking of the PMS of Ω = 2.5 μHz. The blue, red, and orange lines respectively represent the field estimated by considering the magnetostrophic, buoyancy, and equipartition regimes. The black dashed line represents the location of the limit radius between the internal radiative layer and the convective envelope. Bottom: same as top panel at the top of the convective interior along the evolution of the star. The black dashed line represents the location of the limit radius between the convective core (when existing) and the radiative layer.