a) Stability diagram for thin magnetic flux tubes in the middle of the solar overshoot region, for Sun-like differential rotation (given by Eq. (23)). White regions represent stable flux tubes, while shaded areas indicate instability. For light-shaded areas, the fastest growing mode has azimuthal wave number m = 1, while for dark-shaded areas it is m = 2. Contours show lines of constant growth times (e-folding times), labelled in units of days. b) Time-latitude diagram of the dynamo-generated mean toroidal magnetic field B(λ,t) at the bottom of the convection zone (contours at  ± 0.04,  ± 0.1,  ± 0.3,  ± 0.5,  ± 0.7,  ± 0.9 of the maximum value of B, solid for positive and dashed for negative values) and of the flux loops emerging at the surface (dots) for a Sun-like star. c) Time-latitude diagram of the longitudinally averaged radial surface magnetic field for the solar model. d) Time variation of the total unsigned surface magnetic flux. The values are averaged over 27-day time intervals.