^⋆From left to right : the flattening parameter, f = 1- R_pol/R_eq ≥ 0, where R_pol is the polar radius, and R_eq the equatorial radius, the A-parameter, where L ∈ {1,2} is the number of layer, the relative size q_pol = Z₁/R_pol of the core along the axis of rotation, the decimal log. of the equatorial radius R_eq of the planet in units of the Earth's radius, with R_⊕=6.371 × 10⁸ cm, the decimal log. of the total mass M of the planet in units of the Earth's mass, with M_⊕ = 5.972 × 10²⁷ g, the relative mass of the core, M₁/M, the mean mass-density, 〈ρ〉 = M/V in g/cm³, where V is the volume of the planet, the central-to-mean mass-density ratio, ρ_c/〈ρ〉, the top-to-central mass density ratio in the core, ${\rho }_1^{\mathrm{t}\mathrm{o}\mathrm{p}}/{\rho }_{\mathrm{c}}$, the rotation period, T, in h, the relative size Q = R₁/R_eq of the core at the equator, the interface mass-density jump, $\alpha \equiv {\rho }_1^{\mathrm{t}\mathrm{o}\mathrm{p}}/{\rho }_2^{\mathrm{b}\mathrm{o}\mathrm{t}\mathrm{t}\mathrm{o}\mathrm{m}}$, the central-to-surface mass density ratio, ρ_c/a_L, which is identical to 1/A in the single-layer case, the decimal log. of the central pressure, P_c, in dyn/cm², the decimal log. of the interface pressure, P_i ≡ P(Z₁), in dyn/cm², the normalized moment of inertia, $C=I_z/M{R}_{\mathrm{e}\mathrm{q}}^2$, and the m-parameter defined by $m={\mathrm{\Omega }}^2{R}_{\mathrm{e}\mathrm{q}}^3/GM$. We take G = 6.67259 × 10^-8 for the constant of gravitation.