Properties of the warm corona on the accretion rate-magnetic viscosity parameter plane. All models have been calculated for M_BH = 10⁸ M_⊙ and R = 6 R_Schw. Upper panels show: a) average temperature, T_avg, of the corona in keV (colors) and optical depth of the base of the warm corona τ_cor (contours); b) Ξ (colors) and magnetic pressure parameter β (contours) both at τ_cor; and c) number density n_H in cm⁻³ (colors) at τ_cor and total column density Σ in g cm⁻² (contours). Dotted contour here shows where dΣ/dṁ = 0. Bottom panels display: d) y_avg parameter of the warm corona at the thermalization zone, namely, τ^* = 1 (colors), and at the base of the corona, τ_cor (contours); e) fraction of radiative energy produced by the corona f (colors) and the maximum value of magnetic field gradient q (contours); and f) the minimum value of ℒ_rad throughout the disk height (colors) and Thomson optical depth, τ_min, for which it occurs (contours), green areas are stable disks, whereas magenta areas indicate thermal instability in the corona, the gray dotted line corresponds to ℒ_rad = 0. In all panels, the dark contour indicates the parameter sub-space affected by the density inversion.