Properties of the corona on the radius (R/R_schw) – accretion rate (ṁ) parameter plane. All models are calculated for M_BH = 10M_⊙, α_B = 0.1, and ξ = 0.05. The panels display (a) the average temperature of the corona (Eq. (44)) in keV (colors) and τ_cor (contours); (b) the ionization parameter Ξ (colors) and magnetic β parameter (contours), both at the disk midplane; (c) the number density at τ = 2/3 (colors) and the total column density Σ in g cm² (contours); (d) the fraction of radiative energy produced by the corona f (Eq. (45), colors), the maximum value of the magnetic field gradient q (Eq. (35), contours); (e) the y parameter of the warm corona (Eq. (46)), computed up to the thermalization layer τ^⋆ = 1 (colors) and to τ_cor (contours); the (f) photon destruction probability (colors) and electron scattering optical depth (τ_es) (contours) at the thermalization layer; (g) the minimum value of ℒ_rad (Eq. (37)) throughout the disk height (colors), here, green areas are stable disks, and magenta areas indicate thermal instability in the corona, the gray dotted line corresponds to ℒ_rad = 0, and the ionization parameter Ξ at the corona base (contours); and (h) the radiative energy flux normalized to the total accretion flux (colors), and the disk scale ratio H/R (contours).