Fig. 7.
Vertical structure of the disk-corona models computed at R = 10 RSchw for different values of the accretion rate (ṁ), plotted against the total optical depth τ. The panels show (a) the gas temperature, (b) the gradient of the magnetic pressure (Eq. (34)), (c) the radiative energy flux normalized to the total accretion flux Facc, (d) the cooling function gradient (Eq. (37)), (e) the contribution of Compton cooling to the total cooling, and (f) the ionization parameter Ξ (Eq. (43)).
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