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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{0955fig1.ps} % \end{figure}$ Figure 1: Radial mass flow rate in the corona for given parameters $\eta _{\rm M}=1$ , evaporation, and $\eta _{\rm M}=-1$ , condensation; Solid lines: solutions for standard viscosity, ${\alpha =0.3}$ , dashed lines solutions for a lower viscosity $\alpha =0.09$ . Note that the curves do not represent a distribution of the radial mass flow in the corona, but give the typical mass flow rate in the local corona at the distance $R/R_{\rm S}$ under the conditions specified with ${\eta _{\rm M}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=13.6cm,clip]{0955fig2.ps} \end{figure}$ Figure 2: Vertical structure of the corona with mass evaporation from the disk to the corona ( $\eta _{\rm M}=1$ , left panel) and with mass condensation from the corona to the disk ( $\eta _{\rm M}=-1$ , right panel) at the distance $R=10^4 ~R_{\rm S}$ from a central black hole of $3.3\times10^6~M_\odot$ . z/R ratio of height above midplane to distance. Distribution of the following quantities: temperature T in units of virial temperature $T_{\rm {vir}}$ , pressure P, thermal conductive flux $F_{\rm c}$ and vertical mass flow rate $\dot m=\rho v_z$ (the latter ones scaled to their values at the lower boundary: $P_0\approx 1.9\times 10^{-2}~{\rm dyn}~{\rm cm}^{-2}$ , $F_{\rm c0}\approx -5.2\times 10^4$ erg ${\rm cm}^{-2}~{\rm s}^{-1}$ , $\dot m_0\approx 3.4\times 10^{-11}~ {\rm g~cm}^{-2}~{\rm s}^{-1}$ for the left panel, and $P_0\approx 0.6~{\rm dyn}~{\rm cm}^{-2}$ , $F_{\rm c0}\approx -1.6\times 10^{5}$ erg ${\rm cm}^{-2}~{\rm s}^{-1}$ , $\dot m_0\approx -10^{-9}~ {\rm g~cm}^{-2}~{\rm s}^{-1}$ for the right panel).
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{0955fig3.ps} \end{figure}$ Figure 3: Radial mass flow rate in the corona ( upper curve) together with condensation ${\rm rate}=-2\pi R^2 \dot m_0/\dot M_{\rm Edd}$ (dashed line), and evaporation ${\rm rate}=2\pi R^2 \dot m_0/\dot M_{\rm Edd}$ (lower solid line), for the Galactic Center at $R=10^4 ~R_{\rm S}$ (viscosity parameter ${\alpha =0.3}$ ). At $\eta _{\rm M}=-1$ all mass that flows in the corona has come from the outside and condenses into the cool disk, then with increasing ${\eta _{\rm M}}$ a smaller part settles into the disk until at $\eta _{\rm M}=0$ no mass condenses. At $\eta _{\rm M}=1$ all mass flowing inward in the corona has evaporated from the cool disk (for details see text).
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In the text