All Figures

$\begin{figure} \par\hspace*{1.5mm}\includegraphics[width=8.89cm]{8220Fig1a.eps}\\ [1mm] \hspace*{-2mm}\includegraphics[width=8.8cm]{8220Fig1b.eps}\end{figure}$ Figure 1: Calculated cloud structure for a model with $T_{\rm eff} = 1800$ K and $\log g = 5$ ( cond AMES). 1st panel: prescribed temperature T (solid) and mixing time scale $\tau _{\rm mix}$ (dashed). 2nd panel: nucleation rate $J_\star$ (solid) and net growth velocity $\chi _{\rm net}$ (dashed). 3rd panel: mean grain size $\langle a\rangle=\sqrt[3]{3/(4\pi)}~L_1/L_0$ (solid) and mean fall speed $\langle v^{\hspace{-0.8ex}^{\circ}}_{\rm dr}\rangle=\sqrt{\pi}~g\rho_{\rm d} \langle a\rangle~/~(2\rho c_T)$ (dashed). The 4th panel depicts the effective supersaturation ratios $S_{\rm eff}$ for all solids involved.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{8220Fig2a.eps}\par\includegraphics[width=8.8cm,clip]{8220Fig2b.eps}\end{figure}$ Figure 2: Volume fractions $V_{\rm s}/V_{\rm tot}$ ( top) and mass fractions $M_{\rm s}/M_{\rm tot}$ ( bottom) of the various solid compounds for the model depicted in Fig. 1. The temperature scale follows the atmospheric stratification, being cool at the top and hot at the bottom.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{8220Fig3a.eps}\\ \includegraphics[width=8.8cm,clip]{8220Fig3b.eps}\end{figure}$ Figure 3: Volume fractions $V_{\rm s}/V_{\rm tot}$ for different $T_{\rm eff}$ ( top) and different $\log~g$ ( bottom). Only the more abundant solid compounds are viewed, in contrast to Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{8220Fig4.eps}\\ \end{figure}$ Figure 4: Comparison of results for different stellar parameter. $1{\rm st}$ box: mass density $\rho$ , 2nd box: nucleation rate $J_\star$ , 3rd box: net growth velocity $\chi ^{\rm net}$ 4th box: mean particle size $\langle a\rangle$ , 5th box: mean fall speed $\langle v^{\hspace{-0.8ex}^{\circ}}_{\rm dr}\rangle$ . All quantities are plotted as function of temperature T. Dotted line: $T_{\rm eff}=1300$ K, $\log~g = 5$ ; solid line: $T_{\rm eff} = 1800$ K, $\log~g = 5$ ; dash-dotted line: $T_{\rm eff}=1300$ K, $\log~g = 3$ ; dashed line: $T_{\rm eff} = 1800$ K, $\log~g = 3$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8220Fig5a.eps}\\ {\hspace*{1.5mm}\includegraphics[width=8.5cm]{8220Fig5b.eps}\hspace*{1.5mm}} \end{figure}$ Figure 5: Dust-to-gas mass ratios $\rho _{\rm d}/\rho _{\rm gas}$ and dust mass column densities $M_{\rm dust}$ for brown dwarf and giant-planets atmospheres. 1st panel: linear plot, 2nd panel: logarithmic plot. Dotted line: $T_{\rm eff}=1300$ K, $\log~g = 5$ ; solid line: $T_{\rm eff}=1800~$ K, $\log~g = 5$ ; dash-dotted line: $T_{\rm eff}=1300$ K, $\log~g = 3$ ; dashed line: $T_{\rm eff}=1800~$ K, $\log~g = 3$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{8220Fig6.eps}\end{figure}$ Figure 6: Element abundances in dust $\epsilon _{\rm d}$ (thick solid) and in the gas phase $\epsilon _{\rm i}$ (dashed). The solar values $\epsilon _{\rm i, Sun}$ (thin solid) and the linear dust-to-gas ratio $\rho _{\rm d}/\rho _{\rm gas}$ ( lowest panel) are shown for comparison. The stellar parameters are $T_{\rm eff} = 1800$ K and $\log~g = 5$ as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{8220Fig7.eps}\end{figure}$ Figure 7: Element abundances involved in the dust formation process for two effective temperatures and two different gravities. Dotted blue: $T_{\rm eff}=1300$ K, $\log~g = 5$ ; solid green: $T_{\rm eff} = 1800$ K, $\log~g = 5$ ; dash-dotted blue: $T_{\rm eff}=1300$ K, $\log~g = 3$ ; dashed green: $T_{\rm eff} = 1800$ K, $\log~g = 3$ .
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.8cm,clip]{8220Fig8a.eps} \incl... ...8220Fig8c.eps} \includegraphics[width=8.8cm,clip]{8220Fig8d.eps} } \end{figure}$ Figure 8: Grain size distribution function f(a,z) [cm^-4] for a number of selected cloud altitudes. The broad distributions on the lhs of all plots correspond to high altitudes. In the left upper figure, the deeper distributions are very close to a $\delta$ -function and not presentable anymore.
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In the text

$\begin{figure} \mbox{\includegraphics[angle=-90,width=7cm,angle=180]{8220Fig9g.p... ...ps} \includegraphics[angle=-90,width=7cm,angle=180]{8220Fig9c.ps} } \end{figure}$ Figure 9: Left column: $T_{\rm eff} = 1800$ K, $\log~g = 5$ ; middle column: $T_{\rm eff}=1300$ K, $\log~g = 5$ ; right column: $T_{\rm eff}=1300$ K, $\log~g = 3$ . 1st row: transmission spectra $F_\lambda~(T[z_0(\lambda)]) ~/B_\lambda(T_{\rm bb})$ . 2nd and 3rd row: local temperature $T[z_0(\lambda )]$ and pressure $p[z_0(\lambda )]$ , respectively, where optical depth reaches unity. 9.7 $\mu$ m is the Si-O stretching mode of (SiO₂[s], silicates), 16-19 $\mu$ m the bending mode.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{8220Fig2a.eps}\par\includegraphics[width=8.8cm,clip]{8220Fig2b.eps}\end{figure}$	Figure 2: Volume fractions $V_{\rm s}/V_{\rm tot}$ ( top) and mass fractions $M_{\rm s}/M_{\rm tot}$ ( bottom) of the various solid compounds for the model depicted in Fig. 1. The temperature scale follows the atmospheric stratification, being cool at the top and hot at the bottom.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{8220Fig3a.eps}\\ \includegraphics[width=8.8cm,clip]{8220Fig3b.eps}\end{figure}$	Figure 3: Volume fractions $V_{\rm s}/V_{\rm tot}$ for different $T_{\rm eff}$ ( top) and different $\log~g$ ( bottom). Only the more abundant solid compounds are viewed, in contrast to Fig. 2.
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$\begin{figure} \par\includegraphics[width=8.8cm]{8220Fig6.eps}\end{figure}$	Figure 6: Element abundances in dust $\epsilon _{\rm d}$ (thick solid) and in the gas phase $\epsilon _{\rm i}$ (dashed). The solar values $\epsilon _{\rm i, Sun}$ (thin solid) and the linear dust-to-gas ratio $\rho _{\rm d}/\rho _{\rm gas}$ ( lowest panel) are shown for comparison. The stellar parameters are $T_{\rm eff} = 1800$ K and $\log~g = 5$ as in Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{8220Fig7.eps}\end{figure}$	Figure 7: Element abundances involved in the dust formation process for two effective temperatures and two different gravities. Dotted blue: $T_{\rm eff}=1300$ K, $\log~g = 5$ ; solid green: $T_{\rm eff} = 1800$ K, $\log~g = 5$ ; dash-dotted blue: $T_{\rm eff}=1300$ K, $\log~g = 3$ ; dashed green: $T_{\rm eff} = 1800$ K, $\log~g = 3$ .
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$\begin{figure} \par\mbox{\includegraphics[width=8.8cm,clip]{8220Fig8a.eps} \incl... ...8220Fig8c.eps} \includegraphics[width=8.8cm,clip]{8220Fig8d.eps} } \end{figure}$	Figure 8: Grain size distribution function f(a,z) [cm^-4] for a number of selected cloud altitudes. The broad distributions on the lhs of all plots correspond to high altitudes. In the left upper figure, the deeper distributions are very close to a $\delta$ -function and not presentable anymore.
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