\begin{table}%t2
\caption{Typical dust volume composition $V_{\rm s}/V_{\rm tot}$, mass composition $M_{\rm s}/M_{\rm tot}$, and mean particles sizes $\langle a\rangle~[\mu$m] as a function of local temperature for models as depicted in  Fig.~\ref{fig:VOLMASSFRAC}.
($\nearrow$) -- increasing in $T$-interval; ($\searrow$) -- decreasing in $T$-interval.}\label{tab:chemcomp}
\small
%\centerline
{  \begin{tabular}{rlll}
\hline \hline
\noalign{\smallskip}
$T$ & \multicolumn{1}{c}{$V_{\rm s}/V_{\rm tot}$}  & \multicolumn{1}{c}{$M_{\rm s}/M_{\rm tot}$} & $\langle a\rangle$\\
$\rm[K]$ &  &  & $\rm[\mu$m] \\
\hline\noalign{\smallskip}
700  &  24\% MgSiO$_3$, 20\% Mg$_2$SiO$_4$ & 1. MgSiO$_3$  & $10^{-3}$ \\
. & 12\% SiO$_2$, 10\% SiO,  9\% FeS  & 2. Mg$_2$SiO$_4$ & .\\
.    &  \{MgO, FeO, Fe$_2$O$_3$\} $<$9\%  & 3. FeS, Fe$_2$O$_3$, FeO &.\\
.    &  \{Fe,  Al$_2$O$_3$\}$<$5\% & 4. SiO$_2$, MgO, Fe &.\\
950  &  \{TiO$_2$, CaTiO$_3$\} $<$1\%  &5. SiO  &$10^{-2}$\\
%\hline 
950  & \multicolumn{2}{c}{\ } &$10^{-2}$\\
.    & \multicolumn{2}{c}{strongly changing} & .\\
1200 &  \multicolumn{2}{c}{\ } &$10^{-0.5}$\\
%\hline
1200 &  35\% Mg$_2$SiO$_4$, 23\% SiO$_2$ &  1. Fe & $10^{-0.5} $\\
.    &  $<$20\% MgSiO$_3$ ($\searrow$)&  2. Mg$_2$SiO$_4$& .\\
. & 15\% Fe, 5\% MgO  &  3. SiO$_2$/MgSiO$_3$ &  .\\
1700 &  everything else $<$5\%   &  4. MgO &  10\\
%\hline
1700 & \multicolumn{2}{c}{\ }  &  10 \\
.    & \multicolumn{2}{c}{strongly changing}    &  . \\
1900 & \multicolumn{2}{c}{(SiO, MgO peaking but low \%)}  & $10^2$ \\
%\hline
1900 &  72\% Fe ($\searrow$)  &  1. Fe &  $10^2$ \\
.    &   20\% Al$_2$O$_3$ ($\nearrow$), $<$5\% TiO$_2$ & 2. Al$_2$O$_3$ ($\nearrow$) & $(\star)$ \\
2100 &  10\% CaTiO$_3$ (at 2100~K) &  3. CaTiO$_3$   &  0\\
\hline
\end{tabular}}
\medskip
$(\star)$ Mean grain sizes $\langle a\rangle$ can reach up to $10^{3.5}$ in lower gravity atmospheres like giant-gas planets  (compare Fig.~\ref{J*aquer}).    
\end{table}