\begin{table}%t5
\caption {Best parameters of the RT~models, shown in Figs.~\ref{fig:90}--\ref{fig:61}. The dust shell was confined to end at a radius of
  $10^4~R_{\rm i}$.
\label{tab:50}}
%\centerline
 {\begin{tabular}{cccccc} 
\hline\hline    
\noalign{\smallskip}   
$T_*$$^a$  & $T_{\rm dust}$$^b$ & Comp. & $\tau_{8.0, 9.8, 13.~\mu {\rm m}}$ & 
$R_{\rm i}$$^c$  & $L_{*,~{\rm bol}}$$^d$ \\
 $[$kK$]$ & $[$kK$]$ & & & $[$AU/mas/$R_{i/*}]$ &$[ L_\odot ]$ \\
\hline
\noalign{\smallskip}
3 & 1.2 & amC$^e$  & 0.8, 0.6, 0.4 & 35/5/10  & 
 $5\times 10^4$\\
3 & 1.2 & Sil$^f$  & 1, 6, 1.7     & 40/5/10 & 
 $5\times 10^4$\\
25 & 1.2 & amC$^e$ & 0.8, 0.6, 0.4 & 60/8/1000  & $5\times 10^4$\\
25 & 1.2 & Sil$^f$ & 0.8, 4.9, 1.3 & 115/15/2000& $5\times 10^4$\\
\hline             
\end{tabular}}
\par
\smallskip
$^a$~$T_*$ denotes the   stellar effective temperature.
$^b$~{$T_{\rm dust}$ is the dust temperature
  at the sublimation zone, visible as ring of radius $R_{\rm i}$ in Fig.~\ref{fig:61}.}
  $^c$~{$R_{\rm i/*}$ is the size ratio of the stellar and dust sublimation radius $R_{\rm i}$.}
  $^d$~{$L_{*,~{\rm bol}}$ labels the bolometric luminosity of the embedded star.}
  $^e$~{\label{foot:10}100\% amorphous Carbon grains
 \citep{1988ioch.rept...22H}.}
 $^f$~{\label{foot:11}100\% warm amorphous silicate grains
 \citep{1992AetA...261..567O}}.
\par
\end{table}