\begin{table}
\caption[] {\label{tab:v636cen_age}Ages (Gyr) for the primary ($p$) and secondary ($s$) components
of V636~Cen\ determined from comparison between their masses and radii
and Claret models for different mixing length parameters and abundances. 
}
\centerline {
\begin{tabular}{cccccc}
\hline
\hline\noalign{\smallskip}
     & \feh\ & $l/H_{\rm p}(p)$ & $l/H_{\rm p}(s)$ & Age(p)  & Age(s) \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
1 & --0.20  & 1.40      &  1.00      & $1.33 \pm  0.13$ & $1.37 \pm 0.55$ \\  
2 & --0.20  & 1.50      &  1.10      & $1.82 \pm  0.13$ & $3.10 \pm 0.55$ \\ 
3 & --0.12  & 1.60      &  1.10      & $2.46 \pm  0.12$ & $3.25 \pm 0.53$ \\ 
4 & --0.20  & 1.68      &  1.68      & $2.40 \pm  0.13$ &                 \\ 
\hline
\end{tabular}}

\smallskip
Note:
Ages in Gyr.
Except for those with the solar $l/H_{\rm p} = 1.68$ (case~4), the models fit
the observed effective temperatures within errors. 
See text for details.
\end{table}