\begin{table}%t2
\par
%\centering
\par
\caption{\label{models2}Main features of the two additional WD models computed to investigate
the effects of changing the burning rate (quantities are same as in Table~\ref{models}).} 
\begin{tabular}{ccccc}
\hline \hline
\noalign{\smallskip}
Model & $T_{\rm c}$ [$10^8~{\rm K}$] & $\rho_{\rm c}$
[$10^9~{\rm g\ cm^{-3}}$] & $g$ [$10^9~{\rm cm\ s^{-2}}$] &
$r_{{\rm b}}$ [km]\\
\hline
3.1 & 7.68 & 2.20 & 6.23 & 150\\
3 \tablefootmark{a}   & 7.63 & 2.08 & 5.90 & 154\\
3.2 & 7.59 & 2.00 & 5.20 & 164\\
\hline
\end{tabular}
\tablefoot{\tablefoottext{a}{As for model~3, the stellar evolution code
stalls shortly before the actual criterion for ignition is met, hence
these values result of an extrapolation from about 5\% lower
temperature models. However, we do not expect the extrapolation errors
to change much either the absolute or the relative values of the
numbers presented in this table.}}
\end{table}