\begin{table}%t4
\caption {\label{Tab:4}Results of models of different masses computed with HHeB. }
%\centering
\par
\begin{tabular}{ l  l  l  l  l }\hline\hline
\noalign{\smallskip}
$M/M_\odot$ & $\log_{10}L/L_\odot$ & $\log_{10} p$ &
$\log_{10}|\dot p|$ & $\Delta t$\\ \hline
4.0 & 2.440 & 0.0010 &($+$)0.6165 & 0.0703\\
6.0 & 2.953 & 0.4391 &($+$)0.7586 & 0.0078\\
    & 3.205 & 0.6688 &($-$)0.2638 & 0.1845\\
    & 3.248 & 0.6874 &($+$)0.0298 & 0.1115\\
    & 3.272 & 0.7239 &($-$)0.2278 & 0.0950\\
    & 3.251 & 0.6874 &($+$)0.0895 & 0.1605\\
8.0 & 3.395 & 0.7783 &($+$)1.622  & 0.0035\\
    & 3.674 & 1.055  &($-$)1.186  & 0.0172\\
    & 3.687 & 1.043  &($+$)1.408  & 0.0137\\
    & 3.775 & 1.127  &($-$)1.621  & 0.0085\\  
    & 3.536 & 0.9000 &($+$)1.730  & 0.0031\\   
10.0& 3.733 & 1.051  &($+$)2.232  & 0.0017\\
    & 4.031 & 1.344  &($-$)2.187  & 0.0046\\
    & 3.791 & 1.099  &($+$)2.354  & 0.0011\\ 
 \hline
\end{tabular}
\tablefoot {Columns~2 and~3
respectively provide the logarithms of the mean luminosity and period calculated
by considering independently (1) the first section of the evolutionary track
where the period increases monotonously when crossing the instability strip and
(2) the section where the period decreases and so forth. Column~4 provides the
rate of the period change $\dot p={\rm d}p/{\rm d}t$ 
(in seconds per year) and its sign is denoted by ``+'' or ``--''. Column~5 gives the
duration of the crossings $\Delta t$ (in~Myr).}
\end{table}