\begin{table}%t1
\caption {\label{t:reso}Location of the mean motion resonances within the circumprimary disk 
up to order~10.}
%\centerline
 {\begin{tabular}{ccc}
\hline 
\hline
                  $i$   &    $j$   &     $a$ (AU)\\
\hline
                  3   &     1   &     12.89\\
                  10  &     3   &     12.01\\
                  7   &     2   &     11.63\\
                  4   &     1   &     10.64\\
                  9   &     2   &      9.84\\
                  5   &     1   &      9.17\\
                  6   &     1   &      8.12\\
                  7   &     1   &      7.32\\
                  8   &     1   &      6.70\\
                  9   &     1   &      6.19\\
\hline 
\end{tabular} }
\par
\smallskip
 The critical argument is of the type $i \lambda_{\rm c} - 
j \lambda_{\rm g} - n \varpi_{\rm c} -m \varpi_{\rm g}$ where $\lambda_{\rm c}$ is the true
anomaly of the companion star and $\lambda_{\rm g}$ that of the gas while 
$\varpi_{\rm g}$ is the perihelion longitude of the gas. $\varpi_{\rm c}$ is 
the perihelion longitude of the star which is constant in our simulations. \vspace{-3mm}
\end{table}