\begin{table}%t1
\caption {\label{table:comp1}Results   of  the  formation   of  a   Jupiter-like  planet,
  where the accreted planetesimals have a radius of 100~km${^{a}}$. }
%\centerline
 {\begin{tabular}{p{1.1cm} p{1.2cm} p{1.3cm} p{1.2cm} p{1.3cm}}
\hline\hline
Disc density & \multicolumn{2}{p{2cm}}{Previous results} &  
\multicolumn{2}{p{2cm}}{New results}\\
\cline{2-5}
 [MMSN] & Cross- over time [My] & Cross- over mass [${M_{\oplus}}$] & Cross- over 
 time [My] & Cross- over mass [${M_{\oplus}}$]\\
\hline
$\; \; 6$   & 11.40  &  $\; \; 44.70$  & 7.20  & $\; \;25.50$ \\
$\; \; 7$   & $\; \; 8.75$  & $\; \; 55.40$  & 5.58    & $\; \; 27.90$ \\
$\; \; 8$   & $\; \; 7.00$  & $\; \; 66.60$  & 4.60    & $\; \; 29.30$ \\
$\; \; 9$   & $\; \; 5.70$  & $\; \; 77.60$  & 3.78  & $\; \;30.90$ \\
10  & $\; \; 4.80$  & $\; \; 88.50$  & 3.20 & $\; \;31.90$ \\
\hline 
\end{tabular}}
\par
\smallskip
$^{{a}}$ The first column  indicates the disc density  in terms of  the MMSN, the second and third columns show the results corresponding to Paper~I, and the last  two columns  list the  updated  results for  exactly the  same conditions  but with  the corrected  interpolation formulae  for the SCVH's EOS  for a  mixture of hydrogen  and helium.
\end{table}