\begin{table}%t2
      \caption{Manifolds.
         \label{TabManifolds}}
     $$
         %\centerline
{\begin{tabular}{lrrr}
            \hline\hline
            \noalign{\smallskip}
            Orb. param. ($a, T$)& (1, 225)     & (5.2, 123)   & (30, 51.1) \\
            \noalign{\smallskip}
            \hline
%            \noalign{\smallskip}
%            {\ddag}Orb. dist./[AU]& 1         & 5.2       & 30 \\
%            \noalign{\smallskip}
%            $\varrho_{\rm {neb}}^{\rm{MMSN}}{\rm /[kg/m^3]}$
%            & $5.7 \; 10^{-6}$    & $1.4 \; 10^{-8}$    & $1.2 \; 10^{-10}$\\
%            \noalign{\smallskip}
%            $T_{\rm {neb}}/\rm{[K]}$ & 225 & 123 & 51.1 \\
            \noalign{\smallskip}
            $M_{\rm {core,crit}}^{\rm {MMSN}}/[M_{\oplus}]$ & 0.1524 & 0.0948 & 0.0335 \\
            $M_{\rm {env}}^{\rm{max}}/[M_{\oplus}]$ & 21 & 96 & 380 \\
            \noalign{\smallskip}
            \hline
         \end{tabular}}
    $$
\par
    \smallskip
  The critical core mass increases for smaller orbital distances because of (in order of importance):
        the higher gas temperature (cf. Sects.~\ref{SectTemp} and~\ref{SectT-M}), the smaller Hill sphere
        (cf. Sect.~\ref{SectOrbDist}), and the higher densities of the reference nebulae
        (taken from the minimum mass solar nebula models of Kusaka  \cite{kusaka}; and Hayashi \cite{hayashi}).
    \end{table}