\begin{table}%t2    
\par
   \caption{\label{Tab_ICMEs}Summary of results on MCs and ICMEs.  } 
       %\centerline
 {\begin{tabular}{@{}cllllc@{}}    
\hline\hline
Quantity$^{{a}}$ & Object & $D$ range$^{{b}}$ & \multicolumn{1}{c}{$c$}$^{{c}}$ & \multicolumn{1}{c}{$e$} &  Ref.$^{{d}}$\\   
\hline
$d$& model &$ 0.3,~2    $&$               $&$ ~~~ 1             $& ~~\ref{Chen96} \\ 
$d$& model &$ 0.3,~5    $&$               $&$ ~~~ 0.88          $& \ref{Chen96} \\ 
$d$& model &$ 2,~5   $&$               $&$ ~~~ 0.71          $& \ref{Chen96} \\ 
$d$& model &$           $&$               $&$ ~~~ 1             $& \ref{Kumar96} \\ 
$d$& MC    &$ 0.3,~4.   $&$ 0.3           $&$ ~~~ 0.97          $& \ref{Kumar96} \\ 
$S$& MC    &$ 0.3,~4.2  $&$ 0.24 \pm 0.01 $&$ ~~~ 0.78 \pm 0.10 $& \ref{Bothmer98} \\ 
$d$& MC    &$ 0.3,~1    $&$ 0.23 \pm 0.05 $&$ ~~~ 1.14 \pm 0.44 $& \ref{Leitner07} \\ 
$d$& MC    &$ 0.3,~7    $&$ 0.20 \pm 0.02 $&$ ~~~ 0.61 \pm 0.09 $& \ref{Leitner07} \\ 
$S$& ICME  &$ 0.3,~5.4  $&$ 0.25 \pm 0.01 $&$ ~~~ 0.92 \pm 0.07 $& \ref{Liu06} \\ 
$S$& ICME  &$ 0.3,~5.4  $&$ 0.19          $&$ ~~~ 0.61          $& \ref{Wang05} \\ 
$d$& model &$ 0.3,~3    $&$ 0.2           $&$ ~~~ 0.64 \pm 0.05 $& \ref{present} \\ 
\hline
$\Bc    $& model &$          $&$             $&$ -2             $& \ref{Kumar96} \\ 
$\Bc    $& MC    &$ 0.3,~4.  $&$   18        $&$ -1.8           $& \ref{Kumar96} \\ 
$\Bc    $& MC    &$ 0.3,~1   $&$   18 \pm 4  $&$ -1.64 \pm 0.40 $& \ref{Leitner07} \\ 
$\Bc    $& MC    &$ 0.3,~7   $&$   19 \pm 1  $&$ -1.30 \pm 0.09 $& \ref{Leitner07} \\ 
$\bar{B}$& ICME  &$ 0.3,~5.4 $&$~~ 7 \pm 0.4 $&$ -1.40 \pm 0.08 $& \ref{Liu06} \\ 
$\bar{B}$& ICME  &$ 0.3,~5.4 $&$~~ 8.3       $&$ -1.52          $& \ref{Wang05} \\ 
$\Bc    $& model &$ 0.3,~3   $&$   20        $&$ -1.60 \pm 0.10 $& \ref{present} \\ 
\hline
    \end{tabular}}
\par
    \smallskip
\par
$^{{a}}$ The physical quantities studied are:  the diameter of the flux rope $d$, the size, $S$ (estimated along the spacecraft trajectory), the central field strength $\Bc$ (estimated from a fitted magnetic model to the data for MCs), and the average field strength, $\bar{B}$, along the spacecraft trajectory.
 $^{{b}}$  The range of solar distance, $D$, is in AU.  
 $^{{c}}$  The data are fitted with a power law $c (D/\Do )^e$ with $\Do=1~\rm AU$.  $c$ is in AU for the diameter/size and in nT for the magnetic field strength. $e$ is dimensionless.  
 $^{{d}}$   The results are from:
\refstepcounter{ref} \label{Chen96}         \ref{Chen96}: \citet{Chen96},
\refstepcounter{ref} \label{Kumar96}        \ref{Kumar96}: \citet{Kumar96},
\refstepcounter{ref} \label{Bothmer98}      \ref{Bothmer98}: \citet{Bothmer98},
\refstepcounter{ref} \label{Leitner07}      \ref{Leitner07}: \citet{Leitner07},
\refstepcounter{ref} \label{Liu06}          \ref{Liu06}: \citet{Liu06},
\refstepcounter{ref} \label{Wang05}         \ref{Wang05}: \citet{Wang05},
\refstepcounter{ref} \label{present}        \ref{present}: present work.
 The comparison of consecutive lines with the same reference indicate the variation of the results ($c,e$) with the range of $D$ selected or the difference between a model and observations.
   \end{table}