\begin{table}%t3
\caption{Simultaneous MORO solution of the $UBV$ light curves of
the eclipsing system IU~Aur; for comparison, a previous solution
is also presented in the third column.}
\label{SOLUTION}
\renewcommand{\arraystretch}{0.80}
%\centerline
 {
\begin{tabular}{lcc}
\hline\hline
\noalign{\smallskip}
Parameter             & this paper                 & DHLM             \\[1mm]
\hline\noalign{\smallskip}
\multicolumn{3}{l}{Fixed parameters}                                 \\[1mm]
\hline\noalign{\smallskip}
$A_1 = A_2$$^{a}$
                                   & 1.0           & 1.0                   \\
$g_1 = g_2$$^{b}$
                                   & 1.0           & 1.0                   \\
$x_1~( U)$$\ ^c$
                      &  0.342         & 0.20                  \\
$x_1~(B)\ ^{c}$	&  0.337         & 0.25	 \\
$x_1~(V)\ ^{c}$	&  0.303         & 0.20	 \\
$x_2~(U)\ ^{c}$	&  0.353         & 0.30	 \\
$x_2~(B)\ ^{c}$	&  0.352         & 0.35	 \\
$x_2~(V)\ ^{c}$	&  0.313         & 0.30             \\[1mm]
$T_1$~(K)                          & 32~000       & 32~000          \\[1mm]
\hline\noalign{\smallskip}
\multicolumn{3}{l}{Adjusted parameters}                              \\[1mm]
\hline\noalign{\smallskip}
$i$                   & $83\fdg7 \pm 0\fdg8$       & $90\fdg0 \pm 0\fdg3$  \\
                      & (epoch 1998.0)             & (epoch 1984.4)        \\
$q~(=M_2/M_1)$        & $0.672   \pm 0.017$        & 0.691                 \\
$T_2$~(K)             & $27~540 \pm 290$          & 28~220               \\
$\Omega_1$            & $3.366   \pm 0.032$        & 3.502                 \\
$\Omega_2$            & $3.186   \pm 0.037$        & 3.212            \\[1mm]
$L_1~(U)$$^{d}$
                      & $0.625  \pm 0.007$         & 0.587                 \\
$L_1~(B)^{~d}$   & $0.617  \pm 0.008$         & 0.580	           \\
$L_1~(V)^{~d}$   & $0.610  \pm 0.007$         & 0.574	           \\
$l_3~(U)^{e}$
                  & $19.8$\% $\pm 1.8$\%     & 16.9\%	       \\
$l_3~(B)^{~e}$   & $24.3$\% $\pm 1.6$\%     & 20.8\%	       \\
$l_3~(V)^{~e}$   & $24.0$\% $\pm 1.7$\%     & 21.1\%	  \\[1mm]
$\delta_1$$^{f}$
                      & $0.010 \pm 0.004$          &  0.012                \\
$\delta_2^{\;~f}$
                      & $0.002 \pm 0.002$          &  0.001           \\ 
\hline 
   \noalign{\smallskip}
\multicolumn{3}{l}{Roche radii~$^{g}$}\\
\hline
\noalign{\smallskip}
\noalign{\smallskip}
$r_1~({\rm pole})$  & $0.362 \pm 0.006$          & 0.348                 \\
$r_1~({\rm side})$  & $0.378 \pm 0.009$          & 0.362                 \\
$r_1~({\rm back})$  & $0.398 \pm 0.009$          & 0.379                 \\
$r_1~({\rm point})$ & $0.423 \pm 0.008$          & 0.396            \\[1mm]
$r_2~({\rm pole})$  & $0.324 \pm 0.003$          & 0.327                 \\
$r_2~({\rm side})$  & $0.339 \pm 0.004$          & 0.343                 \\
$r_2~({\rm back})$  & $0.371 \pm 0.005$          & 0.376                 \\
$r_2~({\rm point})$ & $0.425 \pm 0.014$          & 0.435            \\[1mm]
\hline\noalign{\smallskip}
$1\sigma$ deviation   & 0.0074                     & 0.0039           \\[1mm]
\hline
\end{tabular}}
\smallskip
$^a$~{Bolometric albedo.}\\
$^b$~{Gravitational darkening exponent.}\\
$^c$~{Linear limb darkening coefficient; theoretical
values taken from\protect  D\'\i az-Cordov\'{e}s et~al. (\cite{diaz}).}\\
$^d$~{Relative luminosities $L_i/(L_1 + L_2)$; $L_2$ is not
independently adjusted, but recomputed from $r_2$ and $T_2$.}\\
$^e$~{Fraction of third light at maximum.}\\
$^f$~{Radiation pressure parameter, see Drechsel et~al.
                    (\cite{drechsel95}).}\\
$^g$~{Fractional Roche radii in units of
                                         separation of mass centers.}
\end{table}