\begin{table}%t1
\caption{\label{table:model_parameters}Model parameters for $\zeta$ Tau.}
%\centerline
 {\small \begin{tabular}{llll}  
 \hline\hline       
Parameter & Value & Type & Ref.$^a$  \\
\hline
\multicolumn{4}{c}{Stellar parameters}\\ 
\hline
Spectral Type & B1IVe shell & fixed & 2, 3 \\
$R_{\rm p}$ & $5.9~R_{\sun}$  & fixed & 2, 4 \\
$R_{\rm e}$ & $7.7~R_{\sun}$  & fixed$^b$ & 1 \\
$T_{\rm p}$ & $25~000~\rm K$  & fixed &  2 \\
$T_{\rm e}$ & $17~950~\rm K$  & fixed$^c$ &  1 \\
$V/V_{\rm crit}$ & $0.8$& fixed  &5 \\ 
$V_{\rm crit}$ & $530~\rm km~s^{-1}$ & free & 1 \\
$M$ & $11.3~M_{\sun}$  & fixed$^d$ & 1 \\
$L $ & $7400~L_{\sun}$ & fixed & 1 \\
$T_{\rm eff}$ & $19~370~\rm K$  & fixed$^e$ &   1 \\
\hline
\multicolumn{4}{c}{Disk parameters}\\ 
$\Sigma_0$ & $2.1~\rm g~cm^{-2}$  &  free & 1 \\
$\rho_0$ & $5.9 \times 10^{-11}~\rm g~cm^{-3}$  &  fixed$^g$ & 1 \\
$R_{\rm t}$ &  $130~R_{\sun}$  &  fixed & 1 \\
$H_0$ &  $0.208~R_{\sun}$ & fixed$^f$  & 1 \\
\hline
\multicolumn{4}{c}{$V/R$ parameters}\\
%\hline
 $P$ & 1429 d & Fixed & 2 \\
$T_0$ & 50414 & Fixed & 2 \\
$k_2$ & 0.006 & Free & 1\\ 
Weak line force &  $5.74\times 10^{-2}(\varpi/R_{\rm e})^{0.1}$ & Free & 1\\
$\dot{M}$ &$10^{-11}~M_{\sun}~\rm yr^{-1}$ & Free & 1 \\
$\alpha$  & 0.4 & Free & 1\\
$\delta$  & 0.95 & Free & 1\\
\hline
\multicolumn{4}{c}{Geometrical parameters}\\ 
%\hline
$i$ & $95\degr$ & free & 1 \\
$\gamma$ & $32\degr$ & free & 1 \\
$\phi_0$ & $280\degr$ & free & 1 \\
distance & 126 pc & fixed$^h$ & 6\\
\hline
\multicolumn{4}{c}{Binary parameters}\\ 
%\hline
$P_{\rm orb}$ & 132.97 d  & fixed & 7 \\
$e$ & 0  & fixed & 7 \\
$a$ & $257~R_{\sun}$ & fixed  & 7\\
$q$ & 0.121 & fixed  & 7 \\
\hline
\end{tabular}}
\medskip
$^a$ References: 1)~this work; 2) Paper~I; 3)~\citet{yan90};
4)~\citet{har88}; 5) \citet{cra05}; 6) \citet{per97}; 7)~\citet{har84}; $^b$  $R_{\rm e}$ was calculated from $R_{\rm p}$ and $V/V_{\rm crit}$ for a rigidly rotating star in the Roche approximation; $^c$~the equatorial temperature, $T_{\rm e}$, was calculated from $V/V_{\rm crit}$ and $T_{\rm p}$ for a rigidly rotating star in the Roche approximation; $^d$~$M$ was calculated from $V_{\rm crit}$; $^e$~$T_{\rm eff}$ corresponds to the average effective temperature of a rotationally deformed, gravity darkened star;
$^f$~$H_0$ was calculated from Eq.~(\ref{eq:scaleheight}), 
assuming  a mean molecular weight of 0.6 and an electron temperature of $18~000~\rm K$ after \citet{car06a}; $^g$~$\rho_0$ is given by $\Sigma_0(2\pi)^{-1/2}H_0^{-1}$ (Eq.~(\ref{eq:rho})); $^h$~$d$ was considered a free parameter within the 113--148~pc range, corresponding to the accuracy in the distance determination the Hipparcos satellite.
\end{table}