All Figures

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3270fg01.eps}\par\vspace*{2mm} \includegraphics[width=8.4cm,clip]{3270fg02.eps} \end{figure}$ Figure 1: Residuals from a linear ephemeris versus HJD minus 2 445 000. The basis of this plot are 112 minima from the Kreiner, Kim and Nha database for V781 Tau with 13 Vienna and 5 Yakut et al. minimum times added. The parabola shows the fit to the residuals between the observed times of minima and the linear ephemeris (1). The Vienna minimum times near HJD 2 445 400 are well reproduced by this fit. The residuals with respect to this parabola are also displayed. 7 points with residuals smaller or larger than -0.015, or 0.015, respectively, are not displayed.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3270fg03.ps}\par\vspace*{2mm} \includegraphics[angle=-90,width=8cm,clip]{3270fg04.ps} \end{figure}$ Figure 2: Radial velocities from Lu (1993) and ZW03 and solution curves. The solid and dashed lines are for stars 1 and 2, respectively, with proximity and eclipse effects excluded ( top panel) and included ( bottom panel). The fit is not improved when proximity effects are included. The standard deviation even increased from 13.0 to 14.2 km s^-1 as shown in Table 4. However q is different. We estimate the internal precision of a single measurement to be $\pm$ 5 km s^-1 at quadrature and $\pm$ 10-15 km s^-1near conjunction, based on comparison with other data from the same nights.
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In the text

$\begin{figure} \includegraphics[angle=-90,width=6.0cm]{3270fg05.ps}\includegraph... ...hspace*{1.5mm}% \includegraphics[angle=-90,width=6.0cm]{3270fg10.ps}\end{figure}$ Figure 3: Hp and the Vienna BV light curve fits and data versus phase. The lower panels show the residuals versus phase.
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In the text

$\begin{figure} \mbox{\includegraphics[angle=-90,width=6.0cm]{3270fg11.ps}\includ... ...pace*{1.3mm} \includegraphics[angle=-90,width=6.0cm]{3270fg16.ps} } \end{figure}$ Figure 4: Same as Fig. 3 but for Cereda BV in the left and center columns. The right column shows the fit and residuals when Cereda B was fitted individually with one dark spot on each star.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{3270fg17.eps}\end{figure}$ Figure 5: Intersections of V781 Tau's inner and outer critical equipotentials with the x-y-plane. The middle curve represents the (over-contact) surface. The left star is component 1.
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In the text

$\begin{figure} \par\includegraphics[angle=-00,width=8cm]{3270fg18.eps}\end{figure}$ Figure 6: System angular momentum vs. total mass. A circle marks V781 Tau, $\times$ marks CN And, and Maceroni's identification numbers indicate the following outliers in one or more of the plots: 70 = XY Boo, 79 = AK Her, 80 = AW UMa, 81 = TV Mus, 82 = TY Men, 84 = DK Cyg, 85 = XZ Leo, 86 = OO Aql, 87 = BU Vel, 88 = $\protect\epsilon$ Cra, 89 = AQ Tuc, 90 = RR Cen, 91 = V535 Ara, 92 = S Ant, 93 = RS Col, 94 = MW Pav, 95 = TY Pup, and 96 = UZ Oct. The dynamical and other properties of V781 Tau, CN And, and the outlier group are listed in Table 9 and are mostly taken from Maceroni & Van't Veer (1996).
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In the text

$\begin{figure} \par\includegraphics[angle=-00,width=6cm]{3270fg19.eps}\end{figure}$ Figure 7: Histograms of the frequency distribution of contact parameters (also called "fill out factors'') of over-contact systems, taken from the Maceroni & Van't Veer (1996) compilation, supplemented with newer data from Maceroni's website. The panels are for W-type, A-type, and for both types together. They demonstrate that V781 Tau's f of 0.205 is relatively large for W-type systems but is more consistent with W-type than A-type.
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In the text

$\begin{figure} \includegraphics[angle=-90,width=6.0cm]{3270fg05.ps}\includegraph... ...hspace*{1.5mm}% \includegraphics[angle=-90,width=6.0cm]{3270fg10.ps}\end{figure}$	Figure 3: Hp and the Vienna BV light curve fits and data versus phase. The lower panels show the residuals versus phase.
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$\begin{figure} \mbox{\includegraphics[angle=-90,width=6.0cm]{3270fg11.ps}\includ... ...pace*{1.3mm} \includegraphics[angle=-90,width=6.0cm]{3270fg16.ps} } \end{figure}$	Figure 4: Same as Fig. 3 but for Cereda BV in the left and center columns. The right column shows the fit and residuals when Cereda B was fitted individually with one dark spot on each star.
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$\begin{figure} \par\includegraphics[width=8cm]{3270fg17.eps}\end{figure}$	Figure 5: Intersections of V781 Tau's inner and outer critical equipotentials with the x-y-plane. The middle curve represents the (over-contact) surface. The left star is component 1.
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