All Tables

Table 1: Observational diary: the data sources, number of points in each curve, passband (effective central wavelength in nm), time interval in Julian date minus 2 400 000, and year of observation. Vienna V and B refer to the light curves obtained at Vienna Observatory, the Cereda B and V curves are by Cereda et al. (1988), $H_{{\rm p}}$ refers to the Hipparcos $H_{{\rm p}}$ -band data centered $\approx$ 500 nm and the Tycho BV data described and analyzed by ZW03, DAO indicates the Lu (1993) radial velocity curves, and Asiago stands for the Asiago Observatory radial velocities from the Ca triplet region (ZW03).
Table 2: Photoelectric minima observed at the Leopold-Figl-Observatory with $\rm O{-}C$ residuals (in days) computed from the linear ephemeris (1).
Table 3: The logarithmic limb darkening coefficients used in the final stages of modeling for the various passbands, including the square passband centered on the calcium triplet region that was used for the radial velocity curves.
Table 4: Radial velocity parameters without and with proximity and eclipse effects: Orbital semi-major axis, a, systemic velocity, $\protect\gamma$ and q. Note that the q's differ by about $4.7\%$ while the a's and $\protect\gamma$ 's are almost the same, within their uncertainties.
Table 5: Parameters and standard errors for the base light curve solution obtained by a simultaneous fit. B is polar surface brightness, f₁ and f₂ are the fill-out factors $f_{i}:=\frac{\Omega ^{{\rm I}}-\Omega _{i}}{\Omega ^{{\rm I}}-\Omega ^{{\rm O}}}$ , with $\Omega ^{{\rm I}% }$ and $\Omega ^{{\rm O}}$ the Roche potentials of the inner and outer critical surfaces. S and V denote surface area and volume and <tex2html_comment_mark> k=R₂/R₁ is the ratio of the mean radii. a is the semimajor axis in solar radii, and $\protect\gamma$ is the systemic velocity in km s^-1.
Table 6: Solutions with standard errors. The last four rows give the standard deviations of the observed points from the solution curves that were used in curve-dependent weighting. The reference epoch, HJD₀, is given minus 2 440 000. The simultaneous fit column is the base for adding spots. The uncertainty specified for T₁ is based on personal judgment. The standard errors derived for T₂ were much smaller than the uncertainties assumed for T₁; therefore we added them to the uncertainties of T₁. All other uncertainties are standard errors.
Table 7: Spot parameters for the Cereda and Vienna light curves: co-latitudes $\protect\theta_1$ and $\protect\theta_2$ of spots on star 1 and star 2, spot longitudes $\protect\lambda_1$ and $\protect\lambda_2$ , spot angular radii $\protect\rho_1$ and $\protect\rho_2$ , and dimensionless temperature factors $T^{\rm F}_1$ and $T^{\rm F}_2$ . Angles are in radians. There are two spots on each star for Cereda BV while Vienna BV has two spots on star 1 and no spots on star 2. The second column has the standard deviation of the fit; $\protect\sigma = 1000 \protect\sigma_{{\rm fit}}$ . In addition to the spot parameters those in the third column also were adjusted. We included i because it effects the amplitudes of light curves.
Table 8: Absolute parameters for V781 Tau. All uncertainties are standard errors except for the temperatures as explained in the caption to Table 6. J is the orbital angular momentum in units of 10⁵² g cm² s^-1and j is the angular momentum per unit of reduced mass in units of 10¹⁸ cm² s^-1. Star 1 is eclipsed at primary minimum (phase 0 $.\!\!^{\scriptscriptstyle\rm p}$ 0).
Table 9: Properties of V781 Tau compared to those of CN And and outlier stars of Fig. 5. CN And data are from Van Hamme et al. (2001). Data for the latter, except for J and j, were taken from Maceroni & Van't Veer (1996) and updated, and numbered, as per Maceroni's website compilation.