All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3792fig1.eps} \end{figure}$ Figure 1: KOREL disentangling of the spectrum of the secondary and telluric lines in the region from 6465 to 6529 Å. The corresponding solution 1 is in Table 5.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3792fg2a.eps}\par\includegraphics[width=8.5cm,clip]{3792fg2b.eps} \end{figure}$ Figure 2: A plot of V-band and B-band residuals from the orbital variations vs. RJD for all photometric data. Simultaneous cyclic variations in both bands are clearly present.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3792fg3a.eps}\par\includegraphics[width=8.3cm,clip]{3792fg3b.eps} \end{figure}$ Figure 3: A time plot of V-band residuals from the orbital variations for the Hipparcos data only: Upper panel: all data. Bottom panel: a subset demonstrating the presence of clear variations on a time scale of days.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3792fig4.eps} \end{figure}$ Figure 4: Plot of H $\alpha$ profiles at 21 phases, from different orbital cycles. Note the phase-locked variation of V/R, with V/R<1 in phases 0.3-0.4 and V/R>1 in phases 0.7-0.8. The sharp, narrow absorption lines are due to the secondary star.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3792fig5.eps} \end{figure}$ Figure 5: Orbital RV curve of the H $\alpha$ emission wings.
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In the text

$\begin{figure} \includegraphics[width=11.1cm,clip]{3792fig6.eps} \end{figure}$ Figure 6: Comparison of rectified synthetic system spectrum, for the preliminary model, with a portion of observed spectrum BXN04816. The continuous line at the top is the system spectrum, superposed on the observed spectrum (grey curve). The middle continuous line is the rectified primary star spectrum. This spectrum has been positioned by adding 0.36 to all ordinates. The bottom line is the rectified secondary star synthetic spectrum, positioned by adding 0.25 to all ordinates. Note that the contribution of the secondary star is much too large, so the preliminary model cannot be correct. See the text for details.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3792fig7.eps} \end{figure}$ Figure 7: Fit of theoretical radial velocities ( RVs) to the observed velocities. The filled circles designate mean KOREL disentangled RVs, the open circles designate reliable RVs from paper 17, and the asterisks designate RVs from paper 17 that may be affected by emission lines and are less reliable.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3792fig8.eps} \end{figure}$ Figure 8: Fit of three theoretical light curves to the observed Vlight curve. The solid line is for a secondary star bolometric albedo of 0.70, the dash line is for a bolometric albedo of 0.90, and the dot-dash line is for a bolometric albedo of 0.50.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3792fig9.eps} \end{figure}$ Figure 9: Contributions of the separate stellar components to the V light curve, and the system V light curve. The top curve is the contribution of the secondary star, with 0.95 added to all ordinates. The bottom curve is the contribution of the primary star, with 0.02 added to all ordinates. It is rotating at 6.19 times the synchronous rate. The middle curve is the system V light curve. See the text for details.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3792fg10.eps} \end{figure}$ Figure 10: Fit of the synthetic B light curve to observations.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3792fg11.eps} \end{figure}$ Figure 11: Fit of the synthetic U light curve to observations. Note the change in ordinate range from the two previous light curve plots.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3792fg12.eps} \end{figure}$ Figure 12: View of system model projected on the plane of the sky, at orbital phase 0.25. The secondary star fills its Roche lobe Rotational distortion is easily visible for the primary star. It rotates at 6.19 times synchronous rate. The unit of distance for both axes is the semi-major axis of the relative orbit.
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In the text

$\begin{figure} \par\includegraphics[width=11.3cm,clip]{3792fg13.eps} \end{figure}$ Figure 13: Fit of system model synthetic spectrum (thin line) to observed (grey curve) spectral region including Balmer lines. The synthetic spectrum fit is reasonably good, including the fits to the ${\lambda }3819$ , ${\lambda }4009$ , ${\lambda }4026$ , and ${\lambda }4144$ He I lines.
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In the text

$\begin{figure} \par\includegraphics[width=11.4cm,clip]{3792fg14.eps} \end{figure}$ Figure 14: Fit of rectified synthetic spectrum (thin line, top), for system model, to observed spectrum BXN04816 (grey curve). The primary star spectrum has been positioned by adding 0.10 to all ordinates, and the secondary star spectrum haas been positioned by adding 0.67 to all ordinates. The synthetic spectrum identifications are as in Fig. 6, but note the different ordinate scale. Note the generally accurate fit of the secondary star lines to the observations. The fit demonstrates that the secondary star is rotating synchronously. Also note the smearing of the primary star lines that results from rapid stellar rotation.
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In the text

$\begin{figure} \includegraphics[width=11.4cm,clip]{3792fg15.eps} \end{figure}$ Figure 15: Fit of model synthetic spectrum (thin line, top) to observed (grey curve) spectral region including H $\gamma$ . This spectrum is at orbital phase 0.91. The spectrum of the primary star is in the middle and that of the secondary star is at the bottom. The spectrum of the primary star has been positioned by adding -0.03 to all ordinates, and the spectrum of the secondary has been positioned by adding 0.40 to all ordinates.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{3792fg16.eps} \end{figure}$ Figure 16: View of V360 Lac model at orbital phase 0.44. The orbital inclination is $65^{\circ }$ . The irradiated inner face of the secondary star is turned toward the observer. Note the rotational distortion of the primary star. This view is associated with the spectra in Figs. 17 and 18.
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In the text

$\begin{figure} \par\includegraphics[width=10.6cm,clip]{3792fg17.eps} \end{figure}$ Figure 17: Synthetic spectrum (thin line, top) compared with observed spectrum V3L14818 (grey curve) at orbital phase 0.44 (see Fig. 16). The middle spectrum is the primary star and the bottom spectrum is the secondary star. The primary star spectrum has been positioned by adding -0.11 to all ordinates, and the secondary star spectrum has been positioned by adding 0.37 to all ordinates. Note the decreasing contribution of the primary star and the increasing contribution of the secondary star with wavelength. Also note the H $\alpha$ emission with the central absorption reversal. The absorption component agrees with the wavelength of the primary star H $\alpha$ line, which is slightly displaced from the wavelength of the composite system synthetic spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=10.6cm,clip]{3792fg18.eps} \end{figure}$ Figure 18: Detail of Fig. 17. The Doppler shift of the secondary star spectral lines is clearly evident, since the line identification annotations are positioned at their listed wavelengths. Note the emission wings on the Si II doublet. As with H $\alpha$ , the emission follows the motion of the primary star and indicates the presence of circumstellar matter associated with the primary star. The contribution of the rotationally-broadened primary star absorption lines is small (see Fig. 17). The strong Si II absorption components must be produced by circumstellar matter.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3792fg19.eps} \end{figure}$ Figure 19: View of V360 Lac model at orbital phase 0.50. Compare with Fig. 16. This view is associated with the spectra in Figs. 20 and 21. The primary star is nearer the observer and the observer sees the irradiated inner face of the secondary.
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In the text

$\begin{figure} \includegraphics[width=11cm,clip]{3792fg20.eps} \end{figure}$ Figure 20: Synthetic spectrum (thin line, top) compared with observed spectrum V3L00848 (grey curve) at orbital phase 0.50 (see Fig. 19). Spectra as in Fig. 17. The H $\alpha$ lines of the two stellar components and the central absorption reversal of the observed spectrum align more accurately at this orbital phase. The primary star spectrum has been positioned by adding -0.11 to all ordinates, and the secondary star spectrum has been positiioned by adding 0.37 to all ordinates.
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In the text

$\begin{figure} \includegraphics[width=11cm,clip]{3792fg21.eps} \end{figure}$ Figure 21: Detail of Fig. 20. Note the subtle changes, in both the observed and synthetic spectrum, from Fig. 18. The Si II emission wings are present, as in Fig. 18, but the observed absorption component is deeper and narrower.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3792fg22.eps} \end{figure}$ Figure 22: View of V360 Lac model at orbital phase 0.98. The secondary star is nearer the observer. This view is associated with the spectra in Figs. 23 and 24.
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In the text

$\begin{figure} \par\includegraphics[width=11.6cm,clip]{3792fg23.eps} \end{figure}$ Figure 23: Synthetic spectrum (thin line, top) compared with observed spectrum V3L10685 (grey curve) at orbital phase 0.98 (see Fig. 22). Spectra as in Fig. 17. Note the much greater depth of the H $\alpha$ absorption feature in the observed spectrum than at orbital phase 0.50, Fig. 20. The primary star spectrum has been positioned by adding -0.11 to all ordinates, and the secondary star spectrum has been positioned by adding 0.37 to all ordinates.
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In the text

$\begin{figure} \par\includegraphics[width=11.6cm,clip]{3792fg24.eps} \end{figure}$ Figure 24: Detail of Fig. 23. Note the differences from Fig. 21. The Si II emission wings are still present but the absorption component profiles are different from both Figs. 18 and 21.
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In the text

$\begin{figure} \par\includegraphics[width=11.6cm,clip]{3792fg25.eps} \end{figure}$ Figure 25: Fit of synthetic spectrum (thin line) to IUE spectrum SWP09204 (grey curve). The synthetic spectrum has been divided by $2.5\times 10^{42}$ to superpose it on the IUE spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{3792fg26.eps} \end{figure}$ Figure 26: Location of individual binary components on a main sequence HR diagram, marked by the heavy solid line, with ZAMS stellar masses indicated. The rightmost diamond marks the primary star as affected by rotation. The leftmost diamond marks the location of the primary star if it were rotating synchronously. The rightmost triangle marks the secondary, including irradiation by the rapidly rotating primary star. The leftmost triangle marks the secondary as it would be located if the primary were rotating synchronously. In the latter case the primary star is hotter, because of reduced gravitational darkening, and so irradiative heating of the secondary star is greater. The bolometric magnitudes are as evaluated by an observer for whom the orbital inclination is $65\hbox {$^\circ $ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3792fig1.eps} \end{figure}$	Figure 1: KOREL disentangling of the spectrum of the secondary and telluric lines in the region from 6465 to 6529 Å. The corresponding solution 1 is in Table 5.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3792fg2a.eps}\par\includegraphics[width=8.5cm,clip]{3792fg2b.eps} \end{figure}$	Figure 2: A plot of V-band and B-band residuals from the orbital variations vs. RJD for all photometric data. Simultaneous cyclic variations in both bands are clearly present.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3792fg3a.eps}\par\includegraphics[width=8.3cm,clip]{3792fg3b.eps} \end{figure}$	Figure 3: A time plot of V-band residuals from the orbital variations for the Hipparcos data only: Upper panel: all data. Bottom panel: a subset demonstrating the presence of clear variations on a time scale of days.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3792fig4.eps} \end{figure}$	Figure 4: Plot of H $\alpha$ profiles at 21 phases, from different orbital cycles. Note the phase-locked variation of V/R, with V/R<1 in phases 0.3-0.4 and V/R>1 in phases 0.7-0.8. The sharp, narrow absorption lines are due to the secondary star.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3792fig5.eps} \end{figure}$	Figure 5: Orbital RV curve of the H $\alpha$ emission wings.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3792fig7.eps} \end{figure}$	Figure 7: Fit of theoretical radial velocities ( RVs) to the observed velocities. The filled circles designate mean KOREL disentangled RVs, the open circles designate reliable RVs from paper 17, and the asterisks designate RVs from paper 17 that may be affected by emission lines and are less reliable.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3792fig8.eps} \end{figure}$	Figure 8: Fit of three theoretical light curves to the observed Vlight curve. The solid line is for a secondary star bolometric albedo of 0.70, the dash line is for a bolometric albedo of 0.90, and the dot-dash line is for a bolometric albedo of 0.50.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3792fg10.eps} \end{figure}$	Figure 10: Fit of the synthetic B light curve to observations.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3792fg11.eps} \end{figure}$	Figure 11: Fit of the synthetic U light curve to observations. Note the change in ordinate range from the two previous light curve plots.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3792fg12.eps} \end{figure}$	Figure 12: View of system model projected on the plane of the sky, at orbital phase 0.25. The secondary star fills its Roche lobe Rotational distortion is easily visible for the primary star. It rotates at 6.19 times synchronous rate. The unit of distance for both axes is the semi-major axis of the relative orbit.
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$\begin{figure} \par\includegraphics[width=11.3cm,clip]{3792fg13.eps} \end{figure}$	Figure 13: Fit of system model synthetic spectrum (thin line) to observed (grey curve) spectral region including Balmer lines. The synthetic spectrum fit is reasonably good, including the fits to the ${\lambda }3819$ , ${\lambda }4009$ , ${\lambda }4026$ , and ${\lambda }4144$ He I lines.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{3792fg16.eps} \end{figure}$	Figure 16: View of V360 Lac model at orbital phase 0.44. The orbital inclination is $65^{\circ }$ . The irradiated inner face of the secondary star is turned toward the observer. Note the rotational distortion of the primary star. This view is associated with the spectra in Figs. 17 and 18.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3792fg19.eps} \end{figure}$	Figure 19: View of V360 Lac model at orbital phase 0.50. Compare with Fig. 16. This view is associated with the spectra in Figs. 20 and 21. The primary star is nearer the observer and the observer sees the irradiated inner face of the secondary.
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$\begin{figure} \includegraphics[width=11cm,clip]{3792fg21.eps} \end{figure}$	Figure 21: Detail of Fig. 20. Note the subtle changes, in both the observed and synthetic spectrum, from Fig. 18. The Si II emission wings are present, as in Fig. 18, but the observed absorption component is deeper and narrower.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3792fg22.eps} \end{figure}$	Figure 22: View of V360 Lac model at orbital phase 0.98. The secondary star is nearer the observer. This view is associated with the spectra in Figs. 23 and 24.
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$\begin{figure} \par\includegraphics[width=11.6cm,clip]{3792fg24.eps} \end{figure}$	Figure 24: Detail of Fig. 23. Note the differences from Fig. 21. The Si II emission wings are still present but the absorption component profiles are different from both Figs. 18 and 21.
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$\begin{figure} \par\includegraphics[width=11.6cm,clip]{3792fg25.eps} \end{figure}$	Figure 25: Fit of synthetic spectrum (thin line) to IUE spectrum SWP09204 (grey curve). The synthetic spectrum has been divided by $2.5\times 10^{42}$ to superpose it on the IUE spectrum.
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