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$\begin{figure} \par\includegraphics[width=8.8cm,height=8cm,clip]{fig1.eps} \end{figure}$ Figure 1: Percent differences between the photometric distances for the individual components of detached eclipsing binaries. Note the position of EK Cep. The data are taken from Ribas et al. (1998).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig2.eps} \end{figure}$ Figure 2: Theoretical standard models for EK Cep (without rotation). The upper panel shows the radius of the models as a function of the age (continuous line represents the primary and dashed line denotes the secondary). The middle panel shows the effective temperature ratio TR. The bottom panel presents the apsidal-motion constants for EK Cep. Note that there is an acceptable agreement between radii and TR for a same isochrone (vertical lines). The horizontal lines represent the error bars.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,height=8cm,clip]{fig3.ps} \end{figure}$ Figure 3: Apsidal-motion constant k₂ as a function of time for a 1.12 $M_{\odot }$ model. The model was followed from the PMS stage up to the giant branch. Continuous line represents k₂ as computed by integrating Radau differential equation while dashed one denotes calculations performed with Kopal approach. During the PMS phase, the differences can reach more than 0.20 dex.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig4.eps} \end{figure}$ Figure 4: The same as for Fig. 2 but taking into account solid rotation.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig5.eps} \end{figure}$ Figure 5: The same as for Fig. 2 but taking into account rotation with local conservation of the angular momentum.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,height=8cm,clip]{fig1.eps} \end{figure}$	Figure 1: Percent differences between the photometric distances for the individual components of detached eclipsing binaries. Note the position of EK Cep. The data are taken from Ribas et al. (1998).
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$\begin{figure} \par\includegraphics[width=8.8cm,height=8cm,clip]{fig3.ps} \end{figure}$	Figure 3: Apsidal-motion constant k₂ as a function of time for a 1.12 $M_{\odot }$ model. The model was followed from the PMS stage up to the giant branch. Continuous line represents k₂ as computed by integrating Radau differential equation while dashed one denotes calculations performed with Kopal approach. During the PMS phase, the differences can reach more than 0.20 dex.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig4.eps} \end{figure}$	Figure 4: The same as for Fig. 2 but taking into account solid rotation.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{fig5.eps} \end{figure}$	Figure 5: The same as for Fig. 2 but taking into account rotation with local conservation of the angular momentum.
Open with DEXTER