$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig1.eps} \end{figure}$ Figure 1: The theoretical HR diagram. The numbers below the tracks indicate the stellar masses in solar units.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig2.eps} \end{figure}$ Figure 2: The evolution of the apsidal-motion constant k₂ for 5 and 40 $M_{\odot }$ models. The numbers on the tracks indicate the initial masses (in solar units). The solid lines represent the present calculations, while the dashed ones represent the models of 1995.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=8.8cm,clip]{fig3.eps} \end{figure}$ Figure 3: The depth of the convective envelope (normalized radius) as a function of the effective temperature for a 1.41 $M_{\odot }$ model.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=8.8cm,clip]{fig4.eps} \end{figure}$ Figure 4: The constant E characterizing a polytropic envelope (Eq. (5)) as a function of the effective temperature. Same models as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=8.8cm,clip]{fig5.eps} \end{figure}$ Figure 5: The behavior of the tidal torque constant E₂ as a function of the logarithm of the age. The models shown are for 2 and 10 $M_{\odot }$ .
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=8.8cm,clip]{fig6.eps} \end{figure}$ Figure 6: The product $\alpha _{\rm P}\beta$ as a function of the logarithm of the age for models of 1, 20 and 125 $M_{\odot }$ . The asterisks indicated the end of hydrogen burning.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=8.8cm,clip]{fig7.eps} \end{figure}$ Figure 7: The evolution of the gravity-darkening exponent $\beta _1$ as a function of the effective temperature for a 10 $M_{\odot }$ model. Note how $\beta _1$ decreases/increases during the loops in the HR diagram.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig1.eps} \end{figure}$	Figure 1: The theoretical HR diagram. The numbers below the tracks indicate the stellar masses in solar units.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig2.eps} \end{figure}$	Figure 2: The evolution of the apsidal-motion constant k₂ for 5 and 40 $M_{\odot }$ models. The numbers on the tracks indicate the initial masses (in solar units). The solid lines represent the present calculations, while the dashed ones represent the models of 1995.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=8cm,width=8.8cm,clip]{fig3.eps} \end{figure}$	Figure 3: The depth of the convective envelope (normalized radius) as a function of the effective temperature for a 1.41 $M_{\odot }$ model.
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$\begin{figure} \par\includegraphics[height=8cm,width=8.8cm,clip]{fig4.eps} \end{figure}$	Figure 4: The constant E characterizing a polytropic envelope (Eq. (5)) as a function of the effective temperature. Same models as in Fig. 3.
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$\begin{figure} \par\includegraphics[height=8cm,width=8.8cm,clip]{fig5.eps} \end{figure}$	Figure 5: The behavior of the tidal torque constant E₂ as a function of the logarithm of the age. The models shown are for 2 and 10 $M_{\odot }$ .
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$\begin{figure} \par\includegraphics[height=8cm,width=8.8cm,clip]{fig6.eps} \end{figure}$	Figure 6: The product $\alpha _{\rm P}\beta$ as a function of the logarithm of the age for models of 1, 20 and 125 $M_{\odot }$ . The asterisks indicated the end of hydrogen burning.
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$\begin{figure} \par\includegraphics[height=8cm,width=8.8cm,clip]{fig7.eps} \end{figure}$	Figure 7: The evolution of the gravity-darkening exponent $\beta _1$ as a function of the effective temperature for a 10 $M_{\odot }$ model. Note how $\beta _1$ decreases/increases during the loops in the HR diagram.
Open with DEXTER