All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h4306F1.eps}} \end{figure}$ Figure 1: Observed amplitude ratios with Johnson photometry for the three observed frequencies (error bars) and theoretical predictions for $0~\le~\ell~\le~4$ (lines), for a model with $M = 9.7 ~ M_{\odot}$ , Z = 0.02, $\log T_{\rm eff}=4.344$ and $\alpha _{\rm ov}=0$ .
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{h4306F2.eps}} \end{figure}$ Figure 2: Evolutionary tracks of stars with masses around 9.5 $M_{\odot }$ , with X=0.70 and for different values of the metallicity Z and the overshooting parameter $\alpha _{\rm ov}$ . The full lines and the dashed line are obtained with models without overshooting, the dotted lines represent evolutionary tracks obtained with $\alpha _{\rm ov}=0.2$ . The error box corresponds to the values for $T_{\rm eff}$ and $\log~g$ given at the end of Sect. 2. The crosses and the dots represent models which present an exact fit for the frequency of the radial fundamental mode p₁. The black dot corresponds to the model which gives exact fits for the frequencies of the two identified modes $\ell _1=0, m_1=0$ and $\ell _2=2, m_2=0$ , for a 9.6 $M_{\odot }$ star and $\alpha _{\rm ov}=0$ . This model corresponds to Z=0.0183.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{h4306F3.eps}} \end{figure}$ Figure 3: Positions, in the HR diagram, of the models which fit both the radial fundamental mode p₁ (l₁=0, m₁=0) and the second frequency corresponding to the g₁ (l₂=2, m₂=0) mode.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{h4306F4.eps}} \end{figure}$ Figure 4: Relation between the stellar mass (in units of $M_{\odot }$ ) and the metallicity obtained by imposing exact fits for the frequencies of the two identified oscillation modes.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{h4306F5.eps}} \end{figure}$ Figure 5: Rotation velocity obtained for models which fit exactly the two identified modes. The observational constraint $v_{\rm rot} \in [35,135]$ km s^-1 (see Paper II) is shown as thicker lines.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{h4306F6.eps}} \end{figure}$ Figure 6: Allowed domain for the stellar parameters M and Z for the star EN Lac, for X=0.70 and for values of $\alpha _{\rm ov}$ between 0 and 0.2. The thick lines represent the results obtained for $\alpha _{\rm ov}=0$ and 0.2, assuming that $m_3=\pm 1$ . The black dots represent the results obtained assuming that m₃=0. The dotted lines represent the constraints on the metallicity obtained through the photometric mode identification (see Sect. 3), $Z\in [0.015;0.020]$ .
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h4306F7.eps}} \end{figure}$ Figure 7: Evolution of the frequencies as a function of age (Myear) for models with $M = 9.79 ~ M_{\odot}$ , Z = 0.02193 and $\alpha _{\rm ov}=0$ . The three horizontal lines correspond to the three observed frequencies of EN Lac. The vertical line corresponds to the model giving the best fit between the theoretical and observed frequencies. The full lines correspond to the unstable modes and the "+'' to the stable modes.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{h4306F1.eps}} \end{figure}$	Figure 1: Observed amplitude ratios with Johnson photometry for the three observed frequencies (error bars) and theoretical predictions for $0~\le~\ell~\le~4$ (lines), for a model with $M = 9.7 ~ M_{\odot}$ , Z = 0.02, $\log T_{\rm eff}=4.344$ and $\alpha _{\rm ov}=0$ .
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$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{h4306F3.eps}} \end{figure}$	Figure 3: Positions, in the HR diagram, of the models which fit both the radial fundamental mode p₁ (l₁=0, m₁=0) and the second frequency corresponding to the g₁ (l₂=2, m₂=0) mode.
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$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{h4306F4.eps}} \end{figure}$	Figure 4: Relation between the stellar mass (in units of $M_{\odot }$ ) and the metallicity obtained by imposing exact fits for the frequencies of the two identified oscillation modes.
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$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{h4306F5.eps}} \end{figure}$	Figure 5: Rotation velocity obtained for models which fit exactly the two identified modes. The observational constraint $v_{\rm rot} \in [35,135]$ km s^-1 (see Paper II) is shown as thicker lines.
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