All Figures

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4980fig1a.eps}\par\vspace*... ...par\vspace*{2mm} \includegraphics[width=7.4cm,clip]{4980fig1c.eps} \end{figure}$ Figure 1: From top to bottom: phase diagram of $\langle v^1\rangle$ for f₁ = 3.9793 c d^-1, for f₂ = 3.9995 c d^-1 after prewhitening with f₁ and for f₃ = 4.1832 c d^-1 after prewhitening with f₁ and f₂.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{4980fig2.eps} \end{figure}$ Figure 2: Amplitude and phase distributions for $f_1 = 3.9793~\ensuremath{{\rm c~d}^{-1}}$ , $f_2 = 3.9995~\ensuremath{{\rm c~d}^{-1}}$ , and $f_3 = 4.1832~\ensuremath{{\rm c~d}^{-1}}$ for the Si III 4553 Å line. The amplitudes are expressed in continuum units and the phases in $\pi$ radians.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{4980fig3.eps} \end{figure}$ Figure 3: The theoretical amplitude distribution for f₁ computed from the line profile time series generated for the best parameter combinations derived with the moment method.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4980fig4.eps} \end{figure}$ Figure 4: Histogram for the equatorial rotational velocity of the star.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4980fig5.eps} \end{figure}$ Figure 5: The variation of the frequency of $\ell =0$ and $\ell =2$ modes of a $13~\ensuremath{M_\odot}$ stellar model with evolution (characterised by the central hydrogen abundance, $\ensuremath {X_{\rm c}}$ ). The dotted lines indicate the $\ell =0$ modes, while the dashed lines show the $\ell =2$ modes. Each mode is labelled by its degree and radial order ( $\ell , n$ ). The horizontal solid line and the shaded strip show the observed radial mode (f₂) and the splitting-corrected $\ell =2$ mode ( $f_1 - \delta \nu _{\rm s}$ ), respectively. The vertical dot-dashed line shows a possible solution where the theoretical frequencies match the respective observed frequencies.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{ \includegraphics[width=5.5cm,clip]{4980fig6a.eps} \hsp... ...hspace*{4mm} \includegraphics[width=5.5cm,clip]{4980fig6c.eps} }\end{figure}$ Figure 6: The variation of the model frequencies with three stellar parameters - M, $\ensuremath {d_{\rm ov}}$ and Z₀. In each panel, two of the parameters are fixed to clearly bring out the effect of the remaining parameter on the frequencies. The $\ell =0,n=2$ frequencies are plotted as abcissae, while the $\ell =2,n=-1$ frequency, corrected for rotational splitting, are plotted as ordinates. The dashed lines indicate the two observed frequencies. The point where the two dashed lines intersect indicates the perfect match of the desired model. Each shaded band represents an evolutionary track. The width of the band along the y-axis indicates the uncertainty due to rotational splitting. A full-colour version of this figure is available in the online edition.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4980fig7.eps} \end{figure}$ Figure 7: Similar to Fig. 6, except that multiple parameters are varied at a time to obtain a good match between the theoretical frequencies and the observed ones. Selected models with limiting values of overshoot and metallicity are shown only. A full-colour version of this figure is available in the online edition.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4980fig1a.eps}\par\vspace... ...par\vspace{2mm} \includegraphics[width=7.4cm,clip]{4980fig1c.eps} \end{figure}$	Figure 1: From top to bottom: phase diagram of $\langle v^1\rangle$ for f₁ = 3.9793 c d^-1, for f₂ = 3.9995 c d^-1 after prewhitening with f₁ and for f₃ = 4.1832 c d^-1 after prewhitening with f₁ and f₂.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16cm,clip]{4980fig2.eps} \end{figure}$	Figure 2: Amplitude and phase distributions for $f_1 = 3.9793~\ensuremath{{\rm c~d}^{-1}}$ , $f_2 = 3.9995~\ensuremath{{\rm c~d}^{-1}}$ , and $f_3 = 4.1832~\ensuremath{{\rm c~d}^{-1}}$ for the Si III 4553 Å line. The amplitudes are expressed in continuum units and the phases in $\pi$ radians.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{4980fig3.eps} \end{figure}$	Figure 3: The theoretical amplitude distribution for f₁ computed from the line profile time series generated for the best parameter combinations derived with the moment method.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4980fig4.eps} \end{figure}$	Figure 4: Histogram for the equatorial rotational velocity of the star.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4980fig7.eps} \end{figure}$	Figure 7: Similar to Fig. 6, except that multiple parameters are varied at a time to obtain a good match between the theoretical frequencies and the observed ones. Selected models with limiting values of overshoot and metallicity are shown only. A full-colour version of this figure is available in the online edition.
Open with DEXTER