All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{fig1.ps} \end{figure}$ Figure 1: Top panel: $\nu ^* d_{01}, \nu ^* d_{10}$ ; middle panel: $\nu ^* dd_{01}, \nu ^* dd_{10}$ , bottom panel: $\nu ^* d_{02}$ , for solar model A. $\nu ^*=\nu$ in units of 2500 $\mu$ Hz.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{fig2.ps} \end{figure}$ Figure 2: Variation of small separations $\nu ^* dd_{01}, \nu ^* dd_{10}$ with $\nu$ for frequencies obtained by the BiSON, IRIS and GOLF experiments. All data sets show the same periodicity and the same phase.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{fig3.ps} \end{figure}$ Figure 3: Residuals to a low order fit; a) $\nu ^* d_{01}, \nu ^* d_{10}$ , b) $\nu ^* dd_{01}, \nu ^* dd_{10}$ .
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{fig4.ps} \end{figure}$ Figure 4: Power spectra of the residuals: a) $\nu ^* d_{01}, \nu ^* d_{10}$ , b) $\nu ^* dd_{01}, \nu ^* dd_{10}$ .
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{fig5.ps} \end{figure}$ Figure 5: Phase shifts $\delta _0, \delta _1$ and $\alpha _0,\alpha _1$ for model A: a) variation with acoustic radius for $\nu=2500~\mu$ Hz. $\alpha _0,\alpha _1$ cannot be separated in these figures; b) variation with frequency for x_f= 0.9, t_f/T=0.615; c) variation of $\nu ^*(\delta _1-\delta _0)$ and $\alpha _1-\alpha _0$ with frequency.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{fig6.ps} \end{figure}$ Figure 6: a) $\alpha -\delta$ as determined from the frequencies and Eigen-frequency Eq. (14) with $\Delta_0=136~\mu$ Hz. b) Phase shift difference $\nu ^*(\delta _1-\delta _0)$ determined from the eigenfrequencies by interpolation (points), the model values (continuous periodic line), the mean variation (smooth line). c) Power spectra of residuals to mean variation - the smaller maximum is that obtained using the points determined from the frequencies.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{fig7.ps} \end{figure}$ Figure 7: Acoustic potentials at base of the convective zone: $U_0/\omega _0^2$ (solid lines), $\omega ^2Q/\omega _0^3$ (dashed lines), and $U_2/\omega _0^2$ (fine dotted lines), at a frequencies $\nu=1000, 2500, 4000~\mu$ Hz.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{fig8.ps} \end{figure}$ Figure 8: Power spectrum (Ampliude²) of simple model Eq. (28). The modulation period corresponding to the base of the convective zone is $\nu_0=352~\mu$ Hz but the maximum power is shifted to $359~\mu$ Hz due to the frequency dependency of the phase shifts $\delta _0, \delta _1$ and of the amplitudes of the two components.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{fig9.ps} \end{figure}$ Figure 9: $\nu ^*(\delta _1-\delta _0)$ derived from the frequencies as described in Sect. 6 for a) model A, b) a BiSON data set, c) IRIS data set, d) GOLF data set. All data sets were analysed using frequencies in the range 1400-3500 $\mu$ Hz. Bottom panel: power spectra of residuals to a low order fit as in Eq. (4). The modulation period at the peak of the power spectra are as listed. There is good agreement between the values derived from solar data and that of the model.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{fig1.ps} \end{figure}$	Figure 1: Top panel: $\nu ^* d_{01}, \nu ^* d_{10}$ ; middle panel: $\nu ^* dd_{01}, \nu ^* dd_{10}$ , bottom panel: $\nu ^* d_{02}$ , for solar model A. $\nu ^*=\nu$ in units of 2500 $\mu$ Hz.
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$\begin{figure} \par\includegraphics[width=8.35cm,clip]{fig2.ps} \end{figure}$	Figure 2: Variation of small separations $\nu ^* dd_{01}, \nu ^* dd_{10}$ with $\nu$ for frequencies obtained by the BiSON, IRIS and GOLF experiments. All data sets show the same periodicity and the same phase.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{fig3.ps} \end{figure}$	Figure 3: Residuals to a low order fit; a) $\nu ^* d_{01}, \nu ^* d_{10}$ , b) $\nu ^* dd_{01}, \nu ^* dd_{10}$ .
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$\begin{figure} \par\includegraphics[width=9cm,clip]{fig4.ps} \end{figure}$	Figure 4: Power spectra of the residuals: a) $\nu ^* d_{01}, \nu ^* d_{10}$ , b) $\nu ^* dd_{01}, \nu ^* dd_{10}$ .
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$\begin{figure} \par\includegraphics[width=9cm,clip]{fig5.ps} \end{figure}$	Figure 5: Phase shifts $\delta _0, \delta _1$ and $\alpha _0,\alpha _1$ for model A: a) variation with acoustic radius for $\nu=2500~\mu$ Hz. $\alpha _0,\alpha _1$ cannot be separated in these figures; b) variation with frequency for x_f= 0.9, t_f/T=0.615; c) variation of $\nu ^*(\delta _1-\delta _0)$ and $\alpha _1-\alpha _0$ with frequency.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{fig7.ps} \end{figure}$	Figure 7: Acoustic potentials at base of the convective zone: $U_0/\omega _0^2$ (solid lines), $\omega ^2Q/\omega _0^3$ (dashed lines), and $U_2/\omega _0^2$ (fine dotted lines), at a frequencies $\nu=1000, 2500, 4000~\mu$ Hz.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{fig8.ps} \end{figure}$	Figure 8: Power spectrum (Ampliude²) of simple model Eq. (28). The modulation period corresponding to the base of the convective zone is $\nu_0=352~\mu$ Hz but the maximum power is shifted to $359~\mu$ Hz due to the frequency dependency of the phase shifts $\delta _0, \delta _1$ and of the amplitudes of the two components.
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