$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4142F1.eps} \end{figure}$ Figure 1: SOLA coefficients c_nl as a function of mode turning point. Modes for l=1, 2, 3 and 4 are identified by crosses, asterisks, circles, and squares respectively. Coefficients for the higher values of l are indicated by points.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4142F2.eps} \end{figure}$ Figure 2: Evolutionary tracks in a theoretical HR diagram $(T_{\rm eff}, \log L/L_\odot)$ for stellar models of $0.85~M_\odot, 1.0~M_\odot, 1.5~M_\odot, 2.0~M_\odot, 3.0~M_\odot, 4.0~M_\odot$ . The tracks are plotted from ZAMS up to the ages indicated, roughly corresponding to the total main sequence life time.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4142F3.eps} \end{figure}$ Figure 3: The scaled moment of inertia $I_{\rm M}$ normalised to the solar value $I_{\rm M,\odot }$ versus the mean stellar density in solar units, for the stellar models of Fig. 2. For all models the mean density and $I_{\rm M}$ decrease as a function of time while on the main sequence.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4142F1.eps} \end{figure}$	Figure 1: SOLA coefficients c_nl as a function of mode turning point. Modes for l=1, 2, 3 and 4 are identified by crosses, asterisks, circles, and squares respectively. Coefficients for the higher values of l are indicated by points.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4142F2.eps} \end{figure}$	Figure 2: Evolutionary tracks in a theoretical HR diagram $(T_{\rm eff}, \log L/L_\odot)$ for stellar models of $0.85~M_\odot, 1.0~M_\odot, 1.5~M_\odot, 2.0~M_\odot, 3.0~M_\odot, 4.0~M_\odot$ . The tracks are plotted from ZAMS up to the ages indicated, roughly corresponding to the total main sequence life time.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4142F3.eps} \end{figure}$	Figure 3: The scaled moment of inertia $I_{\rm M}$ normalised to the solar value $I_{\rm M,\odot }$ versus the mean stellar density in solar units, for the stellar models of Fig. 2. For all models the mean density and $I_{\rm M}$ decrease as a function of time while on the main sequence.
Open with DEXTER