All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{figures/8075fig1.eps}\end{figure}$ Figure 1: Frequency differences $\Delta_m = \frac{\omega_{n,\ell,~m} - \omega_{n,\ell,~m-2\cdot{\rm sg}(m)}}{2}$ as a function of the radial order n for the N=3 polytropic models. The frequencies have been scaled by $\Omega _{\star }$ . For high radial orders, these differences converge to a limit which does not depend on $\ell$ or m.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{figures/8075fig2.eps}\end{figure}$ Figure 2: The large frequency separation $\Delta _n$ as a function of the rotation rate $\Omega$ . $\Delta _n$ has been scaled with different quantities so as to show which other stellar quantity best matches this frequency separation. As can be seen, $\Delta _n$ is roughly proportional to the square root of the mean density of the star.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{figures/8075fig3.eps}\end{figure}$ Figure 3: Comparison between frequencies based on Eq. (1) and complete eigenmode calculations, both of which are given in an inertial frame. $\ell$ and m are indicated on the figure, and the radial orders are n=1to 10. This figure contains four columns subdivided into two, the left part corresponding to Eq. (1) and the right part to complete calculations. The oblique dotted lines in between show the correspondence between the two sets of frequencies. The units are the same as in Fig. 5 of Reese et al. (2006), which allows direct comparison. As can be seen from comparing these figures, Eq. (1) gives a much better description of the frequency spectrum than a $3{\rm rd}$ order perturbative formula.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{figures/8075fig1.eps}\end{figure}$	Figure 1: Frequency differences $\Delta_m = \frac{\omega_{n,\ell,~m} - \omega_{n,\ell,~m-2\cdot{\rm sg}(m)}}{2}$ as a function of the radial order n for the N=3 polytropic models. The frequencies have been scaled by $\Omega _{\star }$ . For high radial orders, these differences converge to a limit which does not depend on $\ell$ or m.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{figures/8075fig2.eps}\end{figure}$	Figure 2: The large frequency separation $\Delta _n$ as a function of the rotation rate $\Omega$ . $\Delta _n$ has been scaled with different quantities so as to show which other stellar quantity best matches this frequency separation. As can be seen, $\Delta _n$ is roughly proportional to the square root of the mean density of the star.
Open with DEXTER