All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{0901fig1.ps} \end{figure}$ Figure 1: A grid of lines at constant $T_{\rm eff}$ and constant $\log g~$ in the theoretical [m₁], [c₁] plane.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0901fig2.ps} \end{figure}$ Figure 2: Theoretical grids in the [m₁],[c₁] plane, compared with the empirical loops of three stars with period shorter than 10 d.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0901fig3.ps} \par\end{figure}$ Figure 3: The same as in Fig. 2 but for three Cepheids with period longer than 15 d.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{0901fig4.ps} \par\end{figure}$ Figure 4: $\log T_{\rm eff}$ as a function of [m₁], [c₁] obtained by a 4th degree polynomial fit of theoretical data (crosses) by C97a,b.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{0901fig5.ps} \end{figure}$ Figure 5: The same as in Fig. 4 but for $\log g$ .
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.8cm,clip]{0901fig6.ps} \end{figure}$ Figure 6: BC as a function of $\log T_{\rm e}$ , $\log g$ obtained by a 4 th degree polynomial fit of theoretical data (crosses) by C97a,b.
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In the text

$\begin{figure} \par\includegraphics[clip,width=6cm,clip]{0901fig7.ps} \end{figure}$ Figure 7: Variations along a full pulsation cycle of magnitude, color and radial velocity for models with $M = 9~M_{\odot}$ and $T_{\rm eff} = 4500$ K ( left) and $M = 7~M_{\odot}$ and $T_{\rm eff} = 5300$ K ( right).
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In the text

$\begin{figure} \par\includegraphics[clip,width=3.5cm]{0901fig8.ps} \end{figure}$ Figure 8: Ratio between "computed'' and "theoretical'' radii as a function of the logarithmic period. The bottom panel displays the radius evaluation based on the revised CORS method, while the top one the radius evaluations based on the pure BW method.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0901fig9.ps} \end{figure}$ Figure 9: Light, color and radial velocity curves for the model (Mod. 4) with $M=6.25~ M_{\odot}$ and $T_{\rm eff}=5100~\rm K.$ The left panels show the pure model curves; the middle and right ones the modified curves in the case of good and fair data respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0901fi10.ps} \end{figure}$ Figure 10: Ratio between "computed'' and "theoretical'' radii as a function of the logarithmic period. In the left panels a) the radius is computed using modified curves that simulate good quality, adopting either the revised CORS method ( bottom) or the pure BW one ( top). In the right panels b) similar plots are shown for radii computed from modified curves that simulate fair quality data.
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In the text

$\begin{figure} \par\includegraphics[clip,width=5.5cm,clip]{0901fi11.ps} \end{figure}$ Figure 11: Ratio between the "computed'' and "theoretical'' radii as a function of the shift $\Delta \phi$ for the model (mod. 2) with M= 5 $M_{\odot }$ , $T_{\rm eff}=5600 ~\rm K$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0901fi12.ps} \end{figure}$ Figure 12: Comparison of radii obtained in this work ( $R_{\rm with \Delta B}$ , $R_{\rm no \Delta B}$ ) with those derived by other authors (Arellano Ferro & Rosenzweing (2000) $R_{\rm AFR}$ ; Ripepi et al. (1997) $R_{\rm RBMR}$ ; Moffett & Barnes (1987) $R_{\rm BM}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0901fi13.ps} \par\end{figure}$ Figure 13: Top: Period-Radius relation obtained in the case without $\Delta B$ ; Bottom: as before, but with $\Delta B$ . Open circle: Binary stars; Triangles: first overtone pulsators; Crosses: stars with loop in the [m₁], [c₁] plane not completely within the theoretical grids (see Sect. 3).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0901fi14.ps} \par\end{figure}$ Figure 14: The same of Fig. 13 but excluding first overtone and binary stars.
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In the text

$\begin{figure} \par\includegraphics[clip,width=7.2cm]{0901fi15.ps} \end{figure}$ Figure 15: Top panel: empirical light curve (dots) for the star Y Oph, compared with the best fit model (solid lines, see text for details). Bottom panel: the same but for the radial velocity curve.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0901fig1.ps} \end{figure}$	Figure 1: A grid of lines at constant $T_{\rm eff}$ and constant $\log g~$ in the theoretical [m₁], [c₁] plane.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0901fig2.ps} \end{figure}$	Figure 2: Theoretical grids in the [m₁],[c₁] plane, compared with the empirical loops of three stars with period shorter than 10 d.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0901fig3.ps} \par\end{figure}$	Figure 3: The same as in Fig. 2 but for three Cepheids with period longer than 15 d.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{0901fig4.ps} \par\end{figure}$	Figure 4: $\log T_{\rm eff}$ as a function of [m₁], [c₁] obtained by a 4th degree polynomial fit of theoretical data (crosses) by C97a,b.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{0901fig5.ps} \end{figure}$	Figure 5: The same as in Fig. 4 but for $\log g$ .
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$\begin{figure} \par\includegraphics[angle=270,width=6.8cm,clip]{0901fig6.ps} \end{figure}$	Figure 6: BC as a function of $\log T_{\rm e}$ , $\log g$ obtained by a 4 th degree polynomial fit of theoretical data (crosses) by C97a,b.
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$\begin{figure} \par\includegraphics[clip,width=6cm,clip]{0901fig7.ps} \end{figure}$	Figure 7: Variations along a full pulsation cycle of magnitude, color and radial velocity for models with $M = 9~M_{\odot}$ and $T_{\rm eff} = 4500$ K ( left) and $M = 7~M_{\odot}$ and $T_{\rm eff} = 5300$ K ( right).
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$\begin{figure} \par\includegraphics[clip,width=3.5cm]{0901fig8.ps} \end{figure}$	Figure 8: Ratio between "computed'' and "theoretical'' radii as a function of the logarithmic period. The bottom panel displays the radius evaluation based on the revised CORS method, while the top one the radius evaluations based on the pure BW method.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{0901fig9.ps} \end{figure}$	Figure 9: Light, color and radial velocity curves for the model (Mod. 4) with $M=6.25~ M_{\odot}$ and $T_{\rm eff}=5100~\rm K.$ The left panels show the pure model curves; the middle and right ones the modified curves in the case of good and fair data respectively.
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$\begin{figure} \par\includegraphics[clip,width=5.5cm,clip]{0901fi11.ps} \end{figure}$	Figure 11: Ratio between the "computed'' and "theoretical'' radii as a function of the shift $\Delta \phi$ for the model (mod. 2) with M= 5 $M_{\odot }$ , $T_{\rm eff}=5600 ~\rm K$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0901fi12.ps} \end{figure}$	Figure 12: Comparison of radii obtained in this work ( $R_{\rm with \Delta B}$ , $R_{\rm no \Delta B}$ ) with those derived by other authors (Arellano Ferro & Rosenzweing (2000) $R_{\rm AFR}$ ; Ripepi et al. (1997) $R_{\rm RBMR}$ ; Moffett & Barnes (1987) $R_{\rm BM}$ ).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0901fi13.ps} \par\end{figure}$	Figure 13: Top: Period-Radius relation obtained in the case without $\Delta B$ ; Bottom: as before, but with $\Delta B$ . Open circle: Binary stars; Triangles: first overtone pulsators; Crosses: stars with loop in the [m₁], [c₁] plane not completely within the theoretical grids (see Sect. 3).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0901fi14.ps} \par\end{figure}$	Figure 14: The same of Fig. 13 but excluding first overtone and binary stars.
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$\begin{figure} \par\includegraphics[clip,width=7.2cm]{0901fi15.ps} \end{figure}$	Figure 15: Top panel: empirical light curve (dots) for the star Y Oph, compared with the best fit model (solid lines, see text for details). Bottom panel: the same but for the radial velocity curve.
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