All Figures

$\begin{figure} \par\includegraphics[width=6.8cm,height=6.4cm,clip]{6010fig1.ps} \end{figure}$ Figure 1: Radial velocity curve for Cen X-4 (from D'Avanzo et al. 2005) obtained through cross-correlation of absorption lines in the range 5930-6750 Å with late-type template stars. Two phases are shown for clarity. The best sine-wave fit is also shown. Residuals from the best fit are shown in the lower panel.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,height=6.6cm,clip]{6010fig2.ps} \end{figure}$ Figure 2: Simulated radial velocity curves for Cen X-4 for the irradiated (stars) and non irradiated (triangles) case. Differences between the two models are shown in the lower panel.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,height=7cm,clip]{6010fig3.ps} \end{figure}$ Figure 3: Variations of the fractional contribution of the companion compared with synthetic models for $\alpha =0^{\circ }$ (dotted line), 7 $^{\circ }$ (solid line) and 14 $^{\circ }$ (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,height=7.4cm,clip,angle=-90]{6010fig4.ps} \end{figure}$ Figure 4: Velocity of the H ${\alpha }$ emission from the companion at different orbital phases. Two cycles are shown for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,height=7.3cm,clip]{6010fig5.ps} \end{figure}$ Figure 5: Determination of the disc flaring angle in Cen X-4. The solid lines represent the result of our model for the considered mass ratio values ( $q \sim 0.17$ and $q \sim 0.23$ ). The dashed lines represent the value $K_{\rm em}=122.8 \pm 11.8$ km s^-1 measured from or Doppler maps. The possible disc flaring angle range is marked with a solid line.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,height=6.4cm,clip]{6010fig1.ps} \end{figure}$	Figure 1: Radial velocity curve for Cen X-4 (from D'Avanzo et al. 2005) obtained through cross-correlation of absorption lines in the range 5930-6750 Å with late-type template stars. Two phases are shown for clarity. The best sine-wave fit is also shown. Residuals from the best fit are shown in the lower panel.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.9cm,height=6.6cm,clip]{6010fig2.ps} \end{figure}$	Figure 2: Simulated radial velocity curves for Cen X-4 for the irradiated (stars) and non irradiated (triangles) case. Differences between the two models are shown in the lower panel.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.2cm,height=7cm,clip]{6010fig3.ps} \end{figure}$	Figure 3: Variations of the fractional contribution of the companion compared with synthetic models for $\alpha =0^{\circ }$ (dotted line), 7 $^{\circ }$ (solid line) and 14 $^{\circ }$ (dashed line).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,height=7.4cm,clip,angle=-90]{6010fig4.ps} \end{figure}$	Figure 4: Velocity of the H ${\alpha }$ emission from the companion at different orbital phases. Two cycles are shown for clarity.
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$\begin{figure} \par\includegraphics[width=7cm,height=7.3cm,clip]{6010fig5.ps} \end{figure}$	Figure 5: Determination of the disc flaring angle in Cen X-4. The solid lines represent the result of our model for the considered mass ratio values ( $q \sim 0.17$ and $q \sim 0.23$ ). The dashed lines represent the value $K_{\rm em}=122.8 \pm 11.8$ km s^-1 measured from or Doppler maps. The possible disc flaring angle range is marked with a solid line.
Open with DEXTER