Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{1223fig1.eps}\end{figure}$ Figure 1: A randomly chosen set of reduced spectra of ${\lambda }$ Scorpii obtained in July 1997, focussed on the Si III triplet, showing the line-profile variations due to pulsation.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{1223fig2.eps}\end{figure}$ Figure 2: Phase diagrams of the mean RVs with respect to the orbital periods of $P_1 = 5\hbox{$.\!\!^{\rm d}$ }9525$ ( top) and $P_2 = 1082^{\rm d}$ ( bottom). The observed RVs are given by dark-gray dots. The orbital solutions obtained with FOTEL (Table 3) are represented by the black lines. The scattered distribution of the RVs in the upper plot is caused by the contribution of the long orbit. $\phi = 0$ corresponds to the epoch of periastron HJD 2 450 659 and 2 451 732 for the close, respectively wide orbit.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{1223fig3.eps}\end{figure}$ Figure 3: Observed RVs obtained between June 1995 and July 2002 (black dots) together with the best solution of the triple system from FOTEL (dark gray line, see Table 3).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{1223fig4.eps}\end{figure}$ Figure 4: RVs of ${\lambda }$ Scorpii from the 421 spectra taken in July 1997. The combination of the FOTEL triple orbit and the main intrinsic variation with frequency f₁ is shown by the full line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1223fig5.eps}\end{figure}$ Figure 5: HIPPARCOS data folded with the period of the close orbit ( $\phi = 0$ at HJD 2 447 921, epoch of periastron). Near phase 0.1 we see an increase in magnitude, corresponding to a decrease of the amount of observed light, most probably caused by an eclipse.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.75cm,clip]{1223fig6.eps}\end{figure}$ Figure 6: Allowable parameter space in the Hertzsprung-Russell diagram for ${\lambda }$ Scorpii-type primaries in our simulated samples of binaries. The evolutionary tracks are computed using the Single Star Evolution (SSE) code developed by Hurley et al. (2000). The main-sequence life times of the $10~M_\odot$ , $11~M_\odot$ , and $12~M_\odot$ models are approximately 24 Myr, 21 Myr, and 18 Myr, respectively.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{1223fig1.eps}\end{figure}$	Figure 1: A randomly chosen set of reduced spectra of ${\lambda }$ Scorpii obtained in July 1997, focussed on the Si III triplet, showing the line-profile variations due to pulsation.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{1223fig3.eps}\end{figure}$	Figure 3: Observed RVs obtained between June 1995 and July 2002 (black dots) together with the best solution of the triple system from FOTEL (dark gray line, see Table 3).
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{1223fig4.eps}\end{figure}$	Figure 4: RVs of ${\lambda }$ Scorpii from the 421 spectra taken in July 1997. The combination of the FOTEL triple orbit and the main intrinsic variation with frequency f₁ is shown by the full line.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.1cm,clip]{1223fig5.eps}\end{figure}$	Figure 5: HIPPARCOS data folded with the period of the close orbit ( $\phi = 0$ at HJD 2 447 921, epoch of periastron). Near phase 0.1 we see an increase in magnitude, corresponding to a decrease of the amount of observed light, most probably caused by an eclipse.
Open with DEXTER