All Figures

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{0396fig1.ps} \end{figure}$ Figure 1: Dereddened stellar energy distribution of $\omega ^1$ Sco (dotted line) in comparison with the best-fit model (solid line). The original flux of $\omega ^1$ Sco is also shown (crosses). The IUE data were calibrated by means of the NEWSIPS reduction package. In the inset, there is a closer view of the short-wavelength part of the spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{0396fig2.ps} \end{figure}$ Figure 2: The positions of the field $\beta$ Cep stars ( left panel) and those from the three open clusters ( right panel) on the $\log g$ vs. $\log T_{\rm eff}$ diagram. The evolutionary tracks were calculated without (solid line) and with (dotted line) taking into account the effect of convective core overshooting. We assumed $d_{\rm ov} = 0.2$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0396fig3.ps} \end{figure}$ Figure 3: Differences in parameters, $\Delta p_i = p_i({\rm NEWSIPS}) - p_i({\rm INES})$ , as a function of the effective temperature obtained from the IUE/NEWSIPS data.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0396fig4.ps} \end{figure}$ Figure 4: The same as in Fig. 3, but as a function of the number of IUE spectra, n (IUE).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0396fig5.ps} \end{figure}$ Figure 5: The distribution of the $\beta$ Cephei stars with the [m/H] parameter. The hatched histogram shows the results obtained from the IUE/NEWSIPS data, while the gray one presents results obtained from the IUE/INES data.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0396fig6.ps} \end{figure}$ Figure 6: The distribution of the metallicity parameter of the $\beta$ Cephei stars from the IUE/NEWSIPS data as a function of the galactocentric distance (in kpc). The dashed line indicates the mean value of [m/H] obtained for all $\beta$ Cephei stars. Symbols are the same as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0396fig7.ps} \end{figure}$ Figure 7: The location of the $\beta$ Cephei stars on the $\log g$ vs. $\log T_{\rm eff}$ diagrams. The instability regions for Z = 0.02, 0.015 and 0.01 were taken from Pamyatnykh (1999). In the upper panel the position of the field $\beta$ Cephei stars is shown, while in the lower one, the position of variables from the open clusters is presented.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0396fig8.ps} \end{figure}$ Figure 8: Dependence of pulsational parameters: P, 2K, A_V and A_U-B/A_V on the metallicity parameter, [m/H].
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{0396fig1.ps} \end{figure}$	Figure 1: Dereddened stellar energy distribution of $\omega ^1$ Sco (dotted line) in comparison with the best-fit model (solid line). The original flux of $\omega ^1$ Sco is also shown (crosses). The IUE data were calibrated by means of the NEWSIPS reduction package. In the inset, there is a closer view of the short-wavelength part of the spectrum.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{0396fig2.ps} \end{figure}$	Figure 2: The positions of the field $\beta$ Cep stars ( left panel) and those from the three open clusters ( right panel) on the $\log g$ vs. $\log T_{\rm eff}$ diagram. The evolutionary tracks were calculated without (solid line) and with (dotted line) taking into account the effect of convective core overshooting. We assumed $d_{\rm ov} = 0.2$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0396fig3.ps} \end{figure}$	Figure 3: Differences in parameters, $\Delta p_i = p_i({\rm NEWSIPS}) - p_i({\rm INES})$ , as a function of the effective temperature obtained from the IUE/NEWSIPS data.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0396fig4.ps} \end{figure}$	Figure 4: The same as in Fig. 3, but as a function of the number of IUE spectra, n (IUE).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0396fig5.ps} \end{figure}$	Figure 5: The distribution of the $\beta$ Cephei stars with the [m/H] parameter. The hatched histogram shows the results obtained from the IUE/NEWSIPS data, while the gray one presents results obtained from the IUE/INES data.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0396fig6.ps} \end{figure}$	Figure 6: The distribution of the metallicity parameter of the $\beta$ Cephei stars from the IUE/NEWSIPS data as a function of the galactocentric distance (in kpc). The dashed line indicates the mean value of [m/H] obtained for all $\beta$ Cephei stars. Symbols are the same as in Fig. 2.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0396fig7.ps} \end{figure}$	Figure 7: The location of the $\beta$ Cephei stars on the $\log g$ vs. $\log T_{\rm eff}$ diagrams. The instability regions for Z = 0.02, 0.015 and 0.01 were taken from Pamyatnykh (1999). In the upper panel the position of the field $\beta$ Cephei stars is shown, while in the lower one, the position of variables from the open clusters is presented.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0396fig8.ps} \end{figure}$	Figure 8: Dependence of pulsational parameters: P, 2K, A_V and A_U-B/A_V on the metallicity parameter, [m/H].
Open with DEXTER