All Figures

$\begin{figure} \par\includegraphics[angle=270,width=8.2cm,clip]{1653fig1.eps}\\ \end{figure}$ Figure 1: A comparison of the 3990-4050 Å regions for the nitrogen rich stars B 32 and B 04 in NGC 330, the nitrogen normal star AV304, and the Be star B 12. We indicate the presence of the He I lines at 4009 and 4026 Å, together with the N II lines at 3995, 4041 and 4043 Å. Note that the extraordinary sharpness of the lines in AV304 permits the secure identification on the N II line at 3995 Å while the high S/N ratio of the data for B12 permits a tentative detection of this same line, which is significantly weaker than in the other NGC 330 stars B 04 and B 32.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1653fig2.ps} \end{figure}$ Figure 2: The fractional contribution, x, of the disk relative to the stellar continuum which is required for metal lines in B 12 to have the same abundance as in the comparison star AV 304. These calculations have been performed for the $T_{\rm eff}$ = 23 000, log g = 3.60 model from Table 2.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=5.9cm,clip]{1653fig3l.eps}\hs... ...*{2mm} \includegraphics[angle=90,width=5.6cm,clip]{1653fig3r.eps} \end{figure}$ Figure 3: H $\delta$ lines with the zero, 25% and 35% continuum disk contribution and the fits by theoretical profiles modelled with the atmospheric parameters corresponding to the low $T_{\rm eff}$ case as presented in Table 2. Parameters for the 35% model are $T_{\rm eff}$ = 22 750 K and log g = 3.95.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1653fig4.eps} \end{figure}$ Figure 4: Comparison of N II 3995 Å region of the spectra of the Be star B 17 with the nitrogen rich B-type star B 32 (smooth line), the latter having been convolved with a rotational broadening fuction of 140 km s^-1. Note that the nitrogen line in question is clearly absent in B 17.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1653fig2.ps} \end{figure}$	Figure 2: The fractional contribution, x, of the disk relative to the stellar continuum which is required for metal lines in B 12 to have the same abundance as in the comparison star AV 304. These calculations have been performed for the $T_{\rm eff}$ = 23 000, log g = 3.60 model from Table 2.
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$\begin{figure} \par\includegraphics[angle=90,width=5.9cm,clip]{1653fig3l.eps}\hs... ...*{2mm} \includegraphics[angle=90,width=5.6cm,clip]{1653fig3r.eps} \end{figure}$	Figure 3: H $\delta$ lines with the zero, 25% and 35% continuum disk contribution and the fits by theoretical profiles modelled with the atmospheric parameters corresponding to the low $T_{\rm eff}$ case as presented in Table 2. Parameters for the 35% model are $T_{\rm eff}$ = 22 750 K and log g = 3.95.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1653fig4.eps} \end{figure}$	Figure 4: Comparison of N II 3995 Å region of the spectra of the Be star B 17 with the nitrogen rich B-type star B 32 (smooth line), the latter having been convolved with a rotational broadening fuction of 140 km s^-1. Note that the nitrogen line in question is clearly absent in B 17.
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