All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,height=10.2cm,clip]{1495fig1.eps} \end{figure}$ Figure 1: Feature trends with variations in gravity and temperature. The asterisk indicates the adopted pair $T_{\rm eff}$ - log g for subsequent element abundance analysis. The Balmer line loci were obtained by fitting the observed lines with the Kurucz's (1993) models. The uncertainty in log g for a given temperature attained in this process is indicated by the error bar in the top panel.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=8.2cm,clip]{1495fig2.eps} \end{figure}$ Figure 2: Agreement between the synthesized and observed spectrum for carbon lines. The best fit is obtained for 7.35.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,height=8.3cm,clip]{1495fig3.eps} \end{figure}$ Figure 3: H $\gamma$ profile of HD 137569. The models correspond to $T_{\rm eff}$ 12 000 K and gravities 1.5, 2.0, 2.5 and 3.0. The best fit is obtained for log g = 2.0.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,height=11cm,clip]{1495fig4.eps} \end{figure}$ Figure 4: The agreement between the synthesized and observed spectrum for spectral regions containing C, N and O lines for HD 137569.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=8.2cm,clip]{1495fig5.eps} \end{figure}$ Figure 5: Elemental abundance plotted as a function of condensation temperature. Filled symbols represent relatively cool stars and open symbols represent hotter stars. Triangles represent PNe stars following the same convention. The post-AGB stars are shown as circles. Filled squares are the values for HD 137569 for which the depletion due to condensation is quite evident.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=8.3cm,clip]{1495fig6.eps} \end{figure}$ Figure 6: H $\alpha$ and H $_\beta$ variations in HD 172324.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,height=10.2cm,clip]{1495fig1.eps} \end{figure}$	Figure 1: Feature trends with variations in gravity and temperature. The asterisk indicates the adopted pair $T_{\rm eff}$ - log g for subsequent element abundance analysis. The Balmer line loci were obtained by fitting the observed lines with the Kurucz's (1993) models. The uncertainty in log g for a given temperature attained in this process is indicated by the error bar in the top panel.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,height=8.2cm,clip]{1495fig2.eps} \end{figure}$	Figure 2: Agreement between the synthesized and observed spectrum for carbon lines. The best fit is obtained for 7.35.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,height=8.3cm,clip]{1495fig3.eps} \end{figure}$	Figure 3: H $\gamma$ profile of HD 137569. The models correspond to $T_{\rm eff}$ 12 000 K and gravities 1.5, 2.0, 2.5 and 3.0. The best fit is obtained for log g = 2.0.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=17cm,height=11cm,clip]{1495fig4.eps} \end{figure}$	Figure 4: The agreement between the synthesized and observed spectrum for spectral regions containing C, N and O lines for HD 137569.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,height=8.2cm,clip]{1495fig5.eps} \end{figure}$	Figure 5: Elemental abundance plotted as a function of condensation temperature. Filled symbols represent relatively cool stars and open symbols represent hotter stars. Triangles represent PNe stars following the same convention. The post-AGB stars are shown as circles. Filled squares are the values for HD 137569 for which the depletion due to condensation is quite evident.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,height=8.3cm,clip]{1495fig6.eps} \end{figure}$	Figure 6: H $\alpha$ and H $_\beta$ variations in HD 172324.
Open with DEXTER