All Figures

$\begin{figure} \par\includegraphics[width=8.cm,clip]{0651fig1.eps} \end{figure}$ Figure 1: The synthetic spectrum around the He I line at $\lambda$ 5875.6 Å. Computations were carried out using a model atmosphere with $T_{\rm eff}=10~300$ K. Open circles - the observed spectrum, dashed line - solar abundance, dot-dashed line - -1.0 dex, solid line - -2.0 dex (adopted), and thin solid line - -3.0 dex compared with the solar value.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{0651fig2.eps} \end{figure}$ Figure 2: The synthetic spectrum around the Fe II $\lambda$ 6147 Å and $\lambda$ 6149 Å lines. Open circles represent the observed spectrum, the solid line is for the adopted abundance (log $\epsilon$ (Fe II) = 8.54) with the 4.7 kG magnetic field, $\xi$ _t = 0 km s^-1. An unidentified feature is indicated by a question mark.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{0651fig3.eps} \end{figure}$ Figure 3: The synthetic line profile fitting of the C II lines at $\lambda$ 4267 Å. Open circles - the observed spectrum, dashed line - the solar abundance, and solid line - -0.25 dex compared with the solar value (adopted).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0651fig4.eps} \end{figure}$ Figure 4: The synthetic line profile fittings for the O I $\lambda$ 6156-6158 Å triplet lines. Open circles - the observed spectrum, dashed line - the solar abundance, solid line - the adopted abundance (-0.56 dex), and thin solid line - -1.0 dex compared with the solar value.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0651fig5.eps} \end{figure}$ Figure 5: The synthetic spectrum of the Cl II lines at $\lambda$ 4794.56 Å. Open circles represent the observed spectrum, and solid line indicates the profile for the adopted abundance (7.21).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0651fig6.eps} \end{figure}$ Figure 6: The synthetic spectrum of the Co II lines at $\lambda$ 4915.42 Å. Open circles represent the observed spectrum, and solid line indicates the profile for the adopted abundance (8.50). Unidentified features are indicated by question marks.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0651fig7.eps} \end{figure}$ Figure 7: The synthetic spectrum of the Ba II line at $\lambda$ 4554.03 Å. Open circles - the observed spectrum, dashed line - +1.0 dex, dot-dashed line - +0.5 dex, solid line - solar abundance (adopted), and thin solid line - -1.0 dex compared with the solar value. An unidentified feature is indicated by a question mark.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0651fig8.eps} \end{figure}$ Figure 8: The synthetic spectrum of the Pr III line at $\lambda$ 6160.23 Å. Open circles represent the observed spectrum, and the solid line indicates the profile for the adopted abundance. An unidentified feature is indicated by a question mark.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0651fig9.eps} \end{figure}$ Figure 9: The abundances in logarithmic units for HR 5049 compared with the solar values. Upper limits for three elements are shown by downward arrows.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0651fig10.eps} \end{figure}$ Figure 10: The relation between the Nd-Pr abundance differences and the effective temperature of various CP stars. Small open circles (Hg-Mn stars) and small open triangles (Am stars) are taken from Dolk et al. (2002). The small filled circle (HR 7775, Hg-Mn star) and the small filled triangle (Am star) are taken from Ryabchikova et al. (2001). The small open circle connecting with the small filled circle is for HR 7775, which are taken from Dolk et al. (2002). Small open squares (roAp stars) are taken from Ryabchikova et al. (2001), Cowley et al. (2000), Kochukhov (2003), Gelbmann et al. (2000), and Ryabchikova et al. (2000). Filled diamonds (non-pulsating CP2 stars) are taken from Ryabchikova et al. (2001). The plus sign (HD 187 474, CP2 star) and the open diamond (HR 6958 = HD 170 973, Si star) are taken from Strasser et al. (2001) and Kato (2003), respectively. The St. Andrew's cross is for HR 5049 (this study). All the log gf values of these authors are transformed into our scale. The horizontal broken line indicates the solar value.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.cm,clip]{0651fig1.eps} \end{figure}$	Figure 1: The synthetic spectrum around the He I line at $\lambda$ 5875.6 Å. Computations were carried out using a model atmosphere with $T_{\rm eff}=10~300$ K. Open circles - the observed spectrum, dashed line - solar abundance, dot-dashed line - -1.0 dex, solid line - -2.0 dex (adopted), and thin solid line - -3.0 dex compared with the solar value.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{0651fig2.eps} \end{figure}$	Figure 2: The synthetic spectrum around the Fe II $\lambda$ 6147 Å and $\lambda$ 6149 Å lines. Open circles represent the observed spectrum, the solid line is for the adopted abundance (log $\epsilon$ (Fe II) = 8.54) with the 4.7 kG magnetic field, $\xi$ _t = 0 km s^-1. An unidentified feature is indicated by a question mark.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.0cm,clip]{0651fig3.eps} \end{figure}$	Figure 3: The synthetic line profile fitting of the C II lines at $\lambda$ 4267 Å. Open circles - the observed spectrum, dashed line - the solar abundance, and solid line - -0.25 dex compared with the solar value (adopted).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{0651fig4.eps} \end{figure}$	Figure 4: The synthetic line profile fittings for the O I $\lambda$ 6156-6158 Å triplet lines. Open circles - the observed spectrum, dashed line - the solar abundance, solid line - the adopted abundance (-0.56 dex), and thin solid line - -1.0 dex compared with the solar value.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0651fig5.eps} \end{figure}$	Figure 5: The synthetic spectrum of the Cl II lines at $\lambda$ 4794.56 Å. Open circles represent the observed spectrum, and solid line indicates the profile for the adopted abundance (7.21).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0651fig6.eps} \end{figure}$	Figure 6: The synthetic spectrum of the Co II lines at $\lambda$ 4915.42 Å. Open circles represent the observed spectrum, and solid line indicates the profile for the adopted abundance (8.50). Unidentified features are indicated by question marks.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0651fig7.eps} \end{figure}$	Figure 7: The synthetic spectrum of the Ba II line at $\lambda$ 4554.03 Å. Open circles - the observed spectrum, dashed line - +1.0 dex, dot-dashed line - +0.5 dex, solid line - solar abundance (adopted), and thin solid line - -1.0 dex compared with the solar value. An unidentified feature is indicated by a question mark.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0651fig8.eps} \end{figure}$	Figure 8: The synthetic spectrum of the Pr III line at $\lambda$ 6160.23 Å. Open circles represent the observed spectrum, and the solid line indicates the profile for the adopted abundance. An unidentified feature is indicated by a question mark.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0651fig9.eps} \end{figure}$	Figure 9: The abundances in logarithmic units for HR 5049 compared with the solar values. Upper limits for three elements are shown by downward arrows.
Open with DEXTER