All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3272fig1.eps} \end{figure}$ Figure 1: The spatial distribution of the investigated sample of CP2 stars divided into Si (filled circle), SiCr (open circle) and SrCrEu (asterisk) objects.
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In the text

$\begin{figure} \par\includegraphics[width=15.3cm,clip]{3272fig2.eps} \end{figure}$ Figure 2: The Hertzsprung-Russell-Diagram for our sample of CP2 stars, the symbols are the same as in Fig. 1. The evolutionary tracks from 1.5 to 4 $M_{\odot }$ , lines of equal $\tau /\tau _{\rm HR}$ , the ZAMS as well as TAMS are for [Z] = 0.016 taken from Schaller et al. (1992) and Schaerer et al. (1993). The typical errors are plotted in the upper right corner.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3272fig3.eps} \end{figure}$ Figure 3: A detailed statistical analysis of our sample. We have divided the sample into Si ( upper left), SiCr ( upper right) and SrCrEu ( lower left) subgroups and investigated the incidence of these objects depending on their masses. The lower right panel shows the comparison of all stars divided into subgroups with masses higher (denoted with a pattern) and lower than 3 $M_{\odot }$ according to the investigated sample by Hubrig et al. (2000). The Spearman rank order correlation coefficient and the $\chi ^2$ test for these two samples give both a significance level of about 25% for a possible correlation. However, these tests are only based on five data points.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3272fig4.eps} \end{figure}$ Figure 4: The log B_e versus $\tau /\tau _{\rm HR}$ as well as log $T_{\rm eff}$ diagrams for our program stars. The magnetic field strengths were taken from Bychkov et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3272fig1.eps} \end{figure}$	Figure 1: The spatial distribution of the investigated sample of CP2 stars divided into Si (filled circle), SiCr (open circle) and SrCrEu (asterisk) objects.
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$\begin{figure} \par\includegraphics[width=15.3cm,clip]{3272fig2.eps} \end{figure}$	Figure 2: The Hertzsprung-Russell-Diagram for our sample of CP2 stars, the symbols are the same as in Fig. 1. The evolutionary tracks from 1.5 to 4 $M_{\odot }$ , lines of equal $\tau /\tau _{\rm HR}$ , the ZAMS as well as TAMS are for [Z] = 0.016 taken from Schaller et al. (1992) and Schaerer et al. (1993). The typical errors are plotted in the upper right corner.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{3272fig4.eps} \end{figure}$	Figure 4: The log B_e versus $\tau /\tau _{\rm HR}$ as well as log $T_{\rm eff}$ diagrams for our program stars. The magnetic field strengths were taken from Bychkov et al. (2003).
Open with DEXTER