All Figures

$\begin{figure} \par\includegraphics[width=14cm,clip]{0082f1.eps} \end{figure}$ Figure 1: Observed solar sidereal rotation velocities as a function of the CMD for 10-deg latitude bins: panel 1 for the latitudes $0.0 \le \psi < 10.0$ deg, panel 2 for the latitudes $10.0 \le \psi < 20.0$ deg, etc. Results obtained with the interactive method are presented for both solar hemispheres treated together. For details see text.
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In the text

$\begin{figure} \par\includegraphics[width=14.3cm,clip]{0082f2.eps} \end{figure}$ Figure 2: As Fig. 1 for the automatic method.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0082f3.eps} \end{figure}$ Figure 3: The mean values of sidereal rotation velocities of coronal bright points (BPs) using the interactive method with and without the height correction, as indicated in the legend. The averaging is performed in 10-deg latitude bins and the error bars indicate the standard errors of the means in each bin (calculated as $M=\sigma /\sqrt {N}$ , where $\sigma$ is the standard deviation and N the number of data points in the bin). Both solar hemispheres are treated together and the lines represent least-squares fits (C=0) to all filtered data points for each case. The parameters are given in the first lines in Tables 2 and 3, for the cases without and with height correction, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0082f4.eps} \end{figure}$ Figure 4: As Fig. 3 for the automatic method (the case with C=0, Tables 4 and 5).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0082f5.eps} \end{figure}$ Figure 5: Solar differential rotation curves for various tracers and methods. In the case of coronal bright points (BPs) the interactive method was used, and the results with and without the height correction are presented, as indicated in the legend (the case with B=C, Tables 2 and 3). The solar rotation parameters for H $\alpha$ filaments, sunspot groups, magnetic correlations and Doppler shifts are specified with further details in Table 6, in the lines 10, 7, 18, and 21,respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0082f6.eps} \end{figure}$ Figure 6: As Fig. 5 for the automatic method (the case with C=0, Tables 4 and 5).
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0082f1.eps} \end{figure}$	Figure 1: Observed solar sidereal rotation velocities as a function of the CMD for 10-deg latitude bins: panel 1 for the latitudes $0.0 \le \psi < 10.0$ deg, panel 2 for the latitudes $10.0 \le \psi < 20.0$ deg, etc. Results obtained with the interactive method are presented for both solar hemispheres treated together. For details see text.
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$\begin{figure} \par\includegraphics[width=14.3cm,clip]{0082f2.eps} \end{figure}$	Figure 2: As Fig. 1 for the automatic method.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0082f4.eps} \end{figure}$	Figure 4: As Fig. 3 for the automatic method (the case with C=0, Tables 4 and 5).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0082f6.eps} \end{figure}$	Figure 6: As Fig. 5 for the automatic method (the case with C=0, Tables 4 and 5).
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