All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2579fig1.ps} \end{figure}$ Figure 1: The two figures illustrate the solar poles in the light emitted by the Fe XII 195 Å line ( $1.5~\times~10^{6}$ K), taken by EIT/SoHO. The vertical white lines show the fixed position of the SUMER slit during the observations for PCH 1 and PCH 2a. The third dataset, PCH 2b, is taken in the same southern hole, four days before the PCH 2a data.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{2579fig2.eps} \end{figure}$ Figure 2: The temporal evolution of the northern coronal hole (PCH 1) seen in the N IV 765 Å ( left) and Ne VIII 770 Å ( right) lines, with a cadence of 30 s. Spicule structures are clearly seen in the TR line N IV (140 000 K), but not in the higher temperature line Ne VIII (630 000 K). At the top of the figures we show the radiance varying with time for both lines at the height of 10 $^{\prime \prime }$ above the limb (indicated, in the 2D plots, by the dotted black line). The continuous black line represents the N IV limb.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{2579fig3.eps} \end{figure}$ Figure 3: The evolution of a small region at the solar limb, inside the southern coronal hole (PCH 2a). The image is a time sequence taken repeatedly every minute for $\approx$ 14 h. Brighter colors represent higher radiance of the N IV 765 Å line.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16.5cm,clip]{2579fig4.eps} \end{figure}$ Figure 4: Radiance ratio $I/I_{\rm b}$ ( $I_{\rm b}$ is the background radiance taken from the darkest pixel at each height) versus time (in min) at 10 $^{\prime \prime }$ and 15 $^{\prime \prime }$ above the limb for PCH 2a (N IV 765 Å line). The over-plotted curves represent $I_{\rm b}\ge 4$ ; we use them for counting the spicules. With "A'' and "B'' we denote two locations where spicules show an obvious periodicity.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2579fig5.eps} \end{figure}$ Figure 5: Top panel: a segment plot (the first 100 min) taken from PCH 2a showing the temporal map of the N IV 765 Å radiance, with overlaid contours showing different levels of radiance in logarithmic scale. The other panels represent the line Doppler shift (thin black curve) and radiance (the thick grey curve) varying with time at three locations: at 5 $^{\prime \prime }$ , 10 $^{\prime \prime }$ and 15 $^{\prime \prime }$ above the limb. Note that the radiance is inverted to enable an easier comparison with the contours from the top panel. Vertical dotted lines show examples of positions where, in the third panel (at 10 $^{\prime \prime }$ ), the velocity changes its sign (negative values represent blue-shifts, or outflows; positive values - redshifts, or inflows). This transition of the spicule Doppler shift could be caused by material falling after rising.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=8.5cm]{2579fig6a.eps}\includegraphics[width=8.3cm]{2579fig6b.eps} }\end{figure}$ Figure 6: Time-series Dopplergram and radiance map for the C III 977 Å line, in PCH 2b, with contours showing levels of radiance in logarithmic scale. Right panels show the relative Doppler shift at four locations above the limb: at 0 $^{\prime \prime }$ , 5 $^{\prime \prime }$ , 10 $^{\prime \prime }$ and 15 $^{\prime \prime }$ off-limb.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{2579fig7.eps} \end{figure}$ Figure 7: Time-series radiance map and Dopplergram in the N IV 765 Å line of two long macrospicules taken from PCH 2a. The plotted time intervals are between 460 and 505 min ( left two panels) and 750 and 795 min ( right two panels). The overlaid contours show radiance in logarithmic scale.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2579fig8.eps} \end{figure}$ Figure 8: The same as Fig. 7, but taken from PCH 1 (the time interval between 60 and 110 min).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2579fig1.ps} \end{figure}$	Figure 1: The two figures illustrate the solar poles in the light emitted by the Fe XII 195 Å line ( $1.5~\times~10^{6}$ K), taken by EIT/SoHO. The vertical white lines show the fixed position of the SUMER slit during the observations for PCH 1 and PCH 2a. The third dataset, PCH 2b, is taken in the same southern hole, four days before the PCH 2a data.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{2579fig3.eps} \end{figure}$	Figure 3: The evolution of a small region at the solar limb, inside the southern coronal hole (PCH 2a). The image is a time sequence taken repeatedly every minute for $\approx$ 14 h. Brighter colors represent higher radiance of the N IV 765 Å line.
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$\begin{figure} \par\mbox{ \includegraphics[width=8.5cm]{2579fig6a.eps}\includegraphics[width=8.3cm]{2579fig6b.eps} }\end{figure}$	Figure 6: Time-series Dopplergram and radiance map for the C III 977 Å line, in PCH 2b, with contours showing levels of radiance in logarithmic scale. Right panels show the relative Doppler shift at four locations above the limb: at 0 $^{\prime \prime }$ , 5 $^{\prime \prime }$ , 10 $^{\prime \prime }$ and 15 $^{\prime \prime }$ off-limb.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{2579fig7.eps} \end{figure}$	Figure 7: Time-series radiance map and Dopplergram in the N IV 765 Å line of two long macrospicules taken from PCH 2a. The plotted time intervals are between 460 and 505 min ( left two panels) and 750 and 795 min ( right two panels). The overlaid contours show radiance in logarithmic scale.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2579fig8.eps} \end{figure}$	Figure 8: The same as Fig. 7, but taken from PCH 1 (the time interval between 60 and 110 min).
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