$\begin{figure} \par\includegraphics[width=12cm,clip]{9235fig1.eps}\end{figure}$ Figure 1: Intensity images of N IV ( left) and Ne VIII ( right) in the first data set (from 18:00 on March 7 to 17:42 on March 8 in 1997). The intensity images are in logarithmic scale. The two sub-regions enclosed by white lines are defined as the coronal-hole and quiet-Sun parts and studied in detail.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{9235fig2.eps}\end{figure}$ Figure 2: Intensity images of S IV ( left) and Ne VIII ( right) of the second data set ( upper panel, observed from 15:10 on September 28 to 03:18 on September 29) and the third data set ( lower panel, observed from 8:21 to 15:48 on April 16). The intensity images are in logarithmic scale.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{9235fig3.eps}\end{figure}$ Figure 3: Temperature/height variations of the characteristic sizes of intensity, Doppler shift and non-thermal width ( left), as well as of the extrapolated magnetic field ( right) in the quiet Sun ( upper panel) and coronal hole ( lower panel) for the first data set.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{9235fig4.eps}\end{figure}$ Figure 4: Temperature/height variations of the characteristic sizes of line intensity structures ( left) and of structures inferred from the coronal magnetic field parameters ( right) in the quiet Sun ( upper panel, for the second data set) and coronal hole ( lower panel, for the third data set).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{9235fig1.eps}\end{figure}$	Figure 1: Intensity images of N IV ( left) and Ne VIII ( right) in the first data set (from 18:00 on March 7 to 17:42 on March 8 in 1997). The intensity images are in logarithmic scale. The two sub-regions enclosed by white lines are defined as the coronal-hole and quiet-Sun parts and studied in detail.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{9235fig2.eps}\end{figure}$	Figure 2: Intensity images of S IV ( left) and Ne VIII ( right) of the second data set ( upper panel, observed from 15:10 on September 28 to 03:18 on September 29) and the third data set ( lower panel, observed from 8:21 to 15:48 on April 16). The intensity images are in logarithmic scale.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{9235fig3.eps}\end{figure}$	Figure 3: Temperature/height variations of the characteristic sizes of intensity, Doppler shift and non-thermal width ( left), as well as of the extrapolated magnetic field ( right) in the quiet Sun ( upper panel) and coronal hole ( lower panel) for the first data set.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{9235fig4.eps}\end{figure}$	Figure 4: Temperature/height variations of the characteristic sizes of line intensity structures ( left) and of structures inferred from the coronal magnetic field parameters ( right) in the quiet Sun ( upper panel, for the second data set) and coronal hole ( lower panel, for the third data set).
Open with DEXTER