All Figures

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{2963fig1.eps}\end{figure}$ Figure 1: The O V $\lambda$ 629.7 intensity at which the division between network and cell centre regions occurs for each of the 24 data-sets.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2963fig2.eps}\end{figure}$ Figure 2: Ionization fraction curves from Mazzotta et al. (1998) for the magnesium and neon ions.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2963fig3.eps}\end{figure}$ Figure 3: Column depths (h) derived from the supergranule network spectrum of CDS data-set s10133r00 (1998 January 10). The three values at $\log~T=5.0$ , 5.6 and 6.1 were derived through the minimization procedure, all other values are obtained by linear interpolation from these three values.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2963fig4.eps}\end{figure}$ Figure 4: The derived Mg/Ne abundance ratios for the network ( upper panel) and cell centre ( lower panel) regions as a function of time. The black horiontal line denotes the photospheric Mg/Ne abundance ratio. The grey line shows the variation in the sunspot number over the period of observations, from a value of 10 at day 0 to 68 at day 900.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2963fig5.eps}\end{figure}$ Figure 5: Variation of the Si IX $\lambda$ 349.9/ $\lambda$ 345.1 ratio as a function of density. Calculated with v4.2 of the CHIANTI database at a temperature of $\log~(T/{\rm K})=6.1$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2963fig6.eps}\end{figure}$ Figure 6: Variation of spectral properties over the 850 day period considered. a) electron density derived from Si IX $\lambda$ 349.9/ $\lambda$ 345.1 diagnostic; b) coronal isothermal temperature derived from Mg X $\lambda$ 624.9/ $\lambda$ 368.1 ratio; c) absolute line intensities for three species. In each plot linear fits to the data are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{2963fig1.eps}\end{figure}$	Figure 1: The O V $\lambda$ 629.7 intensity at which the division between network and cell centre regions occurs for each of the 24 data-sets.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2963fig2.eps}\end{figure}$	Figure 2: Ionization fraction curves from Mazzotta et al. (1998) for the magnesium and neon ions.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2963fig3.eps}\end{figure}$	Figure 3: Column depths (h) derived from the supergranule network spectrum of CDS data-set s10133r00 (1998 January 10). The three values at $\log~T=5.0$ , 5.6 and 6.1 were derived through the minimization procedure, all other values are obtained by linear interpolation from these three values.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2963fig4.eps}\end{figure}$	Figure 4: The derived Mg/Ne abundance ratios for the network ( upper panel) and cell centre ( lower panel) regions as a function of time. The black horiontal line denotes the photospheric Mg/Ne abundance ratio. The grey line shows the variation in the sunspot number over the period of observations, from a value of 10 at day 0 to 68 at day 900.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2963fig5.eps}\end{figure}$	Figure 5: Variation of the Si IX $\lambda$ 349.9/ $\lambda$ 345.1 ratio as a function of density. Calculated with v4.2 of the CHIANTI database at a temperature of $\log~(T/{\rm K})=6.1$ .
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2963fig6.eps}\end{figure}$	Figure 6: Variation of spectral properties over the 850 day period considered. a) electron density derived from Si IX $\lambda$ 349.9/ $\lambda$ 345.1 diagnostic; b) coronal isothermal temperature derived from Mg X $\lambda$ 624.9/ $\lambda$ 368.1 ratio; c) absolute line intensities for three species. In each plot linear fits to the data are shown.
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