Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[scale=0.55,clip]{neo_ratio.eps}\end{figure}$ Figure 2: The derived Ne/O 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 Ne/O abundance ratio (Asplund et al. 2005a).
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In the text

$\begin{figure} \par\includegraphics[scale=0.55,clip]{emd_figure_encap_neo.eps}\end{figure}$ Figure 3: A comparsion of column depths (h) derived from the present analysis (solid line) with those from Young (2005) (dashed line) for the network spectrum from CDS data-set s10133r00. The curves are scaled to remove the dependence on the reference abundances (see text).
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In the text

$\begin{figure} \par\includegraphics[scale=0.55,clip]{ne_o.eps}\end{figure}$	Figure 1: Ionization fraction curves from Mazzotta et al. (1998) for the neon and oxygen ions.
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$\begin{figure} \par\includegraphics[scale=0.55,clip]{neo_ratio.eps}\end{figure}$	Figure 2: The derived Ne/O 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 Ne/O abundance ratio (Asplund et al. 2005a).
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$\begin{figure} \par\includegraphics[scale=0.55,clip]{emd_figure_encap_neo.eps}\end{figure}$	Figure 3: A comparsion of column depths (h) derived from the present analysis (solid line) with those from Young (2005) (dashed line) for the network spectrum from CDS data-set s10133r00. The curves are scaled to remove the dependence on the reference abundances (see text).
Open with DEXTER