All Figures

$\begin{figure} \par\includegraphics[width=7cm,height=12.5cm,clip]{Fd301_Fig1a.ps... ...ps}\includegraphics[width=5.3cm,height=12.5cm,clip]{Fd301_Fig1c.ps} \end{figure}$ Figure 1: A TRACE 1600 Å image of the sunspot and surrounding region (taken at 21:14 UT on 18 March 1999) with the position of the SUMER slit and TRACE white light contours over-plotted (left panel) out-lining the umbra and penumbra. The central panel and the right panel are the intensity variations along the SUMER slit as seen in N IV 765 Å (at 21:01 UT) and Si IV 1402.77 Å (at 20:13 UT) respectively. The 10 $^{\prime \prime }$ region centered around 40 $^{\prime \prime }$ along the slit is known as QS₁, while QS₂ is the region centered around 100 $^{\prime \prime }$ . SS₁ and SS₂ are centered around 70 $^{\prime \prime }$ and 80 $^{\prime \prime }$ respectively along the slit.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{Fd301_Fig2.ps} \end{figure}$ Figure 2: The SUMER sunspot plume spectrum SS₁ (solid line) obtained on 18 March 1999 with the quiet sun QS₂ (dotted line) spectrum over-plotted showing the six lines from within the O V 760 Å multiplet. Note that for presentation purposes the QS₂ spectrum was multiplied by a factor of three, also note the line-shift to the red in the sunspot data.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{Fd301_Fig3.ps} \end{figure}$ Figure 3: Three electron density diagnostic line ratios from within the O V 760 Å multiplet, i.e. R₁ = 761.13/758.68, R₂ = 761.13/759.43 and R₃ = 761.13/761.99 plotted assuming the temperature of formation is $\log T_{\rm e}/{\rm K} = 5.4$ . The derived densities (based on the data in Table 1) in all four regions are indicated.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{Fd301_Fig4.ps} \end{figure}$ Figure 4: The O V 761.13/758.68 line ratio for three different values of $\log T_{\rm e}/{\rm K}$ ; 5.2, 5.4 and 5.6, with the central temperature being the value at the peak of the O V contribution function. The short horizontal line is the SS₁ line ratio while the arrows show the range of inferred electron densities.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{Fd301_Fig2.ps} \end{figure}$	Figure 2: The SUMER sunspot plume spectrum SS₁ (solid line) obtained on 18 March 1999 with the quiet sun QS₂ (dotted line) spectrum over-plotted showing the six lines from within the O V 760 Å multiplet. Note that for presentation purposes the QS₂ spectrum was multiplied by a factor of three, also note the line-shift to the red in the sunspot data.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{Fd301_Fig3.ps} \end{figure}$	Figure 3: Three electron density diagnostic line ratios from within the O V 760 Å multiplet, i.e. R₁ = 761.13/758.68, R₂ = 761.13/759.43 and R₃ = 761.13/761.99 plotted assuming the temperature of formation is $\log T_{\rm e}/{\rm K} = 5.4$ . The derived densities (based on the data in Table 1) in all four regions are indicated.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{Fd301_Fig4.ps} \end{figure}$	Figure 4: The O V 761.13/758.68 line ratio for three different values of $\log T_{\rm e}/{\rm K}$ ; 5.2, 5.4 and 5.6, with the central temperature being the value at the peak of the O V contribution function. The short horizontal line is the SS₁ line ratio while the arrows show the range of inferred electron densities.
Open with DEXTER