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$\begin{figure} {\epsfig{file=H1849f1.ps, width=7cm,angle=90 } } \end{figure}$ Figure 1: The emissivity ratio curves calculated at log $T[{\rm K}]=7.2$ and relative to the $n=4 \to 2$ transitions from singly-excited levels observed in the laser spectra by Boiko et al. (1978). The curves are labelled with increasing numbers. For each line, we indicate: the observed intensities $I_{\rm ob}$ ; the lower and upper level index corresponding to Table 2; the theoretical wavelength. The dashed lines indicate agreement within $\pm$ 20%.
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In the text

$\begin{figure} {\epsfig{file=H1849f2.ps, width=7.cm,angle=90 } } \end{figure}$ Figure 2: The emissivity ratio curves calculated at log $T[{\rm K}]=7.2$ and relative to the $n=4 \to 2$ transitions from doubly-excited levels observed in the laser spectra by Boiko et al. (1978). The dashed lines indicate relative agreement within $\pm$ 50%.
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In the text

$\begin{figure} {\epsfig{file=H1849f3a.ps, width=6.cm,angle=90 } }\vspace*{3mm} {\epsfig{file=H1849f3b.ps, width=6.5cm,angle=90 } } \end{figure}$ Figure 3: Top: total count rates observed by SMM/BCS during the 1985 July 2 flare in the 1.87-1.88 Å range, dominated by Fe XXIII inner-shell lines. The time interval of the region 8.30-8.92 Å scanned by the SMM/FCS is also shown. Line intensities decrease by a maximum 10% during the FCS scan. Bottom: the emissivity ratio curves calculated at 10¹² cm^-3 and relative to the $n=4 \to 2$ transitions measured in the SMM/FCS solar spectrum by Fawcett et al. (1987). With the exception of the first spectral line (8.30 Å), all other ones intersect within $\pm$ 30%, indicating an isothermal plasma at $\log~ T \simeq 7.0 \pm 0.1$ .
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In the text

$\begin{figure} {\epsfig{file=H1849f4.ps, width=7.cm,angle=90 } } \end{figure}$ Figure 4: The emissivity ratio curves calculated at log $T[{\rm K}]=7.2$ and relative to the $n=3 \to 2$ transitions from singly-excited levels observed in laser spectra by Boiko et al. (1978).
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In the text

$\begin{figure} {\epsfig{file=H1849f5a.ps, width=6.cm,angle=90 } }\vspace*{3mm} {\epsfig{file=H1849f5b.ps, width=6.5cm,angle=90 } } \end{figure}$ Figure 5: Top: total count rates observed by SMM/BCS during the 1980 August 25 flare in the 1.87-1.88 Å range, dominated by Fe XXIII inner-shell lines. The time interval of the region 10.98-12.16 Å scanned by the SMM/FCS is also shown. Bottom: the emissivity ratio curves calculated at 10¹² cm^-3 and relative to the $n=3 \to 2$ transitions observed in the SMM/FCS spectrum.
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In the text

$\begin{figure} {\epsfig{file=H1849f6a.ps, width=7.cm,angle=90 } }\vspace*{3mm} {\epsfig{file=H1849f6b.ps, width=7.cm,angle=90 } } \end{figure}$ Figure 6: The emissivity ratio curves calculated at 10¹² cm^-3 and relative to the $n=3,4\to 2$ transitions observed with the SOLEX A and B spectrometers (McKenzie et al. 1985).
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In the text

$\begin{figure} {\epsfig{file=H1849f7.ps, width=7.cm,angle=90 } } \end{figure}$ Figure 7: The emissivity ratio curves calculated at 10¹² cm^-3 and relative to the $n=3 \to 2$ , ${n=2\to 2}$ transitions observed in the Chandra HETG and EUVE spectra of $\sigma ^2$ CrB during its quiescent state reported by Osten et al. (2003). The agreement with theory is excellent (within 20%), indicating an electron temperature log $T[{\rm K}] \simeq 7.25$ .
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In the text

$\begin{figure} {\epsfig{file=H1849f8.ps, width=7.cm,angle=90 } } \end{figure}$ Figure 8: The emissivity ratio curves calculated at 10¹² cm^-3 and relative to the $n=3,4\to 2$ transitions observed with the Chandra HETG and emitted by the hot young star $\Theta ^1$ Ori C (Schulz et al. 2003). The agreement, when considering the entire spectral range, is only marginal ( $\pm$ 50%).
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In the text

$\begin{figure} {\epsfig{file=H1849f2.ps, width=7.cm,angle=90 } } \end{figure}$	Figure 2: The emissivity ratio curves calculated at log $T[{\rm K}]=7.2$ and relative to the $n=4 \to 2$ transitions from doubly-excited levels observed in the laser spectra by Boiko et al. (1978). The dashed lines indicate relative agreement within $\pm$ 50%.
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$\begin{figure} {\epsfig{file=H1849f4.ps, width=7.cm,angle=90 } } \end{figure}$	Figure 4: The emissivity ratio curves calculated at log $T[{\rm K}]=7.2$ and relative to the $n=3 \to 2$ transitions from singly-excited levels observed in laser spectra by Boiko et al. (1978).
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$\begin{figure} {\epsfig{file=H1849f5a.ps, width=6.cm,angle=90 } }\vspace*{3mm} {\epsfig{file=H1849f5b.ps, width=6.5cm,angle=90 } } \end{figure}$	Figure 5: Top: total count rates observed by SMM/BCS during the 1980 August 25 flare in the 1.87-1.88 Å range, dominated by Fe XXIII inner-shell lines. The time interval of the region 10.98-12.16 Å scanned by the SMM/FCS is also shown. Bottom: the emissivity ratio curves calculated at 10¹² cm^-3 and relative to the $n=3 \to 2$ transitions observed in the SMM/FCS spectrum.
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$\begin{figure} {\epsfig{file=H1849f6a.ps, width=7.cm,angle=90 } }\vspace*{3mm} {\epsfig{file=H1849f6b.ps, width=7.cm,angle=90 } } \end{figure}$	Figure 6: The emissivity ratio curves calculated at 10¹² cm^-3 and relative to the $n=3,4\to 2$ transitions observed with the SOLEX A and B spectrometers (McKenzie et al. 1985).
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$\begin{figure} {\epsfig{file=H1849f7.ps, width=7.cm,angle=90 } } \end{figure}$	Figure 7: The emissivity ratio curves calculated at 10¹² cm^-3 and relative to the $n=3 \to 2$ , ${n=2\to 2}$ transitions observed in the Chandra HETG and EUVE spectra of $\sigma ^2$ CrB during its quiescent state reported by Osten et al. (2003). The agreement with theory is excellent (within 20%), indicating an electron temperature log $T[{\rm K}] \simeq 7.25$ .
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$\begin{figure} {\epsfig{file=H1849f8.ps, width=7.cm,angle=90 } } \end{figure}$	Figure 8: The emissivity ratio curves calculated at 10¹² cm^-3 and relative to the $n=3,4\to 2$ transitions observed with the Chandra HETG and emitted by the hot young star $\Theta ^1$ Ori C (Schulz et al. 2003). The agreement, when considering the entire spectral range, is only marginal ( $\pm$ 50%).
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