All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9997fig1.ps}\end{figure}$ Figure 1: A schematic illustratration of the orbit of XMM-Newton in relation to the magnetopause and bow shock (dotted lines), which define the boundaries of the magnetosheath, at different times during the year. The left image shows the highly elliptical orbit of XMM-Newton during mid summer (northern hemisphere), and the right image shows the winter configuration. The Sun has been added to show the direction of the Sun and therefore incoming solar wind.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7cm,clip]{9997fig2.ps}\par\includegraphics[angle=270,width=7cm,clip]{9997fig3.ps}\end{figure}$ Figure 2: Example count rate histograms from the ESAS software where a Gaussian shaped curve is fitted to the histogram. The upper panel shows a count rate histogram where the data and the Gaussian curve are almost coincident and little or no flaring has occurred, whereas the lower panel shows flaring characteristics.
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In the text

$\begin{figure} \par\subfigure[Example scatterplot where no SWCX is expected, sho... ..._{\mu}$\ value]{\includegraphics[width=7.3cm,clip]{9997fig5.ps} } \end{figure}$ Figure 3: Example scatter plots between the line and continuum bands for an observation that has experienced high levels of residual soft proton contamination, yet still shows a good linear fit between the line and continuum count rates ( first panel) and an observation that shows SWCX-emission features ( second panel). Representative average error bars are plotted in the bottom right-hand corner of each plot.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9997fig6.ps} \end{figure}$ Figure 4: Histogram of $\chi ^{2}_{\mu }$ values.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9997fig7.ps} \end{figure}$ Figure 5: Histogram of $R_{\chi }$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9997fig8.ps} \end{figure}$ Figure 6: Histogram of Fin/Fout ratios.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{9997fig9.ps} \end{figure}$ Figure 7: Scatter plot of $\chi ^{2}_{\mu }$ versus $R_{\chi }$ values. Filled circle are used for observations with a suspected or previously published SWCX enhancement.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9997fig10.ps} \end{figure}$ Figure 8: Scatter plot of $R_{\chi }$ versus Fin/Fout values. Filled circles are used for observations with a suspected or previously published SWCX enhancement.
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In the text

$\begin{figure} \par\mbox{\subfigure[Case $\{$ 12$\}$ , GWS1]{ \includegraphics[... ...$\}$ , GWS3]{ \includegraphics[width=4.8cm,clip]{9997fig13.ps} }} \end{figure}$ Figure 9: Lightcurves for observations of the Groth-Westhall Strip. Blue represents the solar proton flux, black the line band count rate and red the continuum band count rate. These observations were studied spectrally by Kuntz & Snowden (2008) and cases $\{$ 13 $\}$ and $\{$ 10 $\}$ were found to have SWCX-enhancement, whereas $\{$ 64 $\}$ was devoid of SWCX features.
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In the text

$\begin{figure} \par\mbox{\subfigure[Case $\{$ 12$\}$ , GWS1]{ \includegraphics[... ...$\}$ , GWS3]{ \includegraphics[width=4.7cm,clip]{9997fig16.ps} }} \end{figure}$ Figure 10: Scatter plots for observations of the Groth-Westhall Strip. These observations were studied spectrally by Kuntz & Snowden (2008) and cases $\{$ 13 $\}$ and $\{$ 10 $\}$ were found to have SWCX-enhancement, whereas $\{$ 64 $\}$ was devoid of SWCX features.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.6cm,clip]{9997fig17.ps} \end{figure}$ Figure 11: The resultant spectrum for case {1}. The model to the SWCX lines folded through the instrument response is plotted in red. The excess seen around 1.49 keV and 1.74 keV results from particle-induced instrumental background.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip=]{9997f12.eps}\par\end{figure}$ Figure 12: XMM-Newton lightcurves, orbital positions and spectra for example cases of SWCX-enhancement. In the first panel for each case, the blue line represents the solar proton flux during each observation, plotted including the expected one hour delay and the vertical lines indicate the start or stop times for the division of the events into SWCX-enhanced and non SWCX-enhanced periods. Black and red represent the line and continuum band lightcurves respectively, similarly for the spectra shown in the last panel. The second and third panels show XMM-Newton in orbit around the Earth in the GSE X-Y and X-Z planes. The positive x-axis is directed towards the Sun and the positive y-axis is directed in the direction of the orbit of XMM-Newton.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip=]{9997f13.eps}\par\end{figure}$ Figure 13: Lightcurves, orbital positions and spectra for suspected cases of weak or dubious SWCX-enhancement, arranged in panels as for the strong cases of SWCX-enhancement.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7cm,clip]{9997fig2.ps}\par\includegraphics[angle=270,width=7cm,clip]{9997fig3.ps}\end{figure}$	Figure 2: Example count rate histograms from the ESAS software where a Gaussian shaped curve is fitted to the histogram. The upper panel shows a count rate histogram where the data and the Gaussian curve are almost coincident and little or no flaring has occurred, whereas the lower panel shows flaring characteristics.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9997fig6.ps} \end{figure}$	Figure 4: Histogram of $\chi ^{2}_{\mu }$ values.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9997fig7.ps} \end{figure}$	Figure 5: Histogram of $R_{\chi }$ .
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9997fig8.ps} \end{figure}$	Figure 6: Histogram of Fin/Fout ratios.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{9997fig9.ps} \end{figure}$	Figure 7: Scatter plot of $\chi ^{2}_{\mu }$ versus $R_{\chi }$ values. Filled circle are used for observations with a suspected or previously published SWCX enhancement.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{9997fig10.ps} \end{figure}$	Figure 8: Scatter plot of $R_{\chi }$ versus Fin/Fout values. Filled circles are used for observations with a suspected or previously published SWCX enhancement.
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$\begin{figure} \par\mbox{\subfigure[Case $\{$ 12$\}$ , GWS1]{ \includegraphics[... ...$\}$ , GWS3]{ \includegraphics[width=4.8cm,clip]{9997fig13.ps} }} \end{figure}$	Figure 9: Lightcurves for observations of the Groth-Westhall Strip. Blue represents the solar proton flux, black the line band count rate and red the continuum band count rate. These observations were studied spectrally by Kuntz & Snowden (2008) and cases $\{$ 13 $\}$ and $\{$ 10 $\}$ were found to have SWCX-enhancement, whereas $\{$ 64 $\}$ was devoid of SWCX features.
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$\begin{figure} \par\mbox{\subfigure[Case $\{$ 12$\}$ , GWS1]{ \includegraphics[... ...$\}$ , GWS3]{ \includegraphics[width=4.7cm,clip]{9997fig16.ps} }} \end{figure}$	Figure 10: Scatter plots for observations of the Groth-Westhall Strip. These observations were studied spectrally by Kuntz & Snowden (2008) and cases $\{$ 13 $\}$ and $\{$ 10 $\}$ were found to have SWCX-enhancement, whereas $\{$ 64 $\}$ was devoid of SWCX features.
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$\begin{figure} \par\includegraphics[angle=270,width=7.6cm,clip]{9997fig17.ps} \end{figure}$	Figure 11: The resultant spectrum for case {1}. The model to the SWCX lines folded through the instrument response is plotted in red. The excess seen around 1.49 keV and 1.74 keV results from particle-induced instrumental background.
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$\begin{figure} \par\includegraphics[width=14cm,clip=]{9997f13.eps}\par\end{figure}$	Figure 13: Lightcurves, orbital positions and spectra for suspected cases of weak or dubious SWCX-enhancement, arranged in panels as for the strong cases of SWCX-enhancement.
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