All Figures

$\begin{figure} \par\includegraphics[width=7.5cm]{3672_f1.eps} \end{figure}$ Figure 1: Green's functions $G(\mu , \epsilon ,\epsilon _0)$ including Compton scattering and photoelectric absorption for three primary photon energies $\epsilon _0 =20,80,300$ keV and $\mu =0.7$ ( $\theta \sim 45^\circ$ ).
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In the text

$\begin{figure} \par\includegraphics[width=73mm]{3672_f2.eps} \end{figure}$ Figure 2: Upper panel: primary (solid line), reflected (dotted line) and total (dashed line) photon spectra calculated assuming a primary spectrum $I_{\rm P}(\epsilon )\sim \epsilon ^{-3}$ , and using the Green's function for a X-ray source at heliocentric angle $\theta = 45^\circ$ . The lower panel shows the reflectivity, defined as the ratio of reflected to primary fluxes $R(\epsilon , \theta =45^\circ )=I_{\rm R}(\epsilon )/I_{\rm P}(\epsilon )$ . The reflectivity taken from Bai & Ramaty (1978) is shown with diamonds. Two absorption edges of Fe at 7.1 keV and Ni at 8.3 keV are seen in the reflected component.
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In the text

$\begin{figure} \par\includegraphics[width=78mm]{3672_f2a.eps} \end{figure}$ Figure 3: Spectrum dependency of the reflected flux. Upper panel: primary (dashed line), reflected (solid line) and total (dotted line) photon spectra calculated for a modelled flare spectrum $I_{\rm P}(\epsilon )\sim \epsilon ^{-3}$ for $\epsilon > 45$ keV, $I_{\rm P}(\epsilon)\sim \epsilon ^{-2}+\exp(-\epsilon/1.7)$ for $\epsilon < 45$ keV. The lower panel shows the reflectivity for a X-ray source at heliocentric angle $\theta = 45^\circ$ , defined as the ratio of reflected to primary fluxes $R(\epsilon , \theta =45^\circ )=I_{\rm R}(\epsilon )/I_{\rm P}(\epsilon )$ (solid line). The reflectivity assuming power-law for a primary source with spectral index 3 (dotted line) and 2 (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=80mm]{3672_f3.eps} \end{figure}$ Figure 4: Temporal variation in four energy channels (4 seconds cadence) of the count rates summed over seven front RHESSI detectors for the September 17, 2002 solar flare. The vertical lines show the accumulation interval selected 5:50:48-5:51:36 UT for further spectral analysis.
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In the text

$\begin{figure} \par\includegraphics[width=72mm]{3672_f4.eps} \end{figure}$ Figure 5: Spectrum of the September 17, 2002 solar flare in the time interval 5:50:48-5:51:36 UT. The solid line shows the observed spectrum; the dash line is the primary spectrum (corrected for Compton back-scattering).
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In the text

$\begin{figure} \par\includegraphics[width=65mm]{3672_f5.eps} \end{figure}$ Figure 6: Energy dependent photon spectral index $\gamma (\epsilon )$ of the September 17, 2002 solar flare. The solid line shows the spectral index of the observed spectrum; the dash line is the spectral index for the primary spectrum (corrected for Compton back-scattering). The confidence intervals represent the range of solutions found by allowing the incident photon spectrum to range randomly within the estimated (instrument + shot noise) errors.
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In the text

$\begin{figure} \par\includegraphics[width=75mm]{3672_f6.eps} \end{figure}$ Figure 7: Mean electron flux spectra of the September, 2002 solar flare. The solid/dash lines show the spectrum without and with albedo correction.
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In the text

$\begin{figure} \par\includegraphics[width=65mm]{3672_f7.eps} \end{figure}$ Figure 8: Inverted mean electron flux of the August 20, 2002 solar flare for the time interval 08:25:20-08:25:40 UT. The dash line shows the spectra with albedo correction. The confidence intervals represent the range of solutions found by allowing the incident photon spectrum to range randomly within the estimated (instrument + shot noise) errors.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{3672_f1.eps} \end{figure}$	Figure 1: Green's functions $G(\mu , \epsilon ,\epsilon _0)$ including Compton scattering and photoelectric absorption for three primary photon energies $\epsilon _0 =20,80,300$ keV and $\mu =0.7$ ( $\theta \sim 45^\circ$ ).
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$\begin{figure} \par\includegraphics[width=80mm]{3672_f3.eps} \end{figure}$	Figure 4: Temporal variation in four energy channels (4 seconds cadence) of the count rates summed over seven front RHESSI detectors for the September 17, 2002 solar flare. The vertical lines show the accumulation interval selected 5:50:48-5:51:36 UT for further spectral analysis.
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$\begin{figure} \par\includegraphics[width=72mm]{3672_f4.eps} \end{figure}$	Figure 5: Spectrum of the September 17, 2002 solar flare in the time interval 5:50:48-5:51:36 UT. The solid line shows the observed spectrum; the dash line is the primary spectrum (corrected for Compton back-scattering).
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$\begin{figure} \par\includegraphics[width=75mm]{3672_f6.eps} \end{figure}$	Figure 7: Mean electron flux spectra of the September, 2002 solar flare. The solid/dash lines show the spectrum without and with albedo correction.
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$\begin{figure} \par\includegraphics[width=65mm]{3672_f7.eps} \end{figure}$	Figure 8: Inverted mean electron flux of the August 20, 2002 solar flare for the time interval 08:25:20-08:25:40 UT. The dash line shows the spectra with albedo correction. The confidence intervals represent the range of solutions found by allowing the incident photon spectrum to range randomly within the estimated (instrument + shot noise) errors.
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