All Figures

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2128f01a.eps}\hspace*{4mm} \includegraphics[width=8.4cm,clip]{2128f01b.eps} \end{figure}$ Figure 1: a) GOES X-ray flux in 0.5-4 Å and 1-8 Å. The two dashed vertical bars indicate the start and end time of RHESSI light curves in b) and the numbers (1-2) mark the two peaks of GOES 0.5-4 Å flux in the time range of RHESSI observation. b) RHESSI light curves in the energy range of 3-12 keV, 12-25 keV, and 25-50 keV retrieved from the RHESSI data of collimators and detectors 3F-8F with a time bin of 4 s. The numbers (1-2) mark the two peaks of RHESSI light curve that temporally correspond to the two GOES 0.5-4 Å peaks marked in Frame a).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{2128f02.eps} \end{figure}$ Figure 2: a), b) Magnetogram at 07:59:03 UT and c) intensity image at 06:46:00 UT observed by SOHO/MDI. d) and e) magnetogram and intensity image observed by THEMIS in the MSDP mode at Na I 5896 Å $\pm$ 0.1 Å. The image size of b)- e) is 130 $^{\prime \prime }$ $\times$ 130 $^{\prime \prime }$ . North is on the top and east to the left for all the images shown in this paper. Many fine thread-like structures are observed in the negative polarity in the THEMIS magnetogram shown in d). The spatial resolution of THEMIS images is estimated to be better than 0.8 $^{\prime \prime }$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{2128f03.eps} \end{figure}$ Figure 3: A selection of reconstructed RHESSI images (not normalized) from collimators and detectors 3F-8F using the CLEAN image algorithm with a time interval of 60 s. The observation times and energy bands are indicated in each image. The image size is 128 $^{\prime \prime }$ $\times$ 128 $^{\prime \prime }$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2128f04a.eps}\hspace*{3mm} \... ...4c.eps}\hspace*{3mm} \includegraphics[width=7cm,clip]{2128f04d.eps} \end{figure}$ Figure 4: Coalignment of RHESSI images of different energy bands and times: a) contour of the image of 25-50 keV at 07:13 UT is superposed on the image of 12-25 keV at 07:13 UT; b) contour of the image of 25-50 keV at 07:21 UT is superposed on the image of 12-25 keV at 07:21 UT; c) contour of the image of 12-25 keV at 07:21 UT is superposed on the image of 12-25 keV at 07:13 UT; d) contour of the image of 25-50 keV at 07:21 UT is superposed on the image of 25-50 keV at 07:13 UT. The RHESSI images are reconstructed from collimators and detectors 3F-8F using the CLEAN image algorithm with a time interval of 60 s. The contour levels of RHESSI image are 60%, 70%, 80%, 90%, and 95% of the maximum value of the image.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{2128f05.eps}\end{figure}$ Figure 5: a)- e) Normalized SOHO/EIT/304 Å images and f) SOHO/EIT/195 Å image. The contours in Frame d) represent the longitudinal magnetic field observed by SOHO/MDI at 07:59:03 UT (the solid line stands for positive field and the dotted for negative field). The letters "R1a'', "R1b'', "R2'' and "R3'' in Frame b) correspond to the H $\alpha$ flare ribbons in Fig. 6f. The observation times and wavelengths are shown in each image. The image size is 286 $^{\prime \prime }$ $\times$ 286 $^{\prime \prime }$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{2128f06.eps} \end{figure}$ Figure 6: Normalized slit-jaw H $\alpha$ images observed by MISS at PMO. The observation times are shown in the upper-left corner of each image. The image size is 170 $^{\prime \prime }$ $\times$ 128 $^{\prime \prime }$ . The letters "R1a'', "R1b'', "R2'', and "R3'' in frame f) mark the H $\alpha$ flare ribbons. Contours in frame f) represent the longitudinal magnetic field observed by SOHO/MDI at 07:59:03 UT (solid line for positive field and dotted line for negative field). The arrows labelled "FL'' and "QS'' in e) indicate the points where we computed the line center intensities shown in Fig. 10 for the flare and quiet sun, respectively. "FL'' corresponds to a point in ribbon R1b.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2128f07a.eps}\hspace*{3mm} \... ...7c.eps}\hspace*{3mm} \includegraphics[width=7cm,clip]{2128f07d.eps} \end{figure}$ Figure 7: RHESSI 25-50 keV image at 07:11-07:12 UT (contour) is superposed on a) EIT/304 Å image at 07:19:34 UT, b) SOHO/MDI magnetogram at 07:59:03 UT, and c) MISS/H $\alpha$ image at 07:23:00 UT. d) EIT/195 Å image at 07:19:23 UT (contour) is superposed on the MISS/H $\alpha$ image at 07:23:00 UT. The contour levels of the RHESSI image are 60%, 70%, 80%, 90%, and 95% of the maximum value of the image.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{2128f08a.ps}\hspace*{3mm} \i... ...e*{4cm}\includegraphics[width=6cm,clip]{2128f08c.ps}\hspace*{4cm}}\end{figure}$ Figure 8: Extrapolated magnetic field lines using the longitudinal magnetic field observed by THEMIS at 09:13:15 UT for the active region NOAA 10484. The THEMIS magnetogram has been inserted in a large MDI map obtained at 09:35:04 UT (303 $^{\prime \prime }$ $\times$ 230 $^{\prime \prime }$ ). The extrapolation was performed in a current-free field configuration. a) observer view, b) radial ( top) view and c) 3D perspective view. The letters "R1a'', "R1b'', "R2'', and "R3'' indicate the locations of the H $\alpha$ flare ribbons. Thick lines indicate the lines where the change of connectivity is drastic.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{2128f09.eps} \end{figure}$ Figure 9: Profiles of a) H $\alpha$ , b) Ca II 8542 Å, and c) He I 10 830 Å lines observed by MISS at 07:11:14 UT. The solid lines stand for the profiles in the flaring region (marked "FL'' (in the ribbon R1b) in Fig. 6e) and dotted lines for those in the nearby quiet region (marked "QS'' in Fig. 6e).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{2128f10.eps} \end{figure}$ Figure 10: Temporal evolution of the line-center intensities of H $\alpha$ , Ca II 8542 Å, and He I 10 830 Å lines observed by MISS at PMO for the point indicated in Fig. 6e by the arrow labelled "FL''. The symbols $+, \diamondsuit , \triangle$ stand for the observed line-center intensities of H $\alpha$ , Ca II 8542 Å, and He I 10 830 Å, respectively, and the corresponding solid lines for the smoothed ones. The horizontal short bars on the left side of the plot indicate the line-center intensities of the three lines observed in the nearby quiet-sun region (marked "QS'' in Fig. 6e). Also plotted is the RHESSI 25-50 keV light curve.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=13.8cm,clip]{2128f11a.eps}\par\vspace*... ...\par\vspace*{3mm} \includegraphics[width=13.8cm,clip]{2128f11d.eps} \end{figure}$ Figure 11: RHESSI spectral fit results for data retrieved from collimators and detectors 1F, 3F-6F and 8F-9F with a 20 s time interval. The energy range is set to 12-80 keV for 07:06:00-07:22:00 UT and 12-60 keV for other times. The background order is taken to be 1 for 3-50 keV and 3 for energy ranges higher than 50 keV. Time profiles of the broken energy ( left of the first panel) and normalization factor ( right of the first panel) from the fitting with the "vth+bpow'' method (cf. Sect. 4.1). The second panel shows the fitted photon spectra with this model for the time interval of 07:11:00-07:11:20 UT ( left) and 07:21:00-07:21:20 UT ( right). The third and the fourth panels are the same as the second panel but with the "vth+thin'' and "vth+thick'' model, respectively (please see the text in Sect. 4.1 for details about the models).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2128f12a.eps}\includegraphics[width=8.3cm,clip]{2128f12b.eps} \end{figure}$ Figure 12: Time profile of a) temperature and b) emission measure derived from GOES-10 (solid line) and RHESSI spectral analysis with "vth+thin'' (dashed line) and "vth+thick'' (dotted line) model.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2128f13a.eps}\hspace*{4mm} \includegraphics[width=7.5cm,clip]{2128f13b.eps} \end{figure}$ Figure 13: a) Temporal variations of thermal energy ( $E_{\rm th}$ , thick line) and non-thermal energy ( $E_{\rm nth}$ , thin line) computed from the fit parameters with the "vth+thick'' (solid line) and "vth+thin'' models (dashed line). b) Time profile of the ratio of non-thermal energy to thermal energy ( $R_{\rm e}$ ) for the studied flare calculated from RHESSI spectral analysis with the "vth+thick'' (solid line) and "vth+thin'' (dashed line) models. The low energy cutoff for the non-thermal electron beam was set to 25 keV based on our estimation. The mean lifetime of non-thermal electrons is set to 1 s.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{2128f03.eps} \end{figure}$	Figure 3: A selection of reconstructed RHESSI images (not normalized) from collimators and detectors 3F-8F using the CLEAN image algorithm with a time interval of 60 s. The observation times and energy bands are indicated in each image. The image size is 128 $^{\prime \prime }$ $\times$ 128 $^{\prime \prime }$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{2128f09.eps} \end{figure}$	Figure 9: Profiles of a) H $\alpha$ , b) Ca II 8542 Å, and c) He I 10 830 Å lines observed by MISS at 07:11:14 UT. The solid lines stand for the profiles in the flaring region (marked "FL'' (in the ribbon R1b) in Fig. 6e) and dotted lines for those in the nearby quiet region (marked "QS'' in Fig. 6e).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{2128f12a.eps}\includegraphics[width=8.3cm,clip]{2128f12b.eps} \end{figure}$	Figure 12: Time profile of a) temperature and b) emission measure derived from GOES-10 (solid line) and RHESSI spectral analysis with "vth+thin'' (dashed line) and "vth+thick'' (dotted line) model.
Open with DEXTER