Downflow as a Reconnection Outflow Ayumi ASAI Kwasan and Hida Observatories, Kyoto University The 5th Solar-B Science Meeting Nov. 12-14, 2003@Tokyo Abstract 1. Introduction Downflow Yohkoh (SXT) has found downflows above postflare loops McKenzie and Hudson 1999; McKenzie 2000 velocity: 45–500 km/s dark feature often seen in the decay phase of LDEs Recently TRACE also has found the downflows above postflare loops Innes et al. 2003a; b  We can examine such TRACE downflows with much higher spatial resolution than before. We present a detailed examination about the evolution of TRACE downflows (sunward motions) seen above postflare loops. We also propose an observation of downflows by Solar-B. downflows observed in the 2000 January 21 flare (Yohkoh/SXT) 2. Data 4. Observation of Downflows by Solar-B/EIS NOAA 0039 Flare 2002-July-23 00:15UT GOES X4.8 NOAA 0039 (Southeast limb) Data EUV…TRACE (195Å) HXR...RHESSI microwave…Nobeyama Radioheliograph Emission Measure 1.  ~ a few×1027 cm-5 FOV & Cadence near the solar limb, 104~105 km above a flare loop  depends on the size of a flare downflows sun flare slit full disk image (Ha) of the flare (Sartorius Telescope) example of the observation FOV 1 slit position (fixed) red thick line slit scan (red box) ~ 50 arcsec width Cadence 5 second or less ~ 60 second Time slice image 3. Results slit A TRACE 195A Velocity 100 – 250 km/s ~previous results Time These TRACE downflows are seen not only in the decay phase but also in the impulsive phase and main phase Timing Down flows appear when microwave/HXR bursts occur. slit A Resolution Size of downflows (> 2000 km; 3 arcsec) must be resolved. Others Co-observation with XRT is needed (to follow the features of high-temperature plasma region) Downflows start to be seen 5~10 min after the beginning of a flare. We can adjust the slit to the proper position just AFTER a flare occurs. slit B slit B NoRH 17GHz RHESSI 50-100keV GOES flux NoRH 17GHz NoRH 34GHz 00:00 01:00 02:00 5. Summary light curve of the flare The downflows occurred when strong magnetic energy was released. These results show that they are correlated with the reconnection outflows. We found that the downflows are seen not only in the decay phase but also in the impulsive and main phases of flares. We also found that the times when the downflow motions are seen correspond to those of the bursts of nonthermal emissions in hard X-ray and microwave. The downflows occurred when strong magnetic energy was released and that they are correlated with the reconnection outflows. The observation of downflows with Solar-B may help to explain what the downflows are. Temperature & Density super-hot, low-density plasma…1 (Previous Woks with SXT, SUMER) T: 0.8~2･107 [K] n: ~109 [cm-3 ] (supra-hot plasma …2) T: >2･107 [K] plasmoid ejection downflows model of the magnetic reconnection