10:00 〜 10:15
[PEM08-12] 太陽フレア双方向インフローの撮像分光立体観測
キーワード：solar flare, reconnection
The standard model of solar flares based on the magnetic reconnection includes bi-directional inflow toward the reconnection point. Corresponding to the bi-directional inflow, high temperature loops like a cusp shape are formed due to the magnetic reconnection. By combination of imaging, spectroscopic and stereoscopic observations, we succeeded in capture the three-dimensional structure of a bi-directional reconnection inflow of a solar flare.We analyzed a C-class flare that occurred on 2012 September 11 beyond the solar limb. The bi-directional inflow was found in the images of coronal temperature filter taken by AIA onboard SDO. Hinode EUV Imaging Spectrometer (EIS) also observed this flare and provide the Doppler velocity of the bi-directional inflows. At the same time, cusp loops were observed with the raster scans of FeIV emission line (over 10 MK) at the region surrounded by the bi-directional inflow. This is clear evidence that 1MK loops are heated over 10MK by the magnetic reconnection. STEREO A/SECCHI was observing this flow from a different line of site. Inflowing angle in STEREO A/SECCHI images is consistent with the angle speculated by apparent velocity of SDO/AIA and line of sight velocity of Hinode/EIS. By combining these data sets, we constructed a self-consistent three-dimensional picture of the flows.