Japan Geoscience Union Meeting 2014

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International Session (Oral)

Symbol P (Space and Planetary Sciences) » P-EM Solar-Terrestrial Sciences, Space Electromagnetism & Space Environment

[P-EM08_2AM1] Space Weather and Space Climate

Fri. May 2, 2014 9:00 AM - 10:45 AM 411 (4F)

Convener:*Ryuho Kataoka(National Institute of Polar Research), Yusuke Ebihara(Research Institute for Sustainable Humanosphere, Kyoto University), Kanya Kusano(Solar-Terrestrial Environment Laboratory, Nagoya University), Toshifumi Shimizu(Institute of Space and Astronautical Science, JAXA), Yoshizumi Miyoshi(Solar-Terrestrial Environement Laboratory, Nagoya University), Ayumi Asai(Unit for Synergetic Studies of Space, Kyoto University), Tatsuhiko Sato(Japan Atomic Energy Agency), Hidekatsu Jin(National Institude of Information and Communications Technology), Kiminori Itoh(Graduate School of Engineering, Yokohama National University), Hiroko Miyahara(College of Art and Design, Musashino Art University), Chair:Toshifumi Shimizu(Institute of Space and Astronautical Science, JAXA)

10:00 AM - 10:15 AM

[PEM08-12] Imaging, spectroscopic and stereoscopic observations of the bi-directional inflow in the solar flare

*Yuki MATSUI1, Takaaki YOKOYAMA1 (1.University of Tokyo)

Keywords: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 FeXXIV 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.