Japan Geoscience Union Meeting 2014

Presentation information

Print

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)

9:45 AM - 10:00 AM

[PEM08-11] Lower temperature response of an EUV wave observed by Hinode/EIS and SDO/AIA

*Kyoung sun LEE1, Ryun young KWON2, David BROOKS2, Toshifumi SHIMIZU1 (1.ISAS/JAXA, 2.George Mason University)

Keywords:Spectroscopy, Corona, EUV wave

We investigate an EUV wave observed by Hinode/EIS and SDO/AIA on 2011 August 04. The EUV wave propagates across the solar disk and the wave front passing through a remote active region (AR 11263) is observed by EIS. This EUV wave has already been analyzed using coronal lines, but the lower temperature response to the EUV wave has not been investigated. Using multi-wavelength observations from EIS and AIA, we determined the intensity and Doppler velocity variation of different temperature lines and compared them. From the comparison, we found an enhancement of the intensity at lower temperatures before the intensity increase seen in the coronal filters of AIA. And a significant enhancement of the red shift (10 km/s) in the lower temperature line (Si VII, log T ~ 5.8) compared to the increase of the red shift (~3 km/s) in coronal lines (Fe XII, FeXIII, and Si X, log T ~ 6.1-6.2) when the EUV wave interacts with the active region. We will discuss the impact of the EUV wave on the lower temperature emission.