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)

9:30 AM - 9:45 AM

[PEM08-10] An energetics study of X-ray jets using Hinode/XRT observation

*Nobuharu SAKO1, Masumi SHIMOJO2, Tetsuya WATANABE2, Takashi SEKII2 (1.The Graduate University for Advanced Studies, 2.National Astronomical Observatory of Japan)

Keywords:Sun, Solar Corona, X-ray jet, Energy release, Hinode

For plasma acceleration in X-ray jets in the solar corona, three mechanisms have been considered, based on the model of X-ray jets by magnetic reconnection (Shibata et al. 1992); The reconnection jet produced by magnetic tension, the evaporation flow produced by pressure gradient, and the twisted jet produced by magnetic pressure. There are some evidences of X-ray jets in active regions (ARs) produced by pressure gradient. On the other hands, there is no observational evidence of X-ray jets by the other forces except the result of a high-speed jet. In order to distinguish the evaporation flow from the other types of jets, I have studied the energetics of the X-ray jets.Using over 100 X-ray jets greater than 3×104 km in length in ARs, quiet regions (QRs), and coronal holes (CHs), I have found no large differences in the life time, the width of the jets, and the area of the footpoint flares in such regions. On the other hands, the plasma number density of the X-ray jets and flares in ARs is ten times larger than those in QRs and CHs. Assuming the energy balance between conductive flux and heat flux by the footpoint flare, we estimate the temperature of the jets. The AR jets has a wide range of the temperature (1 MK-9 MK), while the temperature of most X-ray jets in CH and QR is 1〜2 MK. In my presentation, I will discuss a relationship of the speed with the temperature of the jets.