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)

9:15 AM - 9:30 AM

[PEM08-09] Spatial distribution of nonthermal electrons in an X-class flare on 13 May 2013

*Satoshi MASUDA1 (1.STEL, Nagoya Univeristy)

Keywords:solar flare, particle acceleration, microwave, hard X-ray, solar corona, magnetic recconection

Four X-class flares took place in May 2013. Fortunately three of four were observed with Nobeyama Radioheliograph (NoRH). One of them occurred behind the east limb on 13 May 2013. It is a good chance to investigate the height distribution of nonthermal electrons in the solar corona. In the framework of the standard flare model based on magnetic reconnection, Minoshima et al. (2011) showed that the height distribution of accelerated/heated electrons depends on the energy of the electrons. NoRH has a capability to observe a solar flare in 17 and 34 GHz with a high time resolution (100 ms). The energy of electrons emitting microwaves is very high (~ MeV), and the mean-energy emitting 34 GHz is higher than that for 17 GHz. Hard X-rays are emitted by relatively lower-energy (~ 100 keV) electrons. So this dataset can cover a wide energy range of accelerated electrons. In order to understand the electron acceleration/transport/loss processes, multi-wavelength observation is crucially important. The 13 May 2013 flare was simultaneously observed with NoRH and RHESSI (The Reuven Ramaty High Energy Solar Spectroscopic Imager). Investigating the distribution of these emission sources in the solar corona, we discuss the electron acceleration/transport/loss processes.