Japan Geoscience Union Meeting 2015

Presentation information

International Session (Oral)

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

[P-EM07] Space Weather, Space Climate, and VarSITI

Mon. May 25, 2015 2:15 PM - 4:00 PM 302 (3F)

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

3:30 PM - 3:45 PM

[PEM07-24] Two-dimensional simulation of the small scale structure in the solar chromosphere

*Haruhisa IIJIMA1, Takaaki YOKOYAMA1 (1.Department of Earth and Planetary Science, Graduate School of Science, The University of Tokyo)

Recent observation revealed the highly dynamic and fine structures in the solar chromosphere. The solar chromosphere is known to have wide range of the plasma beta, high nonlinearity with shock waves, cooling from the radiation, thermal conduction by the non-thermal electron, and weak ionization rate. All of the processes above have opportunity contributing to the dynamics of the solar chromosphere. In order to get the proper interpretation of the observation in the solar chromosphere, the numerical simulation with the various effects can be very useful tool. In our study, a new radiative magnetohydrodynamic code is developed for the dynamical simulation of the solar chromosphere. The numerical domain includes the upper part of the convection zone to the lower part of the corona. The convective motion as a driver of the dynamics in the upper atmosphere is consistently modeled using the radiative transfer calculation and the realistic equation of state. The thermal conduction from the non-thermal electron is also included. In this talk, we will report the numerical implementation from this numerical code and the first results filled with small scale structures in the two-dimensional domain.