Japan Geoscience Union Meeting 2019

Presentation information

[J] Poster

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

[P-EM19] Frontiers in the solar physics

Sun. May 26, 2019 5:15 PM - 6:30 PM Poster Hall (International Exhibition Hall8, Makuhari Messe)

convener:Shinsuke Imada(Institute for Space-Earth Environmental Research, Nagoya University), Takaaki Yokoyama(School of Science, University of Tokyo), Toshifumi Shimizu(Institute of Space and Astronautical Science, JAXA), Yukio Katsukawa(National Astronomical Observatory of Japan, National Institute of Natural Sciences)

[PEM19-P05] Stellar flare of a close binary system monitored by the Hisaki satellite during the NICER-Hisaki Observing Campaign 2018-2019

*Tomoki Kimura1, Wataru Iwakiri2, Atsushi Yamazaki3, Go Murakami3, Fuminori Tsuchiya4, Kazuo Yoshioka5, Shin Toriumi6, Hajime Kita3, Masaki Kuwabara3 (1.Frontier Research Institute for Interdisciplinary Sciences, Tohoku University, 2.Faculty of Science and Engineering, Chuo University, 3.Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 4.Planetary Plasma and Atmospheric Research Center, Tohoku University, 5.Department of Complexity Science and Engineering, University of Tokyo, 6.National Astronomical Observatory of Japan)

Keywords:stellar flare, Hisaki

Dynamics of stellar flare is still not well understood compared to that of the sun because of lack of continuous monitoring of distant stars in multiple wavelengths. Here we present a flare event at a close binary system, UX Arietis, monitored with the planetary extreme ultraviolet (EUV) space telescope Hisaki during the coordinated observing campaign with the NICER X-ray Telescope from late 2018 to early 2019. Time variability in the EUV spectrum of the binary was successfully monitored from the begging to the end of flare. Emission power at the EUV wavelengths peaked at ~6x10^24 W, which is comparable with that measured in the previous X-ray observations by e.g., the Advanced Satellite for Cosmology and Astrophysics (ASCA) (Gudel et al., 1999). The EUV spectrum showed emission lines of carbon, nitrogen, oxygen, and silicon ions. Electron temperature and density, emission measure, and ion balance were reduced from the emission lines by EUV spectral diagnostics. Dynamics of the stellar flare will be discussed based on comparison of the reduced plasma parameters with the X-ray spectrum measured with NICER.