Plasma and Fusion Research

Volume 18, 2401041 (2023)

Regular Articles

Measurement of L-Shell Emission from Iron-Group Elements for High-Resolution X-Ray Spectroscopy in Future Astronomy
Yuken OHSHIRO1,2), Tomoko KAWATE3,4), Hiroya YAMAGUCHI2,1) and Izumi MURAKAMI3,4)
1)
Department of Physics, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
2)
Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency (JAXA), 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan
3)
National Institute for Fusion Science, National Institutes of Natural Sciences, 322-6 Oroshi-cho, Toki, Gifu 509-5292, Japan
4)
Department of Fusion Science, The Graduate University for Advanced Studies, SOKENDAI, 322-6 Oroshi-cho, Toki, Gifu 509-5292, Japan
(Received 9 January 2023 / Accepted 23 March 2023 / Published 22 June 2023)

Abstract

Measuring abundance of iron-group elements (IGEs; Cr, Mn, Fe, and Ni) is essential for understanding astrophysical phenomena such as supernovae. The L-shell emissions from IGEs will soon be resolved by next-generation X-ray satellites, enabling more accurate measurements of abundance. However, theoretical calculations for these L-shell transitions have not been sufficiently validated using experimental work. Herein, large helical device (LHD) experiments that measured L-shell emission from Ni and Mn are reported. The temporal evolution of LHD plasma is characterized by three phases, each of which resolves different L-shell emissions. We modeled EUV-Short spectra considering LHD plasma structure with AtomDB, an atomic database widely used in the X-ray astronomy community. We discovered that the observed intensity ratios of the 3C (2p53d1 1P1 → 2p6 1S0) to 3D (2p53d1 3D1 → 2p6 1S0) transition of Ne-like ions are 0.4 - 0.6 times lower than the theoretically predicted ratios.

Keywords

EUV spectroscopy, line identification, intensity ratio, nickel, manganese

DOI: 10.1585/pfr.18.2401041

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