High-Resolution Laboratory Measurements of M-shell Fe EUV Line Emission using EBIT-I

TL;DR

This paper presents high-resolution laboratory measurements of Fe M-shell EUV lines using EBIT-I, aiding in the identification of spectral lines crucial for solar corona diagnostics and improving existing spectroscopic databases.

Contribution

It provides unambiguous charge state identification of Fe lines in the 238-258 Å range, including previously unidentified lines, enhancing solar spectral modeling accuracy.

Findings

Identification of charge states for Fe IX and Fe X lines.

Measurement of key density diagnostic line ratios.

Discovery of new Fe X lines for database updates.

Abstract

Solar physicists routinely utilize observations of Ar-like Fe IX and Cl-like Fe X emission to study a variety of solar structures. However, unidentified lines exist in the Fe IX and Fe X spectra, greatly impeding the spectroscopic diagnostic potential of these ions. Here, we present measurements using the Lawrence Livermore National Laboratory EBIT-I electron beam ion trap in the wavelength range 238-258 A. These studies enable us to unambiguously identify the charge state associated with each of the observed lines. This wavelength range is of particular interest because it contains the Fe IX density diagnostic line ratio 241.74 A/244.91 A, which is predicted to be one of the best density diagnostics of the solar corona, as well as the Fe X 257.26 A magnetic-field-induced transition. We compare our measurements to the Fe IX and Fe X lines tabulated in CHIANTI v10.0.1, which is used for modeling the solar spectrum. In addition, we have measured previously unidentified Fe X lines that will need to be added to CHIANTI and other spectroscopic databases.