Forty Years of the Applications of Stark Broadening Data Determined with the Modified Semiempirical Method

Abstract

The aim of this paper is to analyze the various uses of Stark broadening data for non-hydrogenic lines emitted from plasma, obtained with the modified semiempirical method formulated 40 years ago (1980), which are continuously implemented in the STARK-B database. In such a way one can identify research fields where they are applied and better see the needs of users in order to better plan future work. This is done by analysis of citations of the modified semiempirical method and the corresponding data in international scientific journals, excluding cases when they are used for comparison with other experimental or theoretical Stark broadening data or for development of the theory of Stark broadening. On the basis of our analysis, one can conclude that the principal applications of such data are in astronomy (white dwarfs, A and B stars, and opacity), investigations of laser produced plasmas, laser design and optimization and their applications in industry and technology (ablation, laser melting, deposition, plasma during electrolytic oxidation, laser micro sintering), as well as for the determination of radiative properties of various plasmas, plasma diagnostics, and investigations of regularities and systematic trends of Stark broadening parameters.

Stark broadening of Pd II spectral lines

“…Here are presented results of calculations of Stark full widths at half intensity maximum (FWHM) of spectral lines of ionized palladium (Pd II), by using the modified semiempirical method [25,32]. Atomic energy levels of ionized palladium, needed for present calculations, have been taken from [33,34].…”

Stark Width Data for Tb II, Tb III and Tb IV Spectral Lines

“…Of course, these data may be of interest for laboratory plasma diagnostics and for investigations of laser produced plasma and lasers. A detailed analysis of the usage of published Stark broadening data was published in [19,20].…”

Quantum mechanical line widths of ionized oxygen, silicon, and aluminium; comparisons with recent experimental results

“…Among the line broadening mechanisms, the Stark broadening ★ Email: haelabidi@uqu.edu.sa -resulting from the action of electric field of particles surrounding an emitter-is the most important. There are two origins of this importance: firstly, because Stark broadening occurs for various physical conditions of plasma, especially for astrophysical plasmas: from clouds of interstellar molecular hydrogen, with temperatures around 30 K and electron densities 𝑁 𝑒 = 1−5 cm −3 (conditions that cannot be obtained in laboratory plasmas) to white dwarf atmospheres and hot stars of A and B types with temperature about 10 5 K and density 𝑁 𝑒 = 10 17 cm −3 (Dimitrijević 2020). The reader can find in Dimitrijević (2003) a set of extremely different plasma conditions for which Stark broadening cannot be neglected.…”