Stark Broadening of in III Lines in Astrophysical and Laboratory Plasma

TL;DR

This paper investigates Stark broadening of In III spectral lines in astrophysical and laboratory plasmas using the semiclassical perturbation method, providing parameters crucial for stellar atmosphere analysis and database inclusion.

Contribution

It presents new Stark broadening parameters for In III lines calculated with the semiclassical perturbation method, relevant for astrophysical plasma diagnostics.

Findings

Stark widths are comparable to or larger than Doppler widths in hot star atmospheres.

Results agree with existing experimental data.

Parameters will be added to the STARK-B database.

Abstract

Besides the need of Stark broadening parameters for a number of problems in physics, and plasma technology, in hot star atmospheres the conditions exist where Stark widths are comparable and even larger than the thermal Doppler widths. Using the semiclassical perturbation method we investigated here the influence of collisions with charged particles for In III spectral lines. We determined a number of Stark broadening parameters important for the investigation of plasmas in the atmospheres of A-type stars and white dwarfs. Also, we have compared the obtained results with existing experimental data. The results will be included in the STARK-B database, the Virtual Atomic and Molecular Data Center and the Serbian Virtual Observatory.