On the Stark Broadening of Ar XV Spectral Lines (original) (raw)

On the Stark Broadening of Visible Ar I Lines for Astrophysical Plasma Analysis and Modelling

Stark broadening parameters (width and shift) of Ar I 696.5 nm spectral line have been calculated within the semi-classical perturbation ap-proach and presented here as a part of our investigation of Ar I 522.1, 549.6, 518.6, 603.2, 560.7 and 696.5 nm lines corresponding to the transitions 3p 5 nd -3p 5 4p for n = 7-5 and 4p' -4s. The considered lines are in the optical part of the spectrum which is particularly interesting for astrophysics. Results obtained are compared with available experimental and theoretical data. The validity of impact approximation for ion perturbers is considered as well.

Semiclassical Stark Broadening Parameters of Ar VII Spectral Lines

Using the semi-classical perturbation approach in the impact approximation, full width at half maximum and shift have been determined for eight spectral lines of Ar VII, for broadening by electron-, proton-, and He III-impacts. The results are provided for temperatures from 20,000 K to 500,000 K, and for an electron density of 10 18 cm −3. The obtained results will be included in the STARK-B database, which is also in the virtual atomic and molecular data center (VAMDC).

ON THE STARK BROADENING OF Ar VII SPECTRAL LINES

Stark broadening parameters, full wi dth at half maxi mum of s pectral line and shift, have been calculated for 3 spectral lines of Ar VII, for broadening by electron, proton, and He III i mpacts. For calculations, the semiclassical perturbation approach in the impact approxi mation has been used. The results are provi ded for temperatures from 20 000 K to 500 000 K and for an electron density of 10 17 cm-3. Obtained results will be included in the STARK-B database which is also included in Virtual atomic and molecular data center (VAMDC).

Quantum Stark broadening data for Ar viii and Ar ix lines

Monthly Notices of the Royal Astronomical Society, 2019

We present in this paper quantum Stark broadening data for 14 Ar VIII and 16 Ar IX lines. For the Ar VIII ion, we compare our results to those calculated using the semiclassical method and we find an acceptable agreement. We performed also a comparison between the importance of Stark and Doppler broadening in the atmospheric conditions of DO white dwarfs. To the best of our knowledge, the Stark widths provided for the Ar IX ion are new, and no results have been found in the literature to compare with. We present some of the atomic radiative data used in our broadening calculations, and we compare them to other results. The comparison shows an acceptable agreement. Our results come to fill the lack of line broadening data necessary in stellar spectroscopy and plasma analysis.

STARK BROADENING IN ASTROPHYSICS

Significance for astrophysical plasma research and modelling of broadening of spectral lines by collisions with charged particles, or Stark broadening, is considered and analyzed here, as well as the corresponding applications of Stark broadening data.This line broadening mechanism is particularly of interest e.g. for the research of white dwarfs and hot stars of A and B type, and for the analysis and synthesis of their spectra. For example, a large number of data is needed for calculations of stellar opacities and modeling and investigation of stellar atmospheres. Data on Stark broadening of spectral lines are also important for diagnostics and research of laboratory, fusion, laser produced and technological plasmas. Also, we will review and consider some results of Stark broadening research on Belgrade Astronomical observatory, as well as the organization of Stark broadening data in STARK-B database, a part of VAMDC (Virtual Atomic and Molecular Data Center).

Stark broadening parameters of Ar II and Ar III lines: Comparison of semiclassical calculations

Journal of Quantitative Spectroscopy & Radiative Transfer, 2021

For many applications, the semiclassical, theoretical calculations of Stark broadening parameters of isolated non-hydrogenic ion lines proved useful and reasonably accurate for plasma electron density determination. Several attempts were carried out to improve the calculation procedure of Stark broadening parameters and, in this way, to increase the accuracy of laboratory and astrophysical plasmas and opacity calculations. In this work for the test ions, we selected singly and doubly ionized argon lines. These ions are chosen for several reasons. First, among several studies, there are detailed Ar II calculations by Griem and coworkers, Hamdi et al., and by Blagojevi ć and Konjevi ć for singly and Hamdi et al.for doubly ionized argon lines. These large sets of data facilitate the extension of our work on improving semiclassical calculations. Second, argon gas applications as a plasma matrix are numerous, and reliable plasma diagnostics are of utmost importance for determining electron density, one of the essential plasma parameters for plasma modeling.

On the Stark broadening of Cr VI spectral lines in astrophysical plasma

Stark broadening parameters for Cr VI lines have been calculated using semiclassical perturbation method for conditions of interest for stellar plasma. Here are presented, as an example of obtained results, Stark broadening parameters for electron-and proton-impact broadening for Cr VI 4s 2 S-4p 2 P o λ = 1430Å and Cr VI 4p 2 P o-5s 2 S λ = 611.8 ˚ A multiplets. The obtained results are used to demonstrate the importance of Stark broadening of Cr VI in DO white dwarf atmospheres. Also the obtained results will enter in STARK-B database which is included in Virtual Atomic and Molecula Data Center-VAMDC.

On the semiclassical perturbation Stark shifts of Ar II spectral lines

Contributions of the Astronomical Observatory Skalnaté Pleso, 2020

We present in this paper Stark shifts as a function of temperature for 20 spectral lines of Ar II belonging to 4p-4d transition array. Calculations are made using semiclassical perturbation approach in impact approximation. Atomic data used in this calculation are carried out using Hartree-Fock method with relativistic corrections. Singly charged argon (Ar II) spectral lines are observed in many astrophysical plasmas. Ar II spectral lines are also important for laboratory plasmas and laser physics and technology.

Quantum and Semiclassical Stark Widths for Ar VII Spectral Lines

Atoms

We present in this paper the results of a theoretical study of electron impact broadening for several lines of the Ar VII ion. The results have been obtained using our quantum mechanical method and the semiclassical perturbation one. Results are presented for electron density 10 18 cm −3 and for electron temperatures ranging from 2 × 10 4 to 5 × 10 5 K required for plasma modeling. Our results have been compared to other semiclassical ones obtained using different sources of atomic data. A study of the strong collisions contributions to line broadening has been performed. The atomic structure and collision data used for the calculations of line broadening are also calculated by our codes and compared to available theoretical results. The agreement found between the two calculations ensures that our line broadening procedure uses adequate structure and collision data.

STARK BROADENING OF SEVERAL Ar I SPECTRAL LINES IN THE VISIBLE SPECTRUM

Baltic astronomy an international journal

In order to complete data on Stark broadening parameters for Ar I line in the visible spectrum, we determined Stark widths and shifts due to electron, proton and ionized helium impacts, for nine lines (4191.0, 4259.4, 5912.1, 6043.2, 6045.0, 6752.9, 7503.9, 7514.6, 7724. A), using jK coupling and semiclassical-perturbation theory. The obtained results will enter the STARK-B database, which is a part of the Virtual Atomic and Molecular Data Center.