Zoran Simić

Stark broadening of neutral germanium spectral lines

Stark broadening of the eleven transitions of neutral germanium within the 4p 4p5s transition array has been analyzed within the frame of the semiclassical perturbation method. Obtained results have been compared with available experimental and theoretical data. The importance of the electron-impact broadening in the case of the 4226.562 A line for A star atmospheres has been tested

Stark broadening of B iv spectral lines

Stark broadening parameters for 157 multiplets of helium like boron (B IV) have been calculated using the impact semiclassical perturbation formalism. Obtained results have been used to investigate the regularities within spectral series. An example of the influence of Stark broadening on B IV lines in DO white dwarfs is given.

Stark broadening data for spectral lines of rare-earth elements: Nb III ☆

Abstract The electron-impact widths for 15 doubly charged Nb ion lines have been theoretically determined by using the modified semiempirical method. Using the obtained results, we considered the influence of the electron-impact mechanism on line shapes in spectra of chemically peculiar stars and white dwarfs.

STARK BROADENING AND WHITE DWARFS

Abstract White dwarf and pre-white dwarfs are the best types of stars for the application of Stark broadening research results in astrophysics, since in the atmospheres of these stars physical conditions are very favorable for this line broadening mechanism - in hot hydrogen-deficient white dwarfs and pre-white dwarfs Teff = 75 000–180 000 K and log g = 5.5–8 [cgs]. Even for much cooler DA and DB white dwarfs with the typical effective temperatures 10 000-20 000 K, Stark broadening is usually the dominant broadening mechanism. In this review, Stark broadening in white dwarf spectra is considered, and the attention is drawn to the STARK-B database (http://stark-b.obspm.fr/), containing the parameters needed for analysis and synthesis of white dwarf spectra, as well as for the collective efforts to develop the Virtual Atomic and Molecular Data Center.

Stark broadening of B IV lines for astrophysical and laboratory plasma research

Abstract Stark broadening parameters for 36 multiplets of B IV have been calculated using the semi-classical perturbation formalism. Obtained results have been used to investigate the regularities within spectral series and temperature dependence.

Stark Broadening of In III Lines in Astrophysical and Laboratory Plasma

Abstract In the deeper layers of hot stellar photospheres the Stark widths of spectral lines can be comparable and even larger than the thermal Doppler widths. Using the semiclassical perturbation method, we investigate the influence of the collisions with charged particles for the In III lines. We determine a number of Stark broadening parameters important in the atmospheres of A-type stars and white dwarfs. Also, the obtained results are compared with the available experimental data. The results will be included in the STARK-B database, the Virtual Atomic and Molecular Data Center and the Serbian Virtual Observatory.

Stark Broadening of Several Ne II, Ne III and O III Spectral Lines for the Stark-B Database

Abstract In order to complete Stark broadening data for Ne II and O III lines, needed for analysis of stellar atmospheres, we determined the missing parameters for the broadening by collisions with protons and ionized helium for 15 Ne II and 5 O III multiplets. Also, electron, proton and ionized helium impact broadening parameters for an important Ne II multiplet in the visible part of the spectrum and for three Ne III multiplets were calculated. The obtained data will be included in the STARK-B database, which is a part of the Virtual Atomic and Molecular Data Center.

Te I Stark Broadening Data for Stellar Plasma Analysis

In spite of the fact that tellurium is one of the least abundant element in the Earths litosphere, its cosmic abundance is larger than for any element with atomic number greater than 40, and its spectral lines are observed in stellar spectra. Since the significance of trace element spectral data, including Stark broadening parameters, increases with the development of space‐born spectroscopy, we investigate here theoretically the influence of collisions with charged particles on spectral lines of neutral tellurium. By using the semiclassical perturbation method, Stark widths and shifts of three Te I spectral lines, of interest for modellisation, investigation and diagnostic of stellar plasma have been obtained. Results were applied for the investigation of the influence of Stark broadening mechanism in ultraviolet, optical and infrared part of the spectrum of A‐type star atmospheres. The obtained results demonstrate that, in the considered case, Stark broadening is more important in optical and infrared,...

Serbian virtual observatory

The work on SerVO - Serbian virtual observatory (http://servo.aob.rs/~darko) started in 2008, with aims 1) To establish SerVO and join the EuroVO - European Virtual Observatory and IVOA - Inetrnational Virtual Observatory Alliance; 2) To create SerVO data Center for digitalization and archiving in VO format photo-plates from Belgrade Astronomical Observatory and other astronomical results obtained by the staff; 3) To develop the tools for visualization of data; 3) To develop together with Observatoire de Paris, STARK-B - database containing as the first step Stark widths and shifts of spectral lines, determined within the semiclassical perturbation approach by two of us (MSD-SSB) and to create a mirror site in Belgrade; 4) To make a mirror site for DSED (Darthmouth Stellar Evolution Database) in which development took part one of us (DJ). An additional aim is the creation of VAMDC (Virtual Atomic and Molecular Data Center) AOB (Astronomical Observatory of Belgrade) Node, and a recent objective is the collaboration with the Large Synoptic Telescope (LSST) project. In this contribution SerVO project is reviewed within the context of e-science in Astronomy -- Astroinformatics.

Stark Broadening of Several Ar I Spectral Lines in the Visible Spectrum

Abstract 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, 7724.2 Å), 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.