The electron-impact broadening parameters for Co III spectral lines

Tankosic, D.; Popović, L. Č.; Dimitrijević, M. S.

doi:10.1051/0004-6361:20021801

Cited by 26 publications

(22 citation statements)

References 11 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The atomic data of electronimpact broadening for line synthesis are needed to solve various problems in astrophysics, such as for determining the chemical abundance of elements and also for estimating radiative transfer through stellar plasmas, as well as for opacity calculations. The collisional broadening coefficients may also be important in the case of cooler stars, such as solar type stars, for transitions involving higher principal quantum numbers (Tankosić et al 2003, and references therein).…”

Section: Introductionmentioning

confidence: 99%

Electron-impact broadening parameters for Be II, Sr II, and Ba II spectral lines

Duan

Bari

et al. 2013

A&A

View full text Add to dashboard Cite

Aims. We present results of the electron-impact broadening parameters (i.e., widths and shifts) of spectral lines in singly ionized Be II, Sr II, and Ba II ions, calculated by using our relativistic quantum mechanical methods. Methods. In these calculations, Dirac R-matrix methods were used to solve (N + 1)-electron colliding systems to obtain the required scattering matrices. The dimensionless collision strength Ω(ε) is calculated as a function of incident electron energies ε.Results. The present line-broadening parameters are required for future spectral analysis by means of state-of-the-art nonlocal thermodynamic equilibrium atmospheres, which is now hampered largely by the paucity of reliable atomic and accurate line-broadening data tables. Our results for the spectral line-broadening parameters in the case of three ions obtained for a set of electron temperatures at an electron density 10 17 cm −3 show very good agreement with other theoretical calculations, and are much closer to the available experimental measurements.

show abstract

Section: Introductionmentioning

confidence: 99%

Electron-impact broadening parameters for Be II, Sr II, and Ba II spectral lines

Duan

Bari

et al. 2013

A&A

View full text Add to dashboard Cite

show abstract

“…Spectral lines of highly charged chromium ions, including Cr VI, have been observed in the spectra of white dwarf atmospheres where, as it has been demonstrated several times [12,13,14,15,16,17,18,19,20,21,10], Stark broadening is usually dominant line broadening mechanism. With the results obtained here, we also wish to demonstrate the importance of Stark broadening in DO white dwarf atmospheres, which effective temperature is within the range 40 000 K < T ef f < 120 000 K.…”

Section: Resultsmentioning

confidence: 99%

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

Dimitrijević

Simić

Sahal‐Bréchot

2017

J. Phys.: Conf. Ser.

View full text Add to dashboard Cite

IntroductionRauch et al. [1] have found Cr V, Cr VI and Cr VII lines in the spectrum of LS V +46o21 white dwarf, which is the central star of planetary nebula Sh 2-216. High-resolution, high-signal to noise ratio ultraviolet spectra obtained by FUSE (Far Ultraviolet Spectroscopic Explorer) and HST/STIS (Space Telescope Imaging Spectrograph aboard the Hubble Space Telescope) have been used. Rauch et al. [1] stated that: Theoretical physics should provide data which cover the astrophysical relevant temperature and density space. Better atomic and line-broadening data will then strongly improve future spectral analyses and thus, make determinations of photospheric properties more reliable.Since the Stark broadening is usually the most important line-broadening mechanism in white dwarf atmospheres (see e.g.[10]), we will calculate, using semiclassical perturbation method [3,4,5], Stark broadening parameters of Cr VI spectral lines, due to collisions with electrons, protons and doubly charged helium ions, the main perturbers in white dwarfs, and an example of the obtained results will be presented here. Calculations will be performed in function of perturber density and temperature, for plasma conditions of interest for white dwarfs.Obtained results will be used to demonstrate the importance of Stark broadening of Cr VI lines for analysis and synthesis of spectra of white dwarfs, using theoretical models of DO white dwarf atmosphere and comparing Stark and Doppler widths in function of optical depth. The obtained Stark broadening parameters of spectral lines, broadened by electron-, proton-, and He III-impacts with Cr VI emitter / absorber will be also implemented in the STARK-B database (http://stark-b.obspm.fr [6]), a part of Virtual Atomic and Molecular Data Center (VAMDChttp://www.vamdc.org [7]).

show abstract

“…An important topic where Stark broadening data are needed are astrophysical plasmas (Beauchamp et al, 1997;Dimitrijević & Sahal-Bréchot, 2014b ), in particular at mospheres of white dwarfs, pre white dwarf stars, and post AGB (Asymptotic Giant Branch) stars (Tankosić et al, 2003;Milovanović et al, 2004;Simić et al, 2006;Dufour et al, 2011). Additionally, since for temperatures higher than around 10 000 K hydrogen is mainly ionized, Stark broadening is, in such a case, the principal pressure broadening mechanism (Griem, 1974).…”

Section: Datamentioning

confidence: 99%

On the stark broadening of Ar VII spectral lines

Dimitrijević¹,

Sahal‐Bréchot²

2017

Univ Thought

View full text Add to dashboard Cite

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).

show abstract

The electron-impact broadening parameters for Co III spectral lines

Cited by 26 publications

References 11 publications

Electron-impact broadening parameters for Be II, Sr II, and Ba II spectral lines

Electron-impact broadening parameters for Be II, Sr II, and Ba II spectral lines

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

On the stark broadening of Ar VII spectral lines

Contact Info

Product

Resources

About