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Forty Years of the Applications of Stark Broadening Data Determined with the Modified Semiempirical Method
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Stark Broadening of Co II Lines in Stellar Atmospheres

1
Astronomical Observatory, Volgina 7, 11060 Belgrade, Serbia
2
Sorbonne Université, Observatoire de Paris, Université PSL, CNRS, F-92195 Meudon, France
3
Institute of Physics Belgrade, University of Belgrade, 11001 Belgrade, Serbia
*
Author to whom correspondence should be addressed.
Received: 2 August 2020 / Revised: 17 August 2020 / Accepted: 24 August 2020 / Published: 27 August 2020
(This article belongs to the Special Issue Astronomy in the Big Data Era: Perspectives)
Data for Stark full widths at half maximum for 46 Co II multiplets were calculated using a modified semiempirical method. In order to show the applicability and usefulness of this set of data for research into white dwarf and A type star atmospheres, the obtained results were used to investigate the significance of the Stark broadening mechanism for Co II lines in the atmospheres of these objects. We examined the influence of surface gravity (log g), effective temperature and the wavelength of the spectral line on the importance of the inclusion of Stark broadening contribution in the profiles of the considered Co II spectral lines, for plasma conditions in atmospheric layers corresponding to different optical depths. View Full-Text
Keywords: atomic data; stark broadening data; line profiles; Co II; white dwarfs; A-type stars atomic data; stark broadening data; line profiles; Co II; white dwarfs; A-type stars
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    Doi: 10.1093/mnras/staa1947
    Description: STARK WIDTHS FOR 46 Co II LINES Table 1. MSE Stark Full Width at Half Intensity Maximum (WMSE) calculated for Co II transitions for five different temperature values (Majlinger Z., Dimitrijević M. S., Srećković V. A., MNRAS 2020, 496, 5584). Electron density of 10E+23 m-3 is used. Table 2. Coefficients for fitting formula log w(T) = a + b log T + c log2 T (Sahal-Bréchot S., Dimitrijević M.S., Ben Nessib N., 2011, Baltic Astron., 20, 523) where w(T) is Stark width in A, and T temperature in kelvins. The fitting parameters a, b and c are calculated for electron density of 10E+23 m-3 and tabulated for all lines in Table 1. Although Tab. 1 presents electron-impact widths for temperatures of 5000 K, 10000 K, 20000 K, 50000 K and 100000 K only, interpolation parameters are calculated for interval from 5000 K to 200000 K and thus can be used for any further calculations of Stark widths within this range of temperatures.
MDPI and ACS Style

Majlinger, Z.; Dimitrijević, M.S.; Srećković, V.A. Stark Broadening of Co II Lines in Stellar Atmospheres. Data 2020, 5, 74. https://doi.org/10.3390/data5030074

AMA Style

Majlinger Z, Dimitrijević MS, Srećković VA. Stark Broadening of Co II Lines in Stellar Atmospheres. Data. 2020; 5(3):74. https://doi.org/10.3390/data5030074

Chicago/Turabian Style

Majlinger, Zlatko, Milan S. Dimitrijević, and Vladimir A. Srećković. 2020. "Stark Broadening of Co II Lines in Stellar Atmospheres" Data 5, no. 3: 74. https://doi.org/10.3390/data5030074

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