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![Stark and Doppler broadening of Co II spectral line λ9969 as a function of temperature of atmospheric layers in a DB white dwarf. Stark widths are shown for models [32] with five different values of effective temperature, Teff = 14,000-30,000 K and log g = 8.](profile/Milan-Dimitrijevic-2/publication/343905720/figure/fig2/AS:929068480483331@1598518595603/Stark-and-Doppler-broadening-of-Co-II-spectral-line-l9969-as-a-function-of-temperature-of.jpg)
Stark and Doppler broadening of Co II spectral line λ9969 as a function of temperature of atmospheric layers in a DB white dwarf. Stark widths are shown for models [32] with five different values of effective temperature, Teff = 14,000-30,000 K and log g = 8.
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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 fo...
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... we decided to investigate how effective temperature and surface gravity of DB WD affect the relationship between Stark and Doppler widths for a particular spectral line. In Figure 5, comparison of Stark and Doppler broadening of Co II line λ9969 in white dwarf atmospheres is presented as a function of layer temperature for five different models [34] of DB white dwarf atmospheres with effective temperatures from 14,000 to 30,000 K with a step of 4000 K, and log g = 8. The effective temperature is approximately taken as the temperature of the surface of the star. ...
Citations
... The study of white dwarfs demonstrates the significant importance of Stark broadening data. The influence of these data in DO dwarfs is investigated in [31][32][33], in DB dwarfs in [34][35][36], in DA dwarfs [35,36] in B subdwarfs in [37,38]. Authors in [35,36] outline that such data could be of interest for main-sequence stars of spectral types A and late B. ...
... The study of white dwarfs demonstrates the significant importance of Stark broadening data. The influence of these data in DO dwarfs is investigated in [31][32][33], in DB dwarfs in [34][35][36], in DA dwarfs [35,36] in B subdwarfs in [37,38]. Authors in [35,36] outline that such data could be of interest for main-sequence stars of spectral types A and late B. ...
... The influence of these data in DO dwarfs is investigated in [31][32][33], in DB dwarfs in [34][35][36], in DA dwarfs [35,36] in B subdwarfs in [37,38]. Authors in [35,36] outline that such data could be of interest for main-sequence stars of spectral types A and late B. ...
... The reason is because of how they affect the spectral properties of astrophysical and laboratory plasmas (Srećković et al., 2014;Tielens, 2013;Beuc et al., 2018a). The ionization level, atom excited-state populations, and optical characteristics can all be affected by collisional events that involve electrons, atoms, ions, and small molecule ions (Schneider et al., 1991;Mihajlov et al., 2011;Srećković et al., 2017;Beuc et al., 2018b;Majlinger et al., 2020). ...
We investigated the electron-impact processes involving hydrogen, lithium and sodium molecular cations. Rate coefficients for the dissociative re-combination in domains of principal quantum numbers n ≥ 4 and temperatures from 500 K to 10 000K are reported. Considered collisional processes have an impact on the ionization level and atom excited-state populations as well on optical characteristics. The data are useful for the modeling of the kinetics of the Early Universe and for geocosmical plasma investigation.
... Atomic and molecular databases and data have become crucial for data interpretation, diagnostics, and the creation of models and simulations of intricate physical processes [1][2][3][4]. The importance of studying optical properties in different fields, especially when modelling those systems, is of particular interest [5][6][7]. ...
The calculated photodissociation data of some small molecular ions have been reported. The cross-sections and spectral rate coefficients data have been studied using a quantum mechanical method. The plasma parameters, i.e., conditions, cover temperatures from 1000 to 20,000 K and wavelengths in the EUV and UV region. The influence of temperature and wavelength on the spectral coefficients data of all of the investigated species have been discussed. Data could also be useful for plasma diagnostics in laboratory, astrophysics, and industrial plasmas for their modelling.
... Data on Stark broadening of spectral lines are particularly needed for white dwarfs, because there, this is usually the principal pressure-broadening mechanism. For example, the influence of Stark broadening in DO dwarfs has been investigated in Dimitrijević et al. (2016), Dimitrijević & Chougule (2018), and , in DB in Majlinger, Dimitrijević & Simić (2018), Majlinger, Dimitrijević & Srećković (2020a and Majlinger, Dimitrijević & Srećković (2020b), in DA in Majlinger et al. (2020a) and Majlinger et al. (2020b), and in B subdwarfs in Hamdi et al. (2017) and Chougule et al. (2020). Such data may be also of interest in the case of the main-sequence stars, in particular, for A and late B spectral types (Majlinger et al. 2020a,b). ...
... Data on Stark broadening of spectral lines are particularly needed for white dwarfs, because there, this is usually the principal pressure-broadening mechanism. For example, the influence of Stark broadening in DO dwarfs has been investigated in Dimitrijević et al. (2016), Dimitrijević & Chougule (2018), and , in DB in Majlinger, Dimitrijević & Simić (2018), Majlinger, Dimitrijević & Srećković (2020a and Majlinger, Dimitrijević & Srećković (2020b), in DA in Majlinger et al. (2020a) and Majlinger et al. (2020b), and in B subdwarfs in Hamdi et al. (2017) and Chougule et al. (2020). Such data may be also of interest in the case of the main-sequence stars, in particular, for A and late B spectral types (Majlinger et al. 2020a,b). ...
Stark broadening parameters, full widths at half intensity maximum and shifts for 34 multiplets of singly charged zinc ion have been calculated using the impact semiclassical perturbation formalism. Stark broadening parameters due to collisions with electrons, protons and helium ions have been obtained for a grid of electron densities and temperatures. The obtained results have been used to demonstrate the influence of Stark broadening mechanism on spectral lines of Zn II in stellar atmospheres.
Atomic and molecular (A&M) databases that contain information about species, their identities and radiative/collisional processes are essential and helpful tools that are utilized in many fields of physics, chemistry, and chem/phys-informatics. Errors or inconsistencies in the datasets are a serious issue since they can lead to inaccurate predictions and generate problems with the modeling. This demonstrates that data curation efforts around A&M databases are still indispensable and that in the curation process studious attention is required. Therefore, we herein present research activities around Belgrade "nodes" - datasets of collision/radiative cross-sections and rates needed for spectroscopy analysis in various A&M, optical and plasma physics fields. Methodologies of our research and both present and future aspects of the applications are explained. We explored the possibility to extend our nodes towards building a new database on Judd-Ofelt parameters by using machine learning in order to predict optical properties of luminescence materials. In addition, we hope that public availability of our datasets and their graphical representations will also motivate others to investigate the potential of these data.
We calculated widths and shifts due to collisions with electrons, protons and He II ions for 66 multiplets of neutral boron, using the semiclassical perturbation theory. The range of temperatures is from 2500 K to 50 000 K and electron density values are within the range 1011–1019 cm−3. The obtained Stark broadening parameters have been compared to other theoretical and experimental results.
