Extensive spectroscopic data for multiply ionized scandium: Sc III to Sc XXI

Massacrier, G.; Artru, M. C.

doi:10.1051/0004-6361/201117758

Cited by 22 publications

(27 citation statements)

References 21 publications

(25 reference statements)

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“…For numerical expediency, the levels of the ions treated are combined as described in Alecian & Artru (1990a) during these calculations. Since no other precise radiative accelerations of Sc exist (as opposed to the elements treated in Paper II where the radiative accelerations of Seaton 1997 were available), the values of α i are obtained by fitting the radiative accelerations calculated A89, page 2 of 4 with the SVP method to those calculated in more detail, namely by using the values of φ i and ψ i calculated in each layer of the underlying stellar model with the atomic data of Massacrier & Artru (2012). A fitting procedure using the GLAM results described below could have been employed, but we prefer to have two independent results for g rad which may lead to firmer conclusions rather than having the results of the SVP method depend on those of the GLAM method.…”

Section: The Single-valued Parameters Methodsmentioning

confidence: 99%

“…Recently, Massacrier & Artru (2012) have performed a large scale analysis of the energy levels and transition data for Sc iii to Sc xxi, i.e. all the ions of scandium except for Sc i and Sc ii.…”

Section: New Atomic and Spectroscopic Datamentioning

confidence: 99%

“…Recently, Massacrier & Artru (2012) have published new and extensive theoretical atomic data for Sc. The purpose of the Article published by EDP Sciences A89, page 1 of 4 present paper is to revisit the study of LeBlanc & Alecian (2008) using this new atomic data to calculate the parameters needed to obtain radiative accelerations by the SVP method, instead of using interpolated values of these parameters.…”

Section: Introductionmentioning

confidence: 99%

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Scandium in AmFm stars in the light of new atomic data

Alecian¹,

Leblanc²,

Massacrier³

2013

A&A

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Context. The abundance anomalies observed in AmFm stars are believed to be caused by atomic diffusion below the superficial convection zone. The process by which these anomalies, which are produced in deep layers, propagate toward the stellar surface is well understood. However, it depends on quantities which are not directly observed: the mass-loss flux and the exact position of convections zones. Scandium, which is systematically underabundant at the surface of AmFm stars, is a key element in understanding the interplay between atomic diffusion and the stellar structure and how this structure evolves with time. Aims. In the light of a new extensive set of atomic data, we calculate much more accurate radiative accelerations of Sc than previously done in the aim to better understand the observed abundance anomalies of this element in AmFm stars. Methods. Two methods are employed to obtain these radiative accelerations based on the so-called SVP (single-valued parameters) parametric method and the GLAM method while employing this new atomic data. Results. The radiative accelerations, shown here in a typical Am stellar model, are discussed in the light of the observed anomalies of Sc. Our results are more compatible with the scenario where the scandium depletion is created below the hydrogen convection zone.

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Section: The Single-valued Parameters Methodsmentioning

confidence: 99%

Section: New Atomic and Spectroscopic Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Scandium in AmFm stars in the light of new atomic data

Alecian¹,

Leblanc²,

Massacrier³

2013

A&A

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“…The FAC is a fully relativistic atomic program that takes configuration interaction into consideration; it is widely used in the calculations of the atomic data needed to analyze X-ray spectra (Beiersdorfer 2009). The accuracy of these calculations were assessed by many recent works (Massacrier & Artru 2012;Wei et al 2010). In order to investigate the effects of different atomic data on the calculated absorption spectra, we adopted the same configurations as those in the work of Palmeri et al (2008), who calculated the K-shell atomic data.…”

Section: Modelmentioning

confidence: 99%

Effects of lowly ionized ions on silicon K-shell absorption spectra

Wei

Shi

Liang

et al. 2016

A&A

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Context. In both astrophysical and laboratory plasmas, K-shell absorption spectra have become powerful diagnostic tools to investigate electron density and temperature. These spectra are also widely used to verify the opacity codes in laboratory settings. Aims. We report the effects of the low ionization silicon ions, namely from Si I to Si V, which have rarely been considered in previous models, on the K-shell silicon absorption spectra. Methods. The Si K-shell atomic data were calculated with the flexible atomic code, which is a fully relativistic atomic program with configuration interaction taken into consideration. Detailed level accounting models were employed to calculate the absorption spectra. Results. We calculate the Si absorption spectra in local thermodynamic equilibrium conditions with temperature and density ranges of 20−70 eV and ∼10 20 cm −3 to ∼10 22 cm −3 , respectively, and show the contributions of the lowly ionized ions to the K-shell absorption spectra of silicon. We also investigate the effects of the different atomic data on the absorption spectra. We find good agreement between our results and these from OPLIB. Conclusions. We find that the contributions from these lowly ionized ions cannot be neglected at relative low temperatures. Accurate experimental measurements are needed to benchmark the theoretical calculations.

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“…In addition to the calculations above, see for example, Safronova et al (2000), Froese Fischer et al (2006), Massacrier & Artru (2012), Hu et al (2014), Si et al (2015), Santana & Träbert (2015). The most recent R-matrix calculations for the Mg-like ions include both collisional and radiative data (Fernandez-Menchero et al 2014).…”

Section: Introductionmentioning

confidence: 99%

MCDHF and RCI calculations of energy levels, lifetimes and transition rates for3l3l′,3l4l′, and3s5lstates in Ca IX – As XXII and Kr XXV

Gustafsson

Jönsson

Fischer

et al. 2017

A&A

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Multiconfiguration Dirac-Hartree-Fock (MCDHF) calculations and relativistic configuration interaction (RCI) calculations were performed for states of the 3l3l , 3l4l and 3s5l configurations in the Mg-like ions Ca IX -As XXII and Kr XXV. Valence and core-valence electron correlation effects are accounted for through large configuration state function expansions. Calculated excitation energies are in very good agreement with observations for the lowest levels. For higher lying levels observations are often missing and present energies aid line identification in spectra. Lifetimes and transition data are given for all ions. There is an excellent agreement for both lifetimes and transition data with recent multiconfiguration Hartree-Fock Breit Pauli calculations.

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Extensive spectroscopic data for multiply ionized scandium: Sc III to Sc XXI

Cited by 22 publications

References 21 publications

Scandium in AmFm stars in the light of new atomic data

Scandium in AmFm stars in the light of new atomic data

Effects of lowly ionized ions on silicon K-shell absorption spectra

MCDHF and RCI calculations of energy levels, lifetimes and transition rates for3l3l′,3l4l′, and3s5lstates in Ca IX – As XXII and Kr XXV

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