Extended Calculations With Spectroscopic Accuracy: Energy Levels and Transition Properties for the Fluorine-Like Isoelectronic Sequence With Z = 24–30

Si, R.; Li, Shuang; Guo, Xueling; Chen, ZhanBin; Brage, Tomas; Jönsson, P.; Wang, Kai; Yan, Jun; Chen, ChangYan; Zou, Yaming

doi:10.3847/0067-0049/227/2/16

Cited by 44 publications

(39 citation statements)

References 53 publications

(92 reference statements)

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“…Wang and co-workers have systematically compared large sets of transition rates from accurate RMCDHF/RCI and RMBPT calculations [49][50][51][52]. These comparisons show that the rates from the two methods agree within a few percent for the strong transitions and that the agreement gets slightly worse for the weak intercombination and the two-electron, one photon transitions 1 .…”

Section: Systematic Comparisons Between Methodsmentioning

confidence: 99%

“…To meet this demand, the RMCDHF/RCI and SD-MR calculations for the B-, C-, N-, O-, F-and Ne-like sequences have been extended to hundreds of states in what we refer to as spectrum calculations [45][46][47][48][49][50][51][52]. The range of ions, the targeted configurations and the number of studied states for each sequence are summarized in Table 5.…”

Section: Energies For Higher States In the B- C- N- O- F-and Ne-lmentioning

confidence: 99%

“…The reason for this shift is not known, and further research is needed to shed light on this. To further access the accuracy of the excitation energies, calculations for the N-, O-, F-and Ne-like sequences [49][50][51][52] were done using both the RMCDHF/RCI and RMBPT methods. Cross-validations show that the mean energy differences for N-like, O-like, F-like and Ne-like Fe are 0.023%, 0.011%, 0.01% and 0.029%, respectively.…”

Section: Energies For Higher States In the B- C- N- O- F-and Ne-lmentioning

confidence: 99%

“…The RMCDHF/RCI and SD-MR method has been used to compute tens of thousands of E1, M1, E2, M2 transitions rates for the B-to Si-like sequences [28][29][30][31][32]43,[45][46][47][48][49][50][51][52][54][55][56]. The E1 and E2 rates are internally validated by giving δA/A along with A.…”

Section: Transition Rates For the B-to Si-like Sequencesmentioning

confidence: 99%

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Multiconfiguration Dirac-Hartree-Fock Calculations with Spectroscopic Accuracy: Applications to Astrophysics

Jönsson

Gaigalas

Rynkun

et al. 2017

Atoms

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Abstract:Atomic data, such as wavelengths, spectroscopic labels, broadening parameters and transition rates, are necessary for many applications, especially in plasma diagnostics, and for interpreting the spectra of distant astrophysical objects. The experiment with its limited resources is unlikely to ever be able to provide a complete dataset on any atomic system. Instead, the bulk of the data must be calculated. Based on fundamental principles and well-justified approximations, theoretical atomic physics derives and implements algorithms and computational procedures that yield the desired data. We review progress and recent developments in fully-relativistic multiconfiguration Dirac-Hartree-Fock methods and show how large-scale calculations can give transition energies of spectroscopic accuracy, i.e., with an accuracy comparable to the one obtained from observations, as well as transition rates with estimated uncertainties of a few percent for a broad range of ions. Finally, we discuss further developments and challenges.

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Section: Systematic Comparisons Between Methodsmentioning

confidence: 99%

Section: Energies For Higher States In the B- C- N- O- F-and Ne-lmentioning

confidence: 99%

Section: Energies For Higher States In the B- C- N- O- F-and Ne-lmentioning

confidence: 99%

Section: Transition Rates For the B-to Si-like Sequencesmentioning

confidence: 99%

See 2 more Smart Citations

Multiconfiguration Dirac-Hartree-Fock Calculations with Spectroscopic Accuracy: Applications to Astrophysics

Jönsson

Gaigalas

Rynkun

et al. 2017

Atoms

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show abstract

“…To solve this dilemma, we have computed highly accurate energy and radiative transition data for L-shell atomic ions Ekman et al 2014;Wang et al 2014Wang et al , 2015Wang et al , 2016aWang et al ,b, 2017cRadžiūtė et al 2015;Si et al 2016). This work reports accurate atomic data resulting from our systematic calculations for beryllium-like ions from B II to Ne VII.…”

Section: Introductionmentioning

confidence: 99%

Benchmarking Atomic Data for Astrophysics: Be-like Ions between B ii and Ne vii

Wang

Chen

Zhang

et al. 2018

ApJS

Self Cite

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Large-scale self-consistent multiconfiguration Dirac-Hartree-Fock and relativistic configuration interaction calculations are reported for the n ≤ 6 levels in Be-like ions from B II to Ne VII. Effects from electron correlation are taken into account by means of large expansions in terms of a basis of configuration state functions, and a complete and accurate data set of excitation energies, lifetimes, wavelengths, and electric dipole, magnetic dipole, electric quadrupole, and magnetic quadrupole line strengths, transition rates, and oscillator strengths for these levels is provided for each ion. Comparisons are made with available experimental and theoretical results. The uncertainty of excitation energies is assessed to be 0.01% on average, which makes it possible to find and rule out misidentifications and aid new line identifications involving high-lying levels in astrophysical spectra. The complete data set is also useful for modeling and diagnosing astrophysical plasmas.

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Solar UV and X-ray spectral diagnostics

Zanna

Mason

2018

Living Rev Sol Phys

222

139

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X-ray and ultraviolet (UV) observations of the outer solar atmosphere have been used for many decades to measure the fundamental parameters of the solar plasma. This review focuses on the optically thin emission from the solar atmosphere, mostly found at UV and X-ray (XUV) wavelengths, and discusses some of the diagnostic methods that have been used to measure electron densities, electron temperatures, differential emission measure (DEM), and relative chemical abundances. We mainly focus on methods and results obtained from high-resolution spectroscopy, rather than broad-band imaging. However, we note that the best results are often obtained by combining imaging and spectroscopic observations. We also mainly focus the review on measurements of electron densities and temperatures obtained from single ion diagnostics, to avoid issues related to the ionisation state of the plasma. We start the review with a short historical introduction on the main XUV high-resolution spectrometers, then review the basics of optically thin emission and the main processes that affect the formation of a spectral line. We mainly discuss plasma in equilibrium, but briefly mention non-equilibrium ionisation and non-thermal electron distributions. We also summarise the status of atomic data, which are an essential part of the diagnostic process. We then review the methods used to measure electron densities, electron temperatures, the DEM, and relative chemical abundances, and the results obtained for the lower solar atmosphere (within a fraction of the solar radii), for coronal holes, the quiet Sun, active regions and flares.

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Extended Calculations With Spectroscopic Accuracy: Energy Levels and Transition Properties for the Fluorine-Like Isoelectronic Sequence With Z = 24–30

Cited by 44 publications

References 53 publications

Multiconfiguration Dirac-Hartree-Fock Calculations with Spectroscopic Accuracy: Applications to Astrophysics

Multiconfiguration Dirac-Hartree-Fock Calculations with Spectroscopic Accuracy: Applications to Astrophysics

Benchmarking Atomic Data for Astrophysics: Be-like Ions between B ii and Ne vii

Solar UV and X-ray spectral diagnostics

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