Transitions in C II, N III, and O IV

Correge, Gwenaelle; Hibbert, A

doi:10.1016/j.adt.2003.11.002

Cited by 21 publications

(17 citation statements)

References 15 publications

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“…Calculated transition energies are in good agreement with observed transition energies obtained from [25]. In Table 4 we compare electric dipole transition rates with rates taken from MR RCI [9,11], MCHF [8], CIV3 [12] calculations and values taken from NIST [25]. In this table we give rates in both the Babushkin and Coulomb gauges.…”

Section: Results and Evaluation Of Datasupporting

confidence: 66%

“…4). The results for the energies, transition rates and lifetimes are compared with the earlier available values obtained from calculations in the Breit-Pauli approximation [6], in the relativistic configuration interaction method [9,10], in CIV3 method [12] and also with experimental measurements. Results from our present calculations are in very good agreement with other theoretical methods, also as with experimental values.…”

Section: Discussionmentioning

confidence: 99%

“…K. Koc calculated energy levels and transitions rates based on the multireference relativistic configuration interaction (MR RCI) method with the no-pair Dirac-Coulomb-Breit Hamiltonian [9][10][11]. G. Corrégé and A. Hibbert have presented energy levels, oscillator strengths and transitions probabilities for C II, N III and O IV using the code CIV3 [12]. Jönsson et al presented energy levels, specific mass shift parameters, hyperfine interaction constants, and transition probabilities for C II, N III, and O IV using the multiconfiguration Dirac-Hartree-Fock method [13,14].…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Energies and E1, M1, E2, M2 transition rates for states of the 2s22p, 2s2p2, and 2p3 configurations in boron-like ions between N III and Zn XXVI

Rynkun

Jönsson

Gaigalas

et al. 2012

Atomic Data and Nuclear Data Tables

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Energies, E1, M1, E2, M2 transition rates, line strengths, oscillator strengths, and lifetimes from relativistic configuration interaction calculations are reported for the states of the (1s 2 )2s 2 2p, 2s2p 2 , and 2p 3 configurations in all boron-like ions between N III and Zn XXVI. Valence, core-valence, and core-core correlation effects were accounted for through singledouble multireference (SD-MR) expansions to increasing sets of active orbitals.

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Section: Results and Evaluation Of Datasupporting

confidence: 66%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Energies and E1, M1, E2, M2 transition rates for states of the 2s22p, 2s2p2, and 2p3 configurations in boron-like ions between N III and Zn XXVI

Rynkun

Jönsson

Gaigalas

et al. 2012

Atomic Data and Nuclear Data Tables

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“…We note, however, that we have replaced the A-values of the transitions among the lowest levels as calculated by Liang et al (2012) with autostructure with more accurate values, whenever available. For example, those calculated by Corrégé & Hibbert (2004) with the CIV3 code (Hibbert 1975) and those calculated by Rynkun et al (2012) with the multi-configuration DiracHartree-Fock (MCDHF) GRASP2K code (Jönsson et al 2007). This is because the ab initio energies of the CIV3 and GRASP2K are normally more accurate than those by autostructure, and so are the A-values.…”

Section: Li-like Ionsmentioning

confidence: 99%

CHIANTI – An atomic database for emission lines. Version 8

Zanna

Dere

Young

et al. 2015

A&A

442

407

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We present version 8 of the CHIANTI database. This version includes a large amount of new data and ions, which represent a significant improvement in the soft X-ray, extreme UV (EUV) and UV spectral regions, which several space missions currently cover. New data for neutrals and low charge states are also added. The data are assessed, but to improve the modelling of low-temperature plasma the effective collision strengths for most of the new datasets are not spline-fitted as previously, but are retained as calculated. This required a change of the format of the CHIANTI electron excitation files. The format of the energy files has also been changed. Excitation rates between all the levels are retained for most of the new datasets, so the data can in principle be used to model highdensity plasma. In addition, the method for computing the differential emission measure used in the CHIANTI software has been changed.

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“…comm.) The radiative transition probabilities (A-values) for ground forbidden transitions have been taken from Flower & Nussbaumer (1975), while for the allowed transitions 2s 2 2p − 2s2p 2 and 2s 2 2p − 2s 2 3s the values from Corrégé & Hibbert (2004) are used. All others are taken from NIST.…”

Section: Atomic Datamentioning

confidence: 99%

Comparison between observed and theoretical O IV line ratios in the UV/EUV solar spectrum as derived by SUMER, CDS and EIS

Giunta

Fludra

O’Mullane

et al. 2012

A&A

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Aims. The joint use of SoHO Solar Ultraviolet Measurement of Emitted Radiation (SUMER), Coronal Diagnostic Spectrometer (CDS) and Hinode Extreme-ultraviolet Imaging Spectrometer (EIS) allow observation of several O iv line ratios, useful for temperature plasma diagnostics. Accurate atomic data are required to avoid interpretation errors in deriving the electron temperature from these ratios. Muglach et al. (2010) found that the measured ratio I(787.72 Å)/I(279.93 Å) is lower than the predicted value by a factor 2-5. Here the predicted value for this ratio is revised using updated atomic data. A comparison with other observed O iv line ratios is shown and the electron temperature is derived. Methods. The analysis is based on new observations made during the observational campaign of April 2009 and including three O iv multiplets. The theoretical ratios have been derived using the Atomic Data and Analysis Structure (ADAS) database and include comparison with the most recent calculations available in the literature. Results. The discrepancy for the O iv I(787.72 Å)/I(279.93 Å) ratio has been solved by adding transitions involving higher excited levels, which have been omitted in previous atomic models. This results in a decrease of the theoretical line ratio, providing electron temperatures in the range of log T = 5.17-5.39, close to the temperature expected from a plasma in ionisation equilibrium.

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Transitions in C II, N III, and O IV

Cited by 21 publications

References 15 publications

Energies and E1, M1, E2, M2 transition rates for states of the 2s22p, 2s2p2, and 2p3 configurations in boron-like ions between N III and Zn XXVI

Energies and E1, M1, E2, M2 transition rates for states of the 2s22p, 2s2p2, and 2p3 configurations in boron-like ions between N III and Zn XXVI

CHIANTI – An atomic database for emission lines. Version 8

Comparison between observed and theoretical O IV line ratios in the UV/EUV solar spectrum as derived by SUMER, CDS and EIS

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