Comment on “Theoretical Confirmation of the Low Experimental 
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-Value Ratio in Fe xvii”

Wang, Kai; Jönsson, P.; Ekman, Jörgen; Brage, Tomas; Chen, Chong Yang; Fischer, Charlotte Froese; Gaigalas, Gediminas; Godefroid, Michel

doi:10.1103/physrevlett.119.189301

Cited by 22 publications

(8 citation statements)

References 9 publications

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“…However, it was argued later that the calculated ratio in ref. 12 is unreliable due to a limited and unbalanced treatment of electron correlations 13 . Alternatively, it was proposed that other physical processes beyond those included in the atomic structure calculation of an isolated atomic system, such as the one due to the ultra-high intensities of XFEL with ultra-short pulse period, may be responsible for this discrepancy 10,14,15 .…”

Section: Introductionmentioning

confidence: 99%

Change of the relative line strengths due to the resonance induced population transfer between Fe XVII and FeXVI ions

Gao

2019

Sci Rep

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We present a detailed study to resolve the discrepancy between the existing theoretically estimated oscillator strengths and the recently observed result from the X-ray free electron laser (XFEL) experiment performed at the Linac Coherent Light Source (LCLS) for the intensity ratio between two of the strongest emission lines from Ne-like Fe XVII (Fe 16+ ) ion. By including the dynamic resonance induced population transfer due to autoionization between the coexisting Fe XVII and Fe XVI (Fe 15+ ) ions in the XFEL experiment, we are able to successfully resolve this difference in theory and experiment. Further experimental works are suggested for a more detailed understanding of the dynamic resonance processes for ions.

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Section: Introductionmentioning

confidence: 99%

Change of the relative line strengths due to the resonance induced population transfer between Fe XVII and FeXVI ions

Gao

2019

Sci Rep

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“…An effect of resonance-induced population transfer between Fe XVI and Fe XVII ions was also postulated [35] since the Fe XVI line C (½ð2p 5 Þ 1=2 3s3d 5=2 J¼3=2 → ½2p 6 3s J¼1=2 ) appeared blended with the Fe XVII line 3D. A recent semiempirical calculation [36] reproduces the LCLS results [25] by finetuning relativistic couplings and orbital relaxation effects, but its validity has been disproved [37].…”

mentioning

confidence: 99%

“…Blue crosses: predictions [29,31,32,35,36,[54][55][56][57]. Note that the validity of theory [36] has been disputed [37]. Blue solid circles: present FAC [58], large-scale CI [39], MR-MCDHF [40], and AMBiT [41] calculations.…”

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confidence: 99%

High Resolution Photoexcitation Measurements Exacerbate the Long-Standing Fe XVII Oscillator Strength Problem

Kühn¹,

Shah²,

López‐Urrutia³

et al. 2020

Phys. Rev. Lett.

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For more than 40 years, most astrophysical observations and laboratory studies of two key soft x-ray diagnostic 2p − 3d transitions, 3C and 3D, in Fe XVII ions found oscillator strength ratios fð3CÞ=fð3DÞ disagreeing with theory, but uncertainties had precluded definitive statements on this much studied conundrum. Here, we resonantly excite these lines using synchrotron radiation at PETRA III, and reach, at a millionfold lower photon intensities, a 10 times higher spectral resolution, and 3 times smaller uncertainty than earlier work. Our final result of fð3CÞ=fð3DÞ ¼ 3.09ð8Þð6Þ supports many of the earlier clean astrophysical and laboratory observations, while departing by five sigmas from our own newest large-scale ab initio calculations, and excluding all proposed explanations, including those invoking nonlinear effects and population transfers.

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“…The other aim of the present study is to offer a consistent set of transition rates with high accuracy for all the ions for spectral line modeling. This study is an extension of our previous calculations (Jönsson et al 2011(Jönsson et al , 2014Wang et al 2014Wang et al , 2015Wang et al , 2016aWang et al , 2016bWang et al , 2017aWang et al , 2017bWang et al , 2017cWang et al , 2017dWang et al , 2018aWang et al , 2018cGuo et al 2015Guo et al , 2016Si et al 2016Si et al , 2017Chen et al 2017Chen et al , 2018Zhao et al 2018) for offering atomic data with high accuracy for L-and M-shell systems.…”

Section: Introductionmentioning

confidence: 95%

Benchmarking Atomic Data from Large-scale Multiconfiguration Dirac–Hartree–Fock Calculations for Astrophysics: S-like Ions from Cr ix to Cu xiv

Wang

Song

Jönsson

et al. 2018

ApJS

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We present a consistent set of calculated energies and E1, M1, E2, M2 radiative transition data for the main n=3 levels from the 3s 2 3p 4 , 3p 6 , s p d 3 3 3 4 configurations, producing the strongest lines, are found to be in good agreement, reaching spectroscopic accuracy, with the latest experimental values for Fe XI evaluated by Del Zanna. Our energies can reliably be used to identify in astrophysical and laboratory spectra the s p d 3 3 3 2 3 levels in other S-like ions, which are mostly unknown. On the contrary, significant discrepancies with the 3s3p 4 3d levels were found, emphasizing the need for more detailed experimental studies. A few new tentative identifications are suggested. The benchmarks we present indicate that our consistent set of radiative data is accurate and can be used for spectral line modeling.

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Comment on “Theoretical Confirmation of the Low Experimental 3C/3D f -Value Ratio in Fe xvii”

Abstract: Comment on "Theoretical Confirmation of the Low Experimental 3C=3D f-Value Ratio in Fe XVII" Recently, Mendoza and Bautista (MB) published configuration interaction calculations of the debated 2p 61 S 0 − 2p 5 3d 3 D

Cited by 22 publications

References 9 publications

Change of the relative line strengths due to the resonance induced population transfer between Fe XVII and FeXVI ions

Change of the relative line strengths due to the resonance induced population transfer between Fe XVII and FeXVI ions

High Resolution Photoexcitation Measurements Exacerbate the Long-Standing Fe XVII Oscillator Strength Problem

Benchmarking Atomic Data from Large-scale Multiconfiguration Dirac–Hartree–Fock Calculations for Astrophysics: S-like Ions from Cr ix to Cu xiv

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