Oscillator strength for 3s23p5-3s3p6in Cl-like ions

Berrington, K A; Pelan, John; Waldock, Jeff

doi:10.1088/0953-4075/34/13/102

Cited by 22 publications

(19 citation statements)

References 29 publications

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“…Table 2 lists the set of configurations we finally adopted for our SUPERSTRUCTURE (SS) calculation, after a number of tests had been run. These tests confirmed the importance of including configurations with orbitals 3d 2 and 3d 3 (as discussed in Berrington et al 2001) in order to have accurate g f values and energies. Table 3 lists the results for the 54 levels, ordered according to the energies E CC of the target for the collisional calculations.…”

Section: Model Ion For Fe supporting

confidence: 61%

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Benchmarking atomic data for astrophysics: $\ion{Fe}{x}$

Zanna¹,

Berrington

Mason³

2004

A&A

100

114

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Abstract. This is the first in a series of papers in which we benchmark recent atomic data available for astrophysical applications. We review various issues related to the completeness and accuracy of both theoretical and experimental data. In this paper, the available experimental and atomic data for Fe  (n = 3 configurations) are reviewed and assessed. New collisional and radiative data are calculated to supplement published data. The radiative calculations are done with empirical adjustements that take into account observed wavelengths. Previous line identifications are also reviewed and assessed. Our approach focuses on the brightest spectral lines, and uses both wavelengths and line intensities to assess the line identifications on a quantitative basis. Although many previous line identifications are confirmed, some are rejected (e.g. the coronal line observed at 1582.35 Å). We confirm previously suggested identifications (e.g. 257.262 Å, 1028.02 Å), and we present new ones, (e.g. the lines of the 3s 2 3p 4 3d-3s 3p 5 3d transition array). In addition, we highlight the presence of blends and we review which spectral lines are best for density diagnostics or for instrument calibration. The theoretical data (line intensities and level lifetimes) are benchmarked against well-calibrated spectroscopic observations of the solar corona and laboratory measurements. The agreement between theoretical and experimental data which we achieve with our new model ion is very good.

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Section: Model Ion For Fe supporting

confidence: 61%

“…However line strengths for forbidden transitions are less reliable and more susceptible to which configurations have been used in the calculation. The importance of including the right configurations has been emphasised by many authors (see, for example, the discussion on the Fe  case in Berrington et al 2001). …”

Section: Radiative Datamentioning

confidence: 99%

Benchmarking atomic data for astrophysics: $\ion{Fe}{x}$

Zanna¹,

Berrington

Mason³

2004

A&A

100

114

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“…The other available results of lifetimes are for the 3s3p 6 2 S 1/2 level (3) from Biémont & Träbert (2000) and Berrington et al (2001), which are 0.20 and 0.206 ns, respectively. Both of these results agree very well with our τ value of 0.204 ns from grasp.…”

Section: Lifetimesmentioning

confidence: 99%

“…Particularly noteworthy are the calculations for Co xi by Huang et al (1983), Biémont & Träbert (2000), and Berrington et al (2001). Huang et al performed relativistic calculations among the lowest 31 levels of the 3s 2 3p 5 , 3s3p 6 and 3s 2 3p 4 3d configurations.…”

Section: Introductionmentioning

confidence: 99%

Energy levels and radiative rates for transitions in Co XI

Aggarwal¹,

Keenan²,

Msezane

2007

A&A

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Aims. In this paper we report calculations for energy levels and radiative rates for transitions in Co xi.Methods. The General purpose Relativistic Atomic Structure Package (grasp) and the Flexible Atomic Code (fac) have been adopted for the calculations of energy levels and radiative rates.Results. Energies for the lowest 287 levels of Co xi, including those among the (1s 2 2s 2 2p 6 ) 3s 2 3p 5 , 3s3p 6 , 3s 2 3p 4 3d, 3s3p 5 3d, 3s 2 3p 3 3d 2 , and 3s 2 3p 4 4s configurations, are reported. Additionally, radiative rates and oscillator strengths are reported for all electric dipole (E1) transitions with f ≥ 10 −5 among these levels, and similar results for magnetic dipole (M1), electric quadrupole (E2), and magnetic quadrupole (M2) transitions are reported only for those with f ≥ 10 −8 . Comparisons are made with the available results in the literature, and the accuracy of the present data is assessed. Finally, lifetimes for all excited levels are also listed, although measurements are presently available for only one of these.

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“…Indeed, time-independent R-matrix calculations for the static Ar + structure, performed by the present authors, indicate that the dipole matrix element for a 3s → 3p transition can be up to an order of magnitude lower than those relevant for other transitions, including 3p → 4s, 3p → 3d, 3d → 4p and 4s → 4p. These predictions are supported by the data of both Hibbert and Hansen [60] and Berrington et al [61], which indicate that the corresponding discrepancy in oscillator strengths can readily exceed an order of magnitude. This would suggest that the first excited ( 2 S e ) state of Ar + may not be optimal for realising resonantly enhanced, multiphoton ionization yields in XIHHG schemes, or of driving HHG from an excited state.…”

Section: Cooper Minimummentioning

confidence: 52%

Extreme-ultraviolet-initiated high-order harmonic generation in Ar+

2018

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We employ the R-matrix with time-dependence method to investigate extreme-ultravioletinitiated high-harmonic generation (XIHHG) in Ar + . Using a combination of extreme-ultraviolet (XUV, 92 nm, 3 × 10 12 Wcm −2 ) and time-delayed, infrared (IR, 800 nm, 3 × 10 14 Wcm −2 ) laser pulses, we demonstrate that control over both the mechanism, and timing, of ionization can afford significant enhancements in the yield of plateau, and sub-threshold, harmonics alike. The presence of the XUV pulse is also shown to alter the relative contribution of different electron emission pathways. Manifestation of the Ar + electronic structure is found in the appearance of a pronounced Cooper minimum. Interferences amongst the outer-valence 3p, and inner-valence 3s, electrons are found to incur only a minor suppression of the harmonic intensities, at least for the present combination of XUV and IR laser light. Additionally, the dependence of the XIHHG efficiency on time delay is discussed, and rationalized with the aid of classical trajectory simulations.

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Oscillator strength for 3s²3p⁵-3s3p⁶in Cl-like ions

Cited by 22 publications

References 29 publications

Benchmarking atomic data for astrophysics: $\ion{Fe}{x}$

Benchmarking atomic data for astrophysics: $\ion{Fe}{x}$

Energy levels and radiative rates for transitions in Co XI

Extreme-ultraviolet-initiated high-order harmonic generation in Ar+

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