The classification of transitions between levels of principal quantum numbers 3 and 4 in Fe IX to XVI and Mn VIII to XV

Fawcett, B C; Kononov, É. Ya.; Hayes, R. W.; Cowan, Robert D.

doi:10.1088/0022-3700/5/6/028

Cited by 62 publications

(46 citation statements)

References 21 publications

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“…They are both large-scale calculations. Table 3 presents a selection of fine-structure target level energies E t , compared to experimental energies E exp (from Del Zanna et al 2004, for the n = 3 levels; otherwise from Fawcett et al 1972). There is good overall agreement in terms of energy differences between levels.…”

Section: The R-matrix and Dw Calculations For The N = 3 4 Levelsmentioning

confidence: 91%

“…This was followed by the monumental work by Fawcett et al (1972), where a number of lines arising from the 3s 2 3p 4 4l (l = s, p, d, f) levels were identified. It is important to keep in mind that only lines with strong oscillator strengths were identified, that some identifications were tentative, and that a large number of lines in the laboratory spectra were left unidentified.…”

Section: Previous Observations and Atomic Data For Fe Xmentioning

confidence: 99%

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Atomic data for astrophysics: Fe x soft X-ray lines

Zanna¹,

Storey

Badnell

et al. 2012

A&A

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New atomic calculations for Fe x are presented. They focus on the need to model the soft X-ray spectrum and in particular the line at 94.0 Å which is the dominant contribution to the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA) 94 Å band in quiet Sun conditions. This line, and others in the band, are due to strong decays from n = 4 levels. We present new large-scale R-matrix (up to n = 4) and distorted-wave (DW, up to n = 6) scattering calculations for electron collisional excitation and compare them to earlier work. We find significant discrepancies with previous calculations. We show that resonances significantly increase the cross-sections for excitations from the ground state to some n = 4 levels, in particular to those in the 3s 2 3p 4 4s configuration. Cascading from higher levels is also important. We suggest a new identification for the 3s 3p 6 2 S 1/2 -3s 3p 5 4s 2 P 3/2 transition, that has a predicted intensity larger than the decays from the 3s 2 3p 4 4s levels which were identified by Edlén in 1936. The results presented here are relevant to our understanding of transitions from n = 4 levels in a wide range of other ions.

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Section: The R-matrix and Dw Calculations For The N = 3 4 Levelsmentioning

confidence: 91%

Section: Previous Observations and Atomic Data For Fe Xmentioning

confidence: 99%

Atomic data for astrophysics: Fe x soft X-ray lines

Zanna¹,

Storey

Badnell

et al. 2012

A&A

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“…The identifications of some of the 3s 2 3p 2 4l (l = p, d, f) levels are due to the fundamental work by Fawcett et al (1972), using laboratory spectra in the soft X-rays of n = 4 → n = 3 transitions. A few transitions were only tentatively identified, and the spectra contain a large number of unidentified lines.…”

Section: Previous Observations and Atomic Data For Fe XImentioning

confidence: 99%

“…The latter have been obtained from Del Zanna (2010) for the n = 3 levels, otherwise from the measurements of Edlén (1937) and Fawcett et al (1972). Some of the experimental energies of Fawcett et al (1972) have been slightly revised in the benchmark study of Del Zanna (2012), where also additional lines and levels have been identified.…”

Section: Notesmentioning

confidence: 99%

“…Fawcett et al 1968Fawcett et al , 1972Manson 1972;and Behring et al 1976). Very little atomic data are currently available for these ions and the majority of the spectral lines still await firm identification, despite the fact that various instruments are routinely observing the soft X-rays, such as the Atmospheric Imaging Assembly (AIA, see Lemen et al 2012), the Extreme ultraviolet Variability Experiment (EVE; Woods et al 2012) on-board the Solar Dynamic Observatory (SDO) and the Chandra Low Energy Transmission Grating spectrometer (LETG, see Brinkman et al 2000).…”

Section: Introductionmentioning

confidence: 99%

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Atomic data for astrophysics: Fe xi soft X-ray lines

Zanna¹,

Storey

2012

A&A

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We present new large-scale R-matrix (up to n = 4) and distorted wave (up to n = 6) scattering calculations for electron collisional excitation of Fe xi. These data are needed for the analysis of soft X-ray spectra of astrophysical plasmas, where strong n = 4 → n = 3 transitions are present. As found in previous work on Fe x, Fe xii, and Fe xiii, resonances from within the n = 4 levels and cascading from higher levels significantly increase the intensities of these lines. We provide a list of the strongest lines, many of which are unidentified. The present larger model produces intensities for decays from n = 3 levels mostly consistent with our previous work, however significant enhancements for some lower levels are found, in particular for the 3s 2 3p 3 3d 5 D which can be used to measure electron temperatures in the solar corona with the Hinode/EIS spectrometer.

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OSCILLATOR STRENGTHS FOR DIPOLE-ALLOWED FINE-STRUCTURE TRANSITIONS IN Fe XIII

Nahar

1999

Atomic Data and Nuclear Data Tables

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Oscillator strengths, line strengths, and transition probabilities for fine-structure levels in silicon-like iron, Fe XIII, are reported. The data obtained are for 1223 LS bound terms, 64,456 LS multiplets, and 307,863 fine-structure transitions. Calculations are carried out in LS coupling using the close coupling R-matrix approximation with a 14-term eigenfunction expansion. The fine-structure components are obtained through algebraic transformations. Present data considerably exceed the observed and the previously calculated data available, including those from the Opacity Project. Comparisons with previously measured and calculated values are made.

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The classification of transitions between levels of principal quantum numbers 3 and 4 in Fe IX to XVI and Mn VIII to XV

Cited by 62 publications

References 21 publications

Atomic data for astrophysics: Fe x soft X-ray lines

Atomic data for astrophysics: Fe x soft X-ray lines

Atomic data for astrophysics: Fe xi soft X-ray lines

OSCILLATOR STRENGTHS FOR DIPOLE-ALLOWED FINE-STRUCTURE TRANSITIONS IN Fe XIII

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