Branching ratios and lifetimes for the low-lying levels of Fe xx

Dong, Chenzhong; Fritzsche, S.; Fricke, B.; Sepp, W.‐D.

doi:10.1046/j.1365-8711.1999.02649.x

Cited by 44 publications

(39 citation statements)

References 22 publications

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“…Deb et al (2002) have used the well-known CIV3 structure code of A. Hibbert and calculated radiative data for the lowest 4 configurations but including configuration interaction (CI) between 30 configurations (up to n = 4) that involved one-, two-, and three-electron excitations with respect to the ground (a total of 1351 levels). As in the case of the Dong et al (1999) calculation, the agreement with observations for the lowerenergy states is reasonably good, while for the rest, differences are large. For the strongest Fe  transition, the difference is about 19 000 cm −1 , producing a displacement of 6 Å.…”

Section: Theoretical Energiessupporting

confidence: 71%

“…Dong et al (1999) have performed a multi-configuration Dirac-Fock (MCDF) calculation using the well-known GRASP92 code of I. Grant for the lowest 3 configurations (31 fine-structure levels).…”

Section: Theoretical Energiesmentioning

confidence: 99%

“…However, for the quadrupole E2 and M2 transitions (that have a dependence on the fifth power), the errors introduced by using theoretical energies can be significant. Again considering Fe , for example, the A-values published by Dong et al (1999) and Deb et al (2002) could have been much improved if observed energies had been used. Dong et al (1999) calculates a value of 65 s −1 for the famous Fe  6374.6 Å forbidden transition within the ground configuration, compared to the commonly accepted value of 69 s −1 , the same calculated here.…”

Section: Radiative Datamentioning

confidence: 99%

“…Again considering Fe , for example, the A-values published by Dong et al (1999) and Deb et al (2002) could have been much improved if observed energies had been used. Dong et al (1999) calculates a value of 65 s −1 for the famous Fe  6374.6 Å forbidden transition within the ground configuration, compared to the commonly accepted value of 69 s −1 , the same calculated here. In this paper, the iterative procedure outlined above is implemented, in order to obtain the best energies and line strengths.…”

Section: Radiative Datamentioning

confidence: 99%

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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: Theoretical Energiessupporting

confidence: 71%

Section: Theoretical Energiesmentioning

confidence: 99%

Section: Radiative Datamentioning

confidence: 99%

Section: Radiative Datamentioning

confidence: 99%

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

Zanna¹,

Berrington

Mason³

2004

A&A

100

114

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“…i Bhatia and Doschek (1995). j Kohstall et al (1999), Dong et al (1999). k Moehs et al (2000Moehs et al ( , 2001.…”

Section: Data Evaluation and Resultsmentioning

confidence: 99%

M1/E2 transition rates in FeXthrough FeXIIImeasured at a heavy-ion storage ring

Trabert

Gwinner

Wolf

et al. 2002

J. Phys. B: At. Mol. Opt. Phys.

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The rates of several electric-dipole forbidden decays of 3p and 3d levels in Cl-, S-, P-and Si-like ions of Fe have been measured optically at a heavy-ion storage ring. In several cases, more than one decay contributes to a given decay curve, which complicates the analysis. The lifetime results, with a precision range from 0.6 to 20%, compare well with some theoretical predictions, but are more precise. They are also more precise than some experimental data from an electrostatic ion trap.

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