Hyperfine structure of the 4f
7 (8
S
0) 6s
7
S
03 level in151,153Eu II by fast ion beam — laser spectroscopy

Villemoes, P.; Wang, Mingqi

doi:10.1007/bf01437473

Cited by 7 publications

(5 citation statements)

References 17 publications

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“…In the spectral synthesis calculations, the Eu  line was substituted by its HFS components, calculated by us using Casimir's equation (Casimir 1963), and HFS laboratory data from Becker et al (1993), Broström et al (1995), Villemoes &Wang (1994), andMöller et al (1993). Isotope shift was taken into account, using data from Broström et al (1995) and the solar abundance isotopic ratio ε( 151 Eu)/ε( 153 Eu) = 1.00±0.29 (Lawler et al 2001).…”

Section: Spectral Synthesismentioning

confidence: 99%

The age of the Galactic thin disk from Th/Eu nucleocosmochronology

Peloso

Silva

Mello

et al. 2005

A&A

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Abstract. The first determination of the age of the Galactic thin disk from Th/Eu nucleocosmochronology was accomplished by us in Papers I and II. The present work aimed at reducing the age uncertainty by expanding the stellar sample with the inclusion of seven new objects -an increase by 37%. A set of [Th/Eu] abundance ratios was determined from spectral synthesis and merged with the results from Paper I. Abundances for the new, extended sample were analyzed with the aid of a Galactic disk chemical evolution (GDCE) model developed by us is Paper II. The result was averaged with an estimate obtained in Paper II from a conjunction of literature data and our GDCE model, providing our final, adopted disk age T G = (8.8 ± 1.7) Gyr with a reduction of 0.1 Gyr (6%) in the uncertainty. This value is compatible with the most up-to-date white dwarf age determinations ( 10 Gyr). Considering that the halo is currently presumed to be (13.5 ± 0.7) Gyr old, our result prompts groups developing Galactic formation models to include an hiatus of (4.7 ± 1.8) Gyr between the formation of halo and disk.

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Section: Spectral Synthesismentioning

confidence: 99%

The age of the Galactic thin disk from Th/Eu nucleocosmochronology

Peloso

Silva

Mello

et al. 2005

A&A

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“…Eu abundances were taken from del Peloso et al (2005). They were obtained from spectral synthesis of the Eu  line at 4129.72 Å. HFS was calculated by us in exactly the same way as for Co, using data from Becker et al (1993), Möller et al (1993), Villemoes & Wang (1994), and Broström et al (1995). Isotope shift was taken into account, using data from Broström et al (1995) and the solar abundance isotopic ratio ε( 151 Eu)/ε( 153 Eu) = 1.00 ± 0.29 (Lawler et al 2001).…”

Section: Europiummentioning

confidence: 99%

Abundances of Mn, Co and Eu in a sample of 20 F–G disk stars: the influence of hyperfine structure splitting

Peloso¹,

Cunha²,

Silva³

et al. 2005

A&A

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We present Mn, Co and Eu abundances for a sample of 20 disk F and G dwarfs and subgiants with metallicities in the range −0.8 ≤ [Fe/H] ≤ +0.3. We investigate the influence of hyperfine structure (HFS) on the derived abundances of Mn and Co by using HFS data from different sources in the literature, as well as calculated HFS from interaction factors A and B. Eu abundances were obtained from spectral synthesis of one Eu  line that takes into account HFS from a series of recent laboratory measurements. For the lines analysed in this study, we find that for manganese, the differences between abundances obtained with different HFSs are no greater than 0.10 dex. Our cobalt abundances are even less sensitive to the choice of HFS than Mn, presenting a 0.07 dex maximum difference between determinations with different HFSs. However, the cobalt HFS data from different sources are significantly different. Our abundance results for Mn offer an independent confirmation of literature results, favouring type Ia supernovae as the main nucleosynthesis site of Mn production, in contrast to trends of Mn versus metallicity previously reported in the literature. The observed discrepancies may be attributed to the lack of HFS in the works we used for comparison. Our results for Eu are in accordance with low-mass type II supernovae being the main site of the r-process nucleosynthesis.

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“…LIF measurements on the metastable 4f 7(8So)6s level are included in Table 4 7S 3 o (Villemoes & Wang 1994). These LIF measurements have also been superceded by extraordinarily accurate RF measurements (Revalde et al 1998).…”

Section: Hyperfine and Isotopic Structurementioning

confidence: 99%

“…LIF measurements of the hfs A and B values for Ðve of the levels of the and conÐgu-4f 7(8S 7@2 o )6p 3@2 4f 7(8S 7@2 o )6p 1@2 rations by Arnesen et al (1981), Villemoes et al (1992), and Villemoes & Wang (1994) (Brostro m et al 1995). All lines connecting these same conÐgurations are expected to have nearly the same isotope shift, approximately [145^10 mK, with some variation from line to line.…”

Section: Hyperfine and Isotopic Structurementioning

confidence: 99%

Improved Laboratory Transition Parameters for Euiiand Application to the Solar Europium Elemental and Isotopic Composition

Lawler

Wickliffe

Hartog

et al. 2001

ApJ

342

279

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New radiative lifetime measurements using time-resolved laser-induced Ñuorescence are reported for the lowest six even-parity levels of Eu II. Branching fractions, measured from Fourier transform spectra, are combined with these lifetimes to determine atomic transition probabilities for the strongest blueÈUV lines and additional yellowÈred lines of Eu II. These results are compared with published data, and generally good agreement is found. Recommended hyperÐne structure constants and isotopic shifts for these lines are also assembled from the literature and supplemented, as needed, using results from nonlinear least-squares Ðts of line proÐles in Fourier transform spectra. These laboratory data are applied in a new determination of the solar Eu elemental abundance, yielding with^0.04 Slog 10 e(Eu)T \ 0.52^0.01, estimated for each of internal (scatter) and external (systematic) uncertainties. From analysis of the proÐles of three Eu II lines, primarily j4129, isotopic fractions of 151Eu and 153Eu are shown to be consistent with their values in meteoritic material.

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Hyperfine structure of the 4f 7 (8 S 0) 6s 7 S 03 level in151,153Eu II by fast ion beam — laser spectroscopy

Abstract: Abstract. The

Cited by 7 publications

References 17 publications

The age of the Galactic thin disk from Th/Eu nucleocosmochronology

The age of the Galactic thin disk from Th/Eu nucleocosmochronology

Abundances of Mn, Co and Eu in a sample of 20 F–G disk stars: the influence of hyperfine structure splitting

Improved Laboratory Transition Parameters for Euiiand Application to the Solar Europium Elemental and Isotopic Composition

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