Zur Hyperfeinstruktur des Eu-II

Krebs, K.; Winkler, R.

doi:10.1007/bf01349368

Cited by 39 publications

(15 citation statements)

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“…These LIF measurements have also been superceded by extraordinarily accurate RF measurements (Revalde et al 1998). Older measurements on these levels by Krebs & Winkler (1960) are not included in the table ; these older measurements are less accurate but are in agreement with more recent measurements.…”

Section: Hyperfine and Isotopic Structurementioning

confidence: 66%

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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Section: Hyperfine and Isotopic Structurementioning

confidence: 66%

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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“…The synthetic spectra were produced using KURUCZ06 model atmospheres in conjunction with the 1D LTE code ATLAS, and the Eu line lists were constructed using hyperfine splitting information from Krebs & Winkler (1960) and Becker et al (1993). In addition, the isotopic ratio 0.5:0.5 for Eu 151:153 was adopted.…”

Section: Comparison With Previous Resultsmentioning

confidence: 99%

Origin of the heavy elements in HD 140283

Mello¹,

Barbuy²,

Spite³

et al. 2012

A&A

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Context. HD 140283 is a nearby (V = 7.7) subgiant metal-poor star, extensively analysed in the literature. Although many spectra have been obtained for this star, none showed a signal-to-noise (S/N) ratio high enough to enable a very accurate derivation of abundances from weak lines. Aims. The detection of europium proves that the neutron-capture elements in this star originate in the r-process, and not in the s-process, as recently claimed in the literature. Methods. Based on the OSMARCS 1D LTE atmospheric model and with a consistent approach based on the spectrum synthesis code Turbospectrum, we measured the europium lines at 4129 Å and 4205 Å, taking into account the hyperfine structure of the transitions. The spectrum, obtained with a long exposure time of seven hours at the Canada-France-Hawaii Telescope (CFHT), has a resolving power of 81 000 and a S/N ratio of 800 at 4100 Å. Results. We were able to determine the abundance A(Eu) = −2.35 ± 0.07 dex, compatible with the value predicted for the europium from the r-process. The abundance ratio [Eu/Ba] = +0.58 ± 0.15 dex agrees with the trend observed in metal-poor stars and is also compatible with a strong r-process contribution to the origin of the neutron-capture elements in HD 140283.

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“…In EuIl an IS of 168mK was observed for the isotope pair 153 151Eu in the transition 4f v6s-4f 65d6s [14]. [16].…”

Section: Specific Mass Shifts and Field Shifts In Sm II Linesmentioning

confidence: 97%

Isotope shifts in Sm II and changes in mean-square nuclear charge radii of the stable even Sm isotopes

1979

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lsotope shifts have been measured in SmlI from which the shifts between pure configurations 4f66s and 4f65d can be determined. The specific mass shift for such a "transition" was estimated to be (-1 _+2)inK for a change of two neutrons. The values derived for the change in the nuclear charge distribution, 6(r2), are in good agreement with the results obtained from isotope shift measurements in SmI (H. Brand et al.: J. Phys. B il, L99, 1978). The weighted mean values representing the best information on 6(re) presently available are in fm2: [144, 148]

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Zur Hyperfeinstruktur des Eu-II

Cited by 39 publications

References 0 publications

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

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

Origin of the heavy elements in HD 140283

Isotope shifts in Sm II and changes in mean-square nuclear charge radii of the stable even Sm isotopes

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