Lifetime measurements and calculations in singly ionized ytterbium

Biémont, Émile; Quinet, Pascal; Dai, Zhenwen; Jiang, Zhaoqiang; Zhang, Zhiguo; Xu, Huailiang; Svanberg, Sune

doi:10.1088/0953-4075/35/22/315

Cited by 22 publications

(12 citation statements)

References 37 publications

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“…We adopted the transition probabilities of Biémont et al (1998) renormalized to the lifetime results of Pinnington, Rieger, & Kernahan (1997): log gf 3289 = +0.02, and log gf 3694 = −0.30. These values are close to those derived from Biémont et al (2002), as given in the D.R.E.A.M. database 9 : log gf 3289 = −0.05, and log gf 3694 = −0.32.…”

Section: Discussionsupporting

confidence: 88%

NEW RARE EARTH ELEMENT ABUNDANCE DISTRIBUTIONS FOR THE SUN AND FIVE r -PROCESS-RICH VERY METAL-POOR STARS

Sneden

Lawler

Cowan

et al. 2009

ApJS

200

189

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We have derived new abundances of the rare-earth elements Pr, Dy, Tm, Yb, and Lu for the solar photosphere and for five very metal-poor, neutron-capture r-process-rich giant stars. The photospheric values for all five elements are in good agreement with meteoritic abundances. For the low metallicity sample, these abundances have been combined with new Ce abundances from a companion paper, and reconsideration of a few other elements in individual stars, to produce internally-consistent Ba, rare-earth, and Hf (56 ≤ Z ≤ 72) element distributions. These have been used in a critical comparison between stellar and solar r-process abundance mixes.

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Section: Discussionsupporting

confidence: 88%

NEW RARE EARTH ELEMENT ABUNDANCE DISTRIBUTIONS FOR THE SUN AND FIVE r -PROCESS-RICH VERY METAL-POOR STARS

Sneden

Lawler

Cowan

et al. 2009

ApJS

200

189

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“…Ytterbium (Z ¼ 70, Yb ii).-The g f-value was adopted from Biémont et al (2002). The feature is displayed in Figure 5.…”

Section: Comments On Abundance Derivations Of Individual Elementsmentioning

confidence: 99%

Near‐Ultraviolet Observations of HD 221170: New Insights into the Nature ofr‐Process–rich Stars

Ivans

Simmerer

Sneden

et al. 2006

ApJ

238

255

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Employing high-resolution spectra obtained with the near-UV-sensitive detector on the Keck I HIRES, supplemented by data obtained with the McDonald Observatory 2d-coudé, we have performed a comprehensive chemical composition analysis of the bright r-process-rich metal-poor red giant star HD 221170. Analysis of 57 individual neutral and ionized species yielded abundances for a total of 46 elements and significant upper limits for an additional five. Model stellar atmosphere parameters were derived with the aid of $200 Fe peak transitions. From more than 350 transitions of 35 neutron-capture (Z > 30) species, abundances for 30 neutron-capture elements and upper limits for three others were derived. Utilizing 36 transitions of La, 16 of Eu, and seven of Th, we derive ratios of log (Th / La) ¼ À0:73 (¼ 0:06) and log (Th /Eu) ¼ À0:60 (¼ 0:05), values in excellent agreement with those previously derived for other r-process-rich metal-poor stars such as CS 22892À052, BD +17 3248, and HD 115444. Based on the Th/Eu chronometer, the inferred age is 11:7 AE 2:8 Gyr. The abundance distribution of the heavier neutron-capture elements (Z ! 56) is fitted well by the predicted scaled solar system r-process abundances, as also seen in other r-process-rich stars. Unlike other r-process-rich stars, however, we find that the abundances of the lighter neutron-capture elements (37 < Z < 56) in HD 221170 are also in agreement with the abundances predicted for the scaled solar r-process pattern.

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“…It has been shown in previous papers (see e.g. Biémont et al 2002, Dai et al 2003, Zhang et al 2002a, 2002c) that, for heavy ions such as neutral, singly or doubly ionized lanthanides,the consideration of both intravalence and core-valence correlation is essential in atomic structure calculations. In many different situations, the HFR method, described by Cowan (1981), has appeared usable and reliable (9) a The number between parentheses corresponds to the estimated error on the last digit.…”

Section: Branching Fraction Calculationsmentioning

confidence: 99%

Time-resolved laser-induced fluorescence lifetime measurements and relativistic Hartree–Fock calculations of transition probabilities in Sm II

Xu¹,

Svanberg²,

Quinet

et al. 2003

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

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Radiative lifetime measurements were performed with time-resolved laserinduced fluorescence techniques for 47 levels of the astrophysically important ion Sm 1+ over the energy range 21 000-36 000 cm −1 . The new results have been compared with previous measurements but also with theoretical calculations taking configuration interactions and core-polarization effects into account, and a satisfying agreement has been found for many levels of this complex ion. New calculated transition probabilities are deduced from the experimental lifetimes and from the theoretical branching fractions for 162 transitions of astrophysical interest. These results will help astrophysicists in the quantitative investigation of the chemical composition of CP stars.

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Lifetime measurements and calculations in singly ionized ytterbium

Cited by 22 publications

References 37 publications

NEW RARE EARTH ELEMENT ABUNDANCE DISTRIBUTIONS FOR THE SUN AND FIVE r -PROCESS-RICH VERY METAL-POOR STARS

NEW RARE EARTH ELEMENT ABUNDANCE DISTRIBUTIONS FOR THE SUN AND FIVE r -PROCESS-RICH VERY METAL-POOR STARS

Near‐Ultraviolet Observations of HD 221170: New Insights into the Nature ofr‐Process–rich Stars

Time-resolved laser-induced fluorescence lifetime measurements and relativistic Hartree–Fock calculations of transition probabilities in Sm II

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