Isotope shifts and hyperfine structure in the 369.4-nm 6<i>s</i>-6<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msub><mml:mrow><mml:mi mathvariant="italic">p</mml:mi></mml:mrow><mml:mrow><mml:mn>1</mml:mn><mml:mo>/</mml:mo><mml:mn>2</mml:mn></mml:mrow></mml:msub></mml:mrow></mml:math>resonance line of singly ionized ytterbium

Pendrill, Ann-Marie; Gough, D. S.; Hannaford, Peter

doi:10.1103/physreva.49.3351

Cited by 74 publications

(45 citation statements)

References 43 publications

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“…Ours is the first study on the electric quadrupole HFS constant of the 6p 3/2 state. Our result of Yb + is higher than the previous theoretical results of Martensson-Pendrill and collaborators [71] as well as the experimental results of Berends and Maleki [83].…”

Section: Hyperfine Structure Constant B Of P 3/2 Statescontrasting

confidence: 75%

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Fock-space relativistic coupled-cluster calculations of two-valence atoms

Mani

Angom

2011

Phys. Rev. A

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We have developed an all particle Fock-space relativistic coupled-cluster method for two-valence atomic systems. We then describe a scheme to employ the coupled-cluster wave function to calculate atomic properties. Based on these developments we calculate the excitation energies, magnetic hyperfine structure constants and electric dipole matrix elements of Sr, Ba and Yb. Further more, we calculate the electric quadrupole HFS constants and the electric dipole matrix elements of Sr + , Ba + and Yb + . For these we use the one-valence coupled-cluster wave functions obtained as an intermediate in the two-valence calculations. We also calculate the magnetic dipole hyperfine structure constants of Yb + .

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Section: Hyperfine Structure Constant B Of P 3/2 Statescontrasting

confidence: 75%

“…Our result of 6s 1/2 is slightly higher than both the theoretical and experimental values. However, for 6p 1/2 our result is lower than the previous theoretical result of Martensson [71] and closer to the experimental data [71]. Similarly, our result of 6p 3/2 is lower than the value of Martensson [71].…”

Section: B Hyperfine Structure Constantssupporting

confidence: 69%

Fock-space relativistic coupled-cluster calculations of two-valence atoms

Mani

Angom

2011

Phys. Rev. A

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“…They have renormalised theoretical oscillator strengths from Biémont et al (1998) using lifetimes from Pinnington et al (1997). The isotopic and hyperfine splitting data are taken from Mårtensson-Pendril et al (1994), and the solar isotopic ratios from Anders & Grevesse (1989) have been assumed.…”

Section: Continuedmentioning

confidence: 99%

The Hamburg/ESO R-process enhanced star survey (HERES)

Jonsell¹,

Barklem²,

Gustafsson³

et al. 2006

A&A

168

277

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We have derived abundances of 33 elements and upper limits for 6 additional elements for the metal-poor ([Fe/H] = −2.42) turn-off star HE 0338−3945 from high-quality VLT-UVES spectra. The star is heavily enriched, by about a factor of 100 relative to iron and the Sun, in the heavy s-elements (Ba, La, ...). It is also heavily enriched in Eu, which is generally considered an r-element, and in other similar elements. It is less enriched, by about a factor of 10, in the lighter s-elements (Sr, Y and Zr). C is also strongly enhanced and, to a somewhat lesser degree, N and O. These abundance estimates are subject to severe uncertainties due to NLTE and thermal inhomogeneities which are not taken into detailed consideration. However, an interesting result, which is most probably robust in spite of these uncertainties, emerges: the abundances derived for this star are very similar to those of other stars with an overall enhancement of all elements beyond the iron peak. We have defined criteria for this class of stars, r + s stars, and discuss nine different scenarios to explain their origin. None of these explanations is found to be entirely convincing. The most plausible hypotheses involve a binary system in which the primary component goes through its giant branch and asymptotic giant branch phases and produces CNO and s-elements which are dumped onto the observed star. Whether the r-element Eu is produced by supernovae before the star was formed (perhaps triggering the formation of a low-mass binary), by a companion as it explodes as a supernova (possibly triggered by mass transfer), or whether it is possibly produced in a high-neutron-density version of the s-process is still unclear. Several suggestions are made on how to clarify this situation.Key words. stars: population ii -stars: fundamental parameters -stars: abundances -Galaxy: halo -Galaxy: abundances -Galaxy: evolution IntroductionElements with atomic numbers Z > 30 are believed to be almost exclusively synthesized in neutron-capture (n-capture) reactions. In the most metal-poor stars the overall abundance of these elements varies from star to star, by more than a factor of 100 at a given metallicity (McWilliam et al. 1995;Ryan et al. 1996). Also, the different abundance ratios vary, e.g. the Ba/Eu ratio tends to decline with decreasing [Fe/H]

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“…Initial efforts focused on results for atomic ytterbium, specifically the Yb þ ion. M artensson-Pendrill et al [30] have performed a study of the hyperfine structure in the 369.4 nm Yb þ 6s-6p 1=2 transition; measurable differences in transition energy were found between the various isotopes. The measured shift between atomic lines of 174 Yb þ and 172 Yb þ isotopes was reported as )0.04254(2) cm À1 [30], and both the relative magnitude and sign are similar to the values obtained for the YbCl and YbBr molecules.…”

Section: Isotopic Electronic Energy Shifts In Ybbrmentioning

confidence: 97%