Lifetime measurements and calculations in Y+ and Y2+ ions

Biémont, Émile; Blagoev, K.; Engström, Lars; Hartman, Henrik; Lundberg, Hans; Malcheva, G.; Nilsson, Hampus; Whitehead, R. Blackwell; Palmeri, P.; Quinet, Pascal

doi:10.1111/j.1365-2966.2011.18637.x

Cited by 75 publications

(53 citation statements)

References 26 publications

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“…Although the pair correlation (PC) terms are not as strong as CP, they are significant for precise calculations and are included in our present RCC formalism. Biémont et al [15] used core polarization correction as a modification of the relativistic Hartree-Fock method (HFR+CPOL) to calculate the oscillator strengths of various transitions of Y III. The all-order relativistic many-body perturbation theory (RMBPT) used by Safronova and Safronova [14], employs correlation operators associated with single and double excitations, but with a linearized approximation.…”

Section: Resultsmentioning

confidence: 99%

Electron-correlation study of Y iii-Tc vii ions using a relativistic coupled-cluster theory

Das

Bhowmik

Dutta

et al. 2017

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

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Abstract. Spectroscopic properties, useful for plasma diagnostics and astrophysics, of a few rubidium-like ions are studied here. We choose one of the simplest, but correlationally challenging series where d− and f − orbitals are present in the core and/or valence shells with 4d 2 D 3/2 as the ground state. We study different correlation characteristics of this series and make precise calculations of electronic structure and rates of electromagnetic transitions. Our calculated lifetimes and transition rates are compared with other available experimental and theoretical values. Radiative rates of vacuum ultra-violet electromagnetic transitions of the long lived Tc 6+ ion, useful in several areas of physics and chemistry, are estimated. To the best of our knowledge, there is no literature for most of these transitions.Electron-correlation study of Y III-Tc VII ions using a relativistic coupled-cluster theory 2

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Section: Resultsmentioning

confidence: 99%

Electron-correlation study of Y iii-Tc vii ions using a relativistic coupled-cluster theory

Das

Bhowmik

Dutta

et al. 2017

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

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“…References are MA60 for Martin (1960), DR2006 for Drake (2006), NS81 for Nussbaumer & Storey (1981), KZ91 for Butler, K. & Zeippen, C. J. (1991), W96 for Wiese et al (1996), HBGV91 for Hibbert et al (1991), Si98 for Siegel et al (1998), K79 for Kaufman & Hagan (1979), H99 for Hannaford (1999), Ma01 for Matheron et al (2001), Sh61 for Shenstone (1961), LD89 for Lawler & Dakin (1989), FMW for Fuhr et al (1988), PTP for Pickering et al (2002), SN14 for Sansonetti & Nave (2014), NJ13 for Nave & Johansson (2013), T89 for Theodosiou (1989), RU98 for Raassen & Uylings (1998), PBL95 for Pinnington et al (1995), NBS for Miles & Wiese (1969), KO83 for Kostyk & Orlova (1983), Bie11 for Biémont et al (2011),L06 for Ljung et al (2006), MCS75 for Meggers et al (1975), BL48 for Biermann & Lübeck (1948), Bal81 for Biemont et al (1981), KL01 for Kling et al (2001), DSVD92 for Davidson et al (1992), SR01 for Sansonetti & Reader (2001), Do03 for Dolk et al (2003)…”

Section: Discussionmentioning

confidence: 99%

The nature of the late B-type stars HD 67044 and HD 42035

Monier

Gebran

Royer

2016

Astrophys Space Sci

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While monitoring a sample of apparently slowly rotating superficially normal bright late B and early A stars in the northern hemisphere, we have discovered that HD 67044 and HD 42035, hitherto classified as normal late B-type stars, are actually respectively a new chemically peculiar star and a new spectroscopic binary containing a very slow rotator HD 42035 S with ultra-sharp lines (vsini = 3.7 km/s) and a fast rotator HD 42035 B with broad lines. The lines of Ti, Cr, Mn, Sr, Y, Zr and Ba are conspicuous features in the high resolution SOPHIE spectrum of HD 67044. The HgII line at 3983.93 A is also present as a weak feature. The composite spectrum of HD 42035 is characterised by very sharp lines formed in HD 42035 S superimposed onto the shallow and broad lines of HD 42035 B. These very sharp lines are mostly due to light elements from C to Ni, the only heavy species definitely present are Sr and Ba. Selected lines of 21 chemical elements from He up to Hg have been synthesized using model atmospheres computed with ATLAS9 and the spectrum synthesis code SYNSPEC48 including hyperfine structure of various isotopes when relevant. Abundances of these key elements have been derived HD 67044 and HD 42035 S. HD 67044 is found to have distinct enhancements of Ti, Cr, Mn, Sr, Y, Zr, Ba and Hg and underabundances in He, C, O, Ca and Sc which shows that this star is not a superficially normal late B-type star, but actually is a new CP star most likely of the HgMn type. HD 42035 S has provisional underabundances of the light elements from C to Ti and overabundances of heavier elements up to barium. More accurate fundamental parameters and abundances for HD 42035 S and HD 42035 B will be derived if we manage to disentangle their spectra. They will help clarify the status of the two components in this interesting new spectroscopic binary.Comment: 30 pages, 4 figures, 2 tables, accepted in APSS. arXiv admin note: text overlap with arXiv:1504.0272

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“…The star-to-star scatter is rel- (Sneden 1973). Using the transition probabilities of Hannaford et al (1982) and Biémont et al (2011), we used ten Y ii lines to derive For Star 2, we display our synthetic/observed spectrum match in Fig. 7.…”

Section: Neutron-capture Elementsmentioning

confidence: 99%

Chemical characterisation of the globular cluster NGC 5634 associated to the Sagittarius dwarf spheroidal galaxy

Carretta

Bragaglia

Lucatello

et al. 2017

A&A

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As part of our on-going project on the homogeneous chemical characterisation of multiple stellar populations in globular clusters (GCs), we studied NGC 5634, associated to the Sagittarius dwarf spheroidal galaxy, using high-resolution spectroscopy of red giant stars collected with VLT/FLAMES. We present here the radial velocity distribution of the 45 observed stars, 43 of which are cluster members, the detailed chemical abundance of 22 species for the seven stars observed with UVES-FLAMES, and the abundance of six elements for stars observed with GIRAFFE. On our homogeneous UVES metallicity scale, we derived a low-metallicity [Fe/H] = −1.867 ± 0.019 ± 0.065 dex (±statistical ±systematic error) with σ = 0.050 dex (7 stars). We found the normal anticorrelations between light elements (Na and O, Mg and Al), a signature of multiple populations typical of massive and old GCs. We confirm the associations of NGC 5634 to the Sgr dSph, from which the cluster was lost a few Gyr ago, on the basis of its velocity and position, and the abundance ratios of α and neutron capture elements.

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Lifetime measurements and calculations in Y+ and Y2+ ions

Cited by 75 publications

References 26 publications

Electron-correlation study of Y iii-Tc vii ions using a relativistic coupled-cluster theory

Electron-correlation study of Y iii-Tc vii ions using a relativistic coupled-cluster theory

The nature of the late B-type stars HD 67044 and HD 42035

Chemical characterisation of the globular cluster NGC 5634 associated to the Sagittarius dwarf spheroidal galaxy

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