Sternheimer free determination of the47Ti nuclear quadrupole moment from hyperfine structure measurements

Aydin, R.; Stachowska, Ewa; Johann, Ulrich; Dembczyński, J.; Unkel, P.; Ertmer, W.

doi:10.1007/bf01437170

Cited by 46 publications

(65 citation statements)

References 20 publications

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“…We therefore use the experimental values for the relevant isotope where available, but use rescaled experimental data from the other where it does not exist for both isotopes. Data on hyperfine structure for the Ti  lines for which we have isotopic information are best obtained from Gangrsky et al (1995) and Aydin et al (1990). In cases of overlap, the ABMR data of Aydin et al have smaller uncertainties than those of Johann et al (1981), whereas the LFS data of Gangrsky et al is preferable to Aydin et al's LFS.…”

Section: Isotopic and Hyperfine Structurementioning

confidence: 93%

“…It has been consistently found that the hyperfine A constants for 47 Ti and 49 Ti are essentially equal, and B(47)/B(49) ≈ 1.22, for all levels (Channappa & Pendlebury 1965;Aydin et al 1990;Stachowska et al 1994;Gangrsky et al 1995). We therefore use the experimental values for the relevant isotope where available, but use rescaled experimental data from the other where it does not exist for both isotopes.…”

Section: Isotopic and Hyperfine Structurementioning

confidence: 99%

See 1 more Smart Citation

The elemental composition of the Sun

Scott

Asplund

Grevesse

et al. 2014

A&A

269

202

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We redetermine the abundances of all iron group nuclei in the Sun, based on neutral and singly-ionised lines of Sc, Ti, V, Mn, Fe, Co and Ni in the solar spectrum. We employ a realistic 3D hydrodynamic model solar atmosphere, corrections for departures from local thermodynamic equilibrium (NLTE), stringent line selection procedures and high quality observational data. We have scoured the literature for the best quality oscillator strengths, hyperfine constants and isotopic separations available for our chosen lines. We find log Sc = 3.16 ± 0.04, log Ti = 4.93 ± 0.04, log V = 3.89 ± 0.08, log Cr = 5.62 ± 0.04, log Mn = 5.42 ± 0.04, log Fe = 7.47 ± 0.04, log Co = 4.93 ± 0.05 and log Ni = 6.20 ± 0.04. Our uncertainties factor in both statistical and systematic errors (the latter estimated for possible errors in the model atmospheres and NLTE line formation). The new abundances are generally in good agreement with the CI meteoritic abundances but with some notable exceptions. This analysis constitutes both a full exposition and a slight update of the preliminary results we presented in Asplund et al. (2009, ARA&A, 47, 481), including full line lists and details of all input data we employed.

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Section: Isotopic and Hyperfine Structurementioning

confidence: 93%

Section: Isotopic and Hyperfine Structurementioning

confidence: 99%

The elemental composition of the Sun

Scott

Asplund

Grevesse

et al. 2014

A&A

269

202

View full text Add to dashboard Cite

show abstract

“…relative to Ti I [14] and Ti II [7]. Since these ratios are very close for these two neighbour elements in the Periodic Table, we can conclude that the deduced ( ) In Table 7 we have listed the measured hfs constants A given in MHz, used in our fitting procedure.…”

Section: Accurate Fine and Hyperfine Structure Analysismentioning

confidence: 66%

Fine Structure Analysis of the Configuration System of V II. Part I: Even-Parity Levels

Bouazza¹,

Holt²,

Rosner³

et al. 2014

JMP

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Using a linked-parameter technique of level-fitting calculations in a multi configuration basis, a parametric analysis of fine structure (fs) for even-parity levels of V II, involving six configurations, has been performed. This led us to exchange the assignments of two triplets, 3d 3 ( 2 F)4s c 3 F and 3d 4 d 3 F, reported in earlier analyses as being located at 30,300 cm −1 and 30,600 cm −1 , respectively. This is confirmed by experimental hyperfine structure (hfs) A constants, used as fingerprints. Moreover, the current singlet 3d 2 4s 2 1 D2 position is likely too high. The fs parameters, magnetic Landé g-factors, and the percentage of leading eigenvectors of levels are calculated. We present also predicted singlet, triplet and quintet positions for missing experimental levels up to 100,000 cm −1 . The single-electron hfs parameters are determined in their entirety for 51 V II for the model space (3d + 4s) 4 with good accuracy. For the model space (3d + 4s) 4 of 51 V II the single-electron hfs parameters are computed; furthermore, our achieved theoretical evaluations of the single-electron hfs parameters, thanks to the use of ab initio calculations, reinforce the validity of these hfs parameter values, deduced from experimental data.

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“…Later, in 1985, Dembczyński [25] elaborated a new parametrization method which took into account simultaneously one-and two-body interactions in atomic hfs structure of the configurations (3d+4s) N +2 . This method was applied to the interpretation of iron, vanadium, titanium and cobalt atoms [26][27][28][29]. In the following years, the above mentioned method of parametrization of interactions in the hfs was extended up to three open electronic shells [6,30].…”

Section: Electrostatically Correlated Hyperfine Interactions (Chfs)mentioning

confidence: 99%

Construction of the energy matrix for complex atoms

2016

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Abstract. The continuation of the previous series of papers related to the construction of the energy matrix for complex atoms is presented. The contributions from the second-order perturbation theory concerning electrostatically correlated spin-orbit interactions (CSO), as well as electrostatically correlated hyperfine interactions (CHFS) to the atomic structure of nl N , nl N n1lconfigurations, are considered. This theory assumes that the electron excitation n 0l0 → nl affects spin-orbit splitting and magnetic dipole and electric quadrupole hyperfine structure in the same way which will be discussed below. Part I of the series presented, in general terms, a method allowing the analysis of complex electronic systems. Parts II, III and IV provided a description of an electrostatic interaction up to second-order perturbation theory; they constitute the basis for the design of an efficient computer program package for large-scale calculations of accurate wave functions. Analyses presented in the entire series of our papers clearly demonstrate that obtaining the precise wave functions is impossible without considering the contribution from the second-order effects into fine and hyperfine atomic structure.

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Sternheimer free determination of the47Ti nuclear quadrupole moment from hyperfine structure measurements

Cited by 46 publications

References 20 publications

The elemental composition of the Sun

The elemental composition of the Sun

Fine Structure Analysis of the Configuration System of V II. Part I: Even-Parity Levels

Construction of the energy matrix for complex atoms

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