The Isotope Effect in the Spectra of the Heavy Elements

Golovin, A. F.; Striganov, A. R.

doi:10.1070/pu1968v010n05abeh005851

Cited by 10 publications

(4 citation statements)

References 3 publications

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“…Mo consists of a pot pouri of different isotopes, but the two lines we use are very weak, and their isotopic splitting is small (Hughes 1961;Golovin & Striganov 1968). We can therefore safely ignore isotopic and hyperfine structure for these lines.…”

Section: Molybdenummentioning

confidence: 99%

The elemental composition of the Sun

Grevesse

Scott

Asplund

et al. 2014

A&A

211

252

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We re-evaluate the abundances of the elements in the Sun from copper (Z = 29) to thorium (Z = 90). Our results are mostly based on neutral and singly-ionised lines in the solar spectrum. We use the latest 3D hydrodynamic solar model atmosphere, and in a few cases also correct for departures from local thermodynamic equilibrium (LTE) using non-LTE (NLTE) calculations performed in 1D. In order to minimise statistical and systematic uncertainties, we make stringent line selections, employ the highest-quality observational data and carefully assess oscillator strengths, hyperfine constants and isotopic separations available in the literature, for every line included in our analysis. Our results are typically in good agreement with the abundances in the most pristine meteorites, but there are some interesting exceptions. This analysis constitutes both a full exposition and a slight update of the relevant parts 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 that we have employed.

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Section: Molybdenummentioning

confidence: 99%

The elemental composition of the Sun

Grevesse

Scott

Asplund

et al. 2014

A&A

211

252

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“…The isotope nearest to the selected one and having largest abundance is 174 Yb which is considered to be the unselected isotope. The reported values (Golovin and Striganov 1965) of the isotope shift corresponding to the first and second steps equal to 1.04 and 0.46 GHz, respectively are taken. Considering the laser line with ν L = ν D tuned to the absorption line of the 172 Yb isotope and the mismatch of the laser line relative to the absorption line of 174 Yb isotope, we have calculated the excitation cross sections of the selected and unselected isotopes using equations ( 15) and ( 16).…”

Section: Results For 172 Yb Systemmentioning

confidence: 99%

Ionization yield and isotopic selectivity of three-step photoionization of atoms by pulsed lasers

Gupta

Suri

2002

J. Phys. D: Appl. Phys.

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Estimate of ionization yield and selectivity in multi-step photoionization is of interest in studies related to trace analysis and laser isotope separation. Analytical expressions of ionization yield for the desired and interfering isotopes have been derived by solving rate equations for three-step photoionization. The partial overlap of absorption lines of the isotopes and the charge exchange of the ions of the desired isotope with the atoms of the interfering isotope have been considered. The ionization yield and the isotopic selectivity of the photoionization process are calculated for ytterbium isotopes, considering various atomic and laser parameters. Numerical results have been discussed, showing the effect of both factors on the ionization yield and the isotopic selectivity of the process.

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“…Earlier Doppler-limited IS measurements were reported in spectral line at 3694.19Å (Krebs and Nelkowski [1], Golovin and Striganov [2] and Chaiko [3]) and in lines at 2970.56Å, 3031.11Å and 3289.37Å [3]. All the four lines involve the ground state level 2 S 1/2 of 4f 14 6s configuration: two lines at 3694.19Å (D 1 line) and 3289.37Å (D 2 line) belong to 4f 14 6p − 4f 14 6s transition, whereas the lines at 2970.56Å and 3031.11Å belong to 4f 13 5d6s − 4f 14 6s transition.…”

Section: Introductionmentioning

confidence: 96%

“…All the four lines involve the ground state level 2 S 1/2 of 4f 14 6s configuration: two lines at 3694.19Å (D 1 line) and 3289.37Å (D 2 line) belong to 4f 14 6p − 4f 14 6s transition, whereas the lines at 2970.56Å and 3031.11Å belong to 4f 13 5d6s − 4f 14 6s transition. Golovin and Striganov [2] measured IS involving all even-A (A = 168, 170, 172, 174 and 176) isotopes of ytterbium and using the relative IS values they evaluated the static quadrupole moment Q 0 of rare stable isotope 168 Yb. Chaiko [3] measured IS in 3694Å line of Yb II and apart from even-A isotopes mentioned above, he measured IS and hyperfine structure of the odd isotopes 171 Yb and 173 Yb; he also evaluated Q 0 of 168 Yb.…”

Section: Introductionmentioning

confidence: 99%

Isotope shifts in spectral lines of Yb+ in 322-615nm region and term shifts of odd and even parity energy levels of Yb II

Ahmad

Rao

Afzal

1997

Z Phys D - Atoms, Molecules and Clusters

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Isotope shift ∆σ( 172 Yb − 176 Yb) has been measured in 79 classified lines of Yb II in the region 3225-6155Å. Earlier studies provide isotope shift data in just six lines of Yb II. Term isotope shift ∆T ( 172 Yb-176 Yb) have been evaluated for 38 even and 30 odd parity levels of Yb II, using the present isotope shift data. The ∆T values have been discussed and correlated with the purity of the configuration assigned to an energy level, which enabled to check the reported eigenvector percentages of different configurations for some of the levels of Yb II. ∆T values of different levels resulting from J I L II couplings are also discussed.

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The Isotope Effect in the Spectra of the Heavy Elements

Cited by 10 publications

References 3 publications

The elemental composition of the Sun

The elemental composition of the Sun

Ionization yield and isotopic selectivity of three-step photoionization of atoms by pulsed lasers

Isotope shifts in spectral lines of Yb+ in 322-615nm region and term shifts of odd and even parity energy levels of Yb II

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