Isotope shifts and hyperfine structure in near-ultraviolet transitions of Pb I by Doppler-free saturation spectroscopy

Bouazza, S.; Gough, D. S.; Hannaford, Peter; Löwe, R. M.; Wilson, M

doi:10.1103/physreva.63.012516

Cited by 32 publications

(23 citation statements)

References 24 publications

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“…We hope that this work can be a stimulus for further experimental HFS and IS investigations in Zr II: this element is light and then the expected Doppler width of lines, which is inversely proportional to the square root of the mass, is surely consequent and unfortunately constitutes a real handicap (see, e.g., the difference between figures of recorded spectra of one line of a light element: arsenic [37] and another line of a heavy element: lead [38]); so the predicted A, VS, and SMS values given in Table III and VII can help to simulate the shapes of lines under study with laser spectroscopy.…”

Section: Discussionmentioning

confidence: 98%

Semiempirical hyperfine structure and ab initio isotope shift predictions in Zr II

Bouazza

2011

Int J of Quantum Chemistry

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ABSTRACT:The fine structure of the even-parity low configurations has been reanalyzed by simultaneous parameterization of the one-and two-body interactions for the model space (4d þ 5s) 3 . Using the calculated eigenfunctions, the magnetic-dipole A hyperfine constants for the whole 37 existing levels of the model space were predicted and compared partially to those obtained using relativistic configuration-interaction approach. Moreover, volume shifts (VS) and specific mass shifts (SMS) of numerous configurations of singly ionised zirconium are deduced by means of ab initio estimates combined with a few experimental isotope shift data available in literature: VS (4d 1 5s 2 )

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Section: Discussionmentioning

confidence: 98%

Semiempirical hyperfine structure and ab initio isotope shift predictions in Zr II

Bouazza

2011

Int J of Quantum Chemistry

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“…Energy levels are adopted from Wood & Andrew (1968). The hfs A values are adopted from Bouazza et al (2000) for all lines. The IS are adopted from Bouazza et al for the λλ3639, 3683, and 4057 lines and Thompson et al (1983) for the λ2833 line.…”

Section: Appendix C New Hfs Patterns For Neutral Leadmentioning

confidence: 99%

NEW HUBBLE SPACE TELESCOPE OBSERVATIONS OF HEAVY ELEMENTS IN FOUR METAL-POOR STARS

Roederer

Lawler

Sobeck

et al. 2012

ApJS

136

127

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Elements heavier than the iron group are found in nearly all halo stars. A substantial number of these elements, key to understanding neutron-capture nucleosynthesis mechanisms, can only be detected in the near-ultraviolet. We report the results of an observing campaign using the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope to study the detailed heavy-element abundance patterns in four metal-poor stars. We derive abundances or upper limits from 27 absorption lines of 15 elements produced by neutron-capture reactions, including seven elements (germanium, cadmium, tellurium, lutetium, osmium, platinum, and gold) that can only be detected in the near-ultraviolet. We also examine 202 heavy-element absorption lines in ground-based optical spectra obtained with the Magellan Inamori Kyocera Echelle Spectrograph on the Magellan-Clay Telescope at Las Campanas Observatory and the High Resolution Echelle Spectrometer on the Keck I Telescope on Mauna Kea. We have detected up to 34 elements heavier than zinc. The bulk of the heavy elements in these four stars are produced by r-process nucleosynthesis. These observations affirm earlier results suggesting that the tellurium found in metal-poor halo stars with moderate amounts of r-process material scales with the rare earth and third r-process peak elements. Cadmium often follows the abundances of the neighboring elements palladium and silver. We identify several sources of systematic uncertainty that must be considered when comparing these abundances with theoretical predictions. We also present new isotope shift and hyperfine structure component patterns for Lu ii and Pb i lines of astrophysical interest.

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“…The method of calculation used to obtain the results in this work is based on the so‐called pseudo‐relativistic Hartree–Fock (PSUHFR) procedure, whose usefulness for the interpretation of IS studies was tested, for example, on Ce II38 and Pb I39. This procedure includes, as in the Cowan code, the mass‐velocity and Darwin terms of the Pauli approximation into the usual nonrelativistic Hartree–Fock (NRHF) Hamiltonian.…”

Section: Is Evaluationsmentioning

confidence: 99%

Investigations of hyperfine structure and isotope shift predictions in Hf II

Bouazza¹

2011

Int J of Quantum Chemistry

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ABSTRACT:The fine structure of the even-parity low configurations of singly ionized hafnium has been reanalyzed by simultaneous parameterization of the one-and two-body interactions for the model space (5d þ 6s) 3 . Using the calculated eigenfunctions, the magnetic-dipole A hyperfine constants for the whole 37 existing levels of the model space were predicted and compared partially with those obtained using relativistic configuration-interaction approach. Moreover, combined with experimental data, previously given in the literature, and pseudo-relativistic HartreeFock estimates, the field shifts (FSs) and specific mass shifts (SMSs) of numerous configurations are deduced: FS (5d 1 6s 2 ) ¼

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Isotope shifts and hyperfine structure in near-ultraviolet transitions of Pb I by Doppler-free saturation spectroscopy

Cited by 32 publications

References 24 publications

Semiempirical hyperfine structure and ab initio isotope shift predictions in Zr II

Semiempirical hyperfine structure and ab initio isotope shift predictions in Zr II

NEW HUBBLE SPACE TELESCOPE OBSERVATIONS OF HEAVY ELEMENTS IN FOUR METAL-POOR STARS

Investigations of hyperfine structure and isotope shift predictions in Hf II

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