Fine and hyperfine structure in the atomic spectrum of niobium

Kröger, S.; Öztürk, I. K.; Acar, F. Gülay; Başar, Günay; Wyart, J.-F.

doi:10.1140/epjd/e2006-00207-y

Cited by 20 publications

(28 citation statements)

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“…We here continue our earlier systematic investigations of the spectrum of Nb I Kröger et al 2004Kröger et al , 2007Kröger et al , 2010Başar et al 2008;Er et al 2011). Our purpose is to supplement hyperfine structure (hfs) data for this element, in particular, to fill gaps for all energy levels of even parity with unknown hyperfine structure (hfs) constants.…”

Section: Introductionmentioning

confidence: 52%

“…The resulting hfs constants A exp and B exp are listed in Tables 3 and 4 for the levels of even and odd parity, respectively. Level energies are given according to Humphreys & Meggers (1945) and Kröger et al (2004Kröger et al ( , 2007, configurations and terms according to for levels of even parity and according to Kröger et al (2007) for levels of odd parity. The wavelength λ air given in the fifth column specifies the line that was used to determine the hfs constants A exp and B exp .…”

Section: Resultsmentioning

confidence: 99%

“…Notes. Configurations and terms according to Kröger et al (2007); the wavelength given in the fifth column specifies the line that was used to determine the A exp and B exp values; when a hyperfine structure constant was determined by more than one line, the weighted mean value A mean and A mean , respectively, are calculated, using error bar of A exp and B exp as weight. In column A mean , twice the standard deviation that resulted from the weighted mean value calculation is given as error.…”

Section: Discussionmentioning

confidence: 99%

“…E l , J l , E u and J u are the energy and total electronic angular momentum quantum number of the lower and upper level, respectively; intensities Int. according to Humphreys & Meggers (1945), energy levels according to Humphreys & Meggers (1945) and Kröger et al (2004Kröger et al ( , 2007; in the last column the fluorescence wavelength λ f in air is given for the LIFS measurements; nl: new line; nc: new classification; B(Ne): a neon line, B(Nb) blend by a niobium line, B(? ): blend by unclassified line.…”

Section: Hyperfine Structure Analysismentioning

confidence: 99%

“…Doppler-limited measurements of hfs constants have been made using Fourier transform spectroscopy (Kröger et al 2010;Er et al 2011) and Doppler-limited laser spectroscopic methods (Singh & Rao 1989;Singh et al 1992;Bouzed et al 2003;Kröger 2007). In addition to the experimental investigations, a theoretical analysis of hfs of atomic Nb has been performed by , , and Kröger et al (2007).…”

Section: Introductionmentioning

confidence: 99%

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Hyperfine structure investigations of atomic niobium with optogalvanic and laser-induced fluorescence spectroscopy in the near-infrared wavelength range

Başar

Öztürk

et al. 2013

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Aims. The aim of this work is to increase the amount of hyperfine structure data of atomic niobium (Nb I), which is needed for astrophysicists for the detailed analysis of new stellar spectra. Particular emphasis was placed on the investigation of energy levels with unknown hyperfine structure constants. Methods. The hyperfine structure in the spectrum of Nb I was studied using laser-induced fluorescence spectroscopy and laser optogalvanic spectroscopy with a tuneable single-mode cw Ti:Sa laser in the wavelength range from 750 nm to 865 nm. The Nb atoms were produced and excited in a liquid-nitrogen-cooled hollow-cathode plasma. Results. We measured and analysed 81 spectral lines, 19 of which are not previously known from the literature. In total, the magnetic dipole hyperfine structure constants A were determined for 28 energy levels of even and 53 energy levels of odd parity. The electric quadrupole hyperfine structure constants B were only determined in a few cases, when the spectra were clearly resolved and/or when a level was found from several transitions. The magnetic dipole hyperfine structure constants A of 13 even and 11 odd levels as well as the electric quadrupole hyperfine structure constants B of 13 even and 17 odd levels are presented for the first time. For the other levels, improved values of hyperfine structure constants are given. Conclusions. The hyperfine structure can have a significant effect on stellar absorption line profiles, and the corresponding abundances can be substantially overestimated if these effects are not taken into account. Therefore, a detailed consideration of the hyperfine structure is important for stellar abundance determinations. The present work substantially increases the knowledge of hyperfine structure of Nb, which plays an important role in investigating the nucleosynthesis of heavy elements.

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