Hyperfine Structure Investigations of Mn I. Part I: Experimental and Theoretical Studies of the Hyperfine Structure in the Even Configurations

Başar, Günay; Başar, Gönül; Acar, Gülay; Öztürk, I. K.; Kröger, S.

doi:10.1238/physica.regular.067a00476

Cited by 20 publications

(15 citation statements)

References 30 publications

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“…The best original data come from the extremely accurate spin-exchange results of Davis et al (1971), the ABMR of Johann et al (1981), ABMR by Dembczyński et al (1979), interference spectroscopy by Brodzinski et al (1987) and laser-atomic-beam spectroscopy by Kronfeldt et al (1985). The second and third tiers consist of FTS and OGS data obtained by Blackwell-Whitehead et al (2005a) and Başar et al (2003) respectively. We do not use the B values of Başar et al for the odd levels however, because in our opinion their accuracy is insufficient to clearly distinguish them from zero.…”

Section: Hyperfine Structurementioning

confidence: 99%

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: Hyperfine Structurementioning

confidence: 99%

The elemental composition of the Sun

Scott

Asplund

Grevesse

et al. 2014

A&A

269

202

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“…The inset shows a schematic depiction of the hyperfine structure of an I = 1 state along with the allowed hyperfine transitions. The frequency is shown relative to the 6 S 5/2 → 6 P 3/2 literature centroid of 55 Mn [23].…”

Section: Fig 2 (Color Online)mentioning

confidence: 99%

Spins and magnetic moments ofMn58,60,62,64ground states and isomers

et al. 2015

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The odd-odd 54,56,58,60,62,64 Mn isotopes (Z = 25) were studied using bunched-beam collinear laser spectroscopy at ISOLDE, CERN. From the measured hyperfine spectra the spins and magnetic moments of Mn isotopes up to N = 39 were extracted. The previous tentative ground state spin assignments of 58,60,62,64 Mn are now firmly determined to be I = 1 along with an I = 4 assignment for the isomeric states in 58,60,62 Mn. The I = 1 magnetic moments show a decreasing trend with increasing neutron number while the I = 4 moments remain quite constant between N = 33 and N = 37. The results are compared to large-scale shell-model calculations using the GXPF1A and LNPS effective interactions. The excellent agreement of the ground state moments with the predictions from the LNPS calculations illustrates the need for an increasing amount of proton excitations across Z = 28 and neutron excitations across N = 40 in the ground state wave functions from N = 37 onwards.

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“…; (6) Johann et al (1981); (7) Luc & Gerstenkorn (1972); (8) Lefèbvre et al (2003); (9) Başar et al (2003).…”

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confidence: 99%

Formation of Mn I lines in the solar atmosphere

Bergemann¹,

Gehren²

2007

A&A

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Context. We present a detailed NLTE analysis of 39 Mn i lines in the solar spectrum. The influence of NLTE effects on the line formation and element abundance is investigated. Aims. Our goal is the derivation of solar log g f ε values for manganese lines, which will later be used in differential abundance analyses of metal-poor stars. Methods. The method of spectrum synthesis is employed, which is based on a solar model atmosphere with initially specified element abundances. A manganese abundance of log ε Mn, = 5.47 dex is used with the theoretical line-blanketed model atmosphere. Statistical equilibrium calculations are carried out for the model atom, which comprises 245 and 213 levels for Mn i and Mn ii, respectively.Photoionization cross-sections are assumed hydrogenic. Results. For line synthesis van der Waals broadening is calculated according to Anstee & O'Mara's formalism. It is shown that hyperfine structure of the Mn lines also has strong broadening effects, and that manganese is prone to NLTE effects in the solar atmosphere. The nature of the NLTE effects and the validity of the LTE approach are discussed in detail. The role of photoionization and collisional interaction is investigated. Conclusions. Maximum NLTE corrections of +0.1 dex with respect to LTE profiles are found. We propose an absolute solar abundance of 5.36 ± 0.1 dex. The main source of errors in the abundance calculations is uncertain oscillator strengths.

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Hyperfine Structure Investigations of Mn I. Part I: Experimental and Theoretical Studies of the Hyperfine Structure in the Even Configurations

Cited by 20 publications

References 30 publications

The elemental composition of the Sun

The elemental composition of the Sun

Spins and magnetic moments ofMn58,60,62,64ground states and isomers

Formation of Mn I lines in the solar atmosphere

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