Hyperfinestructure-investigations in the mangan I configurations 3d
5 4s 4p and 4s 5s

Brodzinski, T.; Kronfeldt, H.-D.; Kropp, J.‐R.; Winkler, R.

doi:10.1007/bf01384582

Cited by 25 publications

(24 citation statements)

References 11 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.…”

Section: Hyperfine Structurementioning

confidence: 99%

The elemental composition of the Sun

Scott

Asplund

Grevesse

et al. 2014

A&A

264

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

264

202

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“…The nuclear spin (I = 2.5) of the only nuclide that contributes for the manganese abundance ( 55 Mn) was found in Woodgate & Martin (1957). For the Mn i 6013/6016/6021 and 5394 lines, experimental data on hyperfine coupling constants, namely the magnetic dipole A-factor, and the electric quadrupole B-factor, were adopted from Handrich et al (1969), Biehl (1976, and Brodzinski et al (1987) (transformed from MKaysers(cm −1 ) to MHz), and are given in Table 1. The hfs components for the Mn i lines and corresponding oscillator strengths are reported in Table 3.…”

Section: Observationsmentioning

confidence: 99%

Manganese abundances in Galactic bulge red giants

Barbuy

Hill

Zoccali

et al. 2013

A&A

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Context. Manganese is mainly produced in type II SNe during explosive silicon burning, in incomplete Si-burning regions, and depends on several nucleosynthesis environment conditions, such as mass cut between the matter ejected and falling back onto the remnant, electron and neutron excesses, mixing fallback, and explosion energy. Manganese is also produced in type Ia SNe. Aims. The aim of this work is the study of abundances of the iron-peak element Mn in 56 bulge giants, among which 13 are red clump stars. Four bulge fields along the minor axis are inspected. The study of abundances of Mn-over-Fe as a function of metallicity in the Galactic bulge may shed light on its production mechanisms. Methods. High-resolution spectra were obtained using the FLAMES+UVES spectrograph on the Very Large Telescope. The spectra were obtained within a program to observe 800 stars using the GIRAFFE spectrograph, together with the present UVES spectra. [O/H] has a behaviour running parallel, at higher metallicities, compared to thick disc stars, indicating that the bulge enrichment might have proceeded differently from that of the thick disc.

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“…The h f s constants for Mn i were taken from Brodzinski et al (1987) and Walther (1962). The nuclear spin (I = 2.5) of the only nuclide that contributes to the manganese abundance ( 55 Mn) was found in Woodgate & Martin (1957).…”

Section: Iron-peak Elementsmentioning

confidence: 99%

Mn, Cu, and Zn abundances in barium stars and their correlations with neutron capture elements

Allen

Mello

2010

A&A

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Barium stars are optimal sites for studying the correlations between the neutron-capture elements and other species that may be depleted or enhanced, because they act as neutron seeds or poisons during the operation of the s-process. These data are necessary to help constrain the modeling of the neutron-capture paths and explain the s-process abundance curve of the solar system. Chemical abundances for a large number of barium stars with different degrees of s-process excesses, masses, metallicities, and evolutionary states are a crucial step towards this goal. We present abundances of Mn, Cu, Zn, and various light and heavy elements for a sample of barium and normal giant stars, and present correlations between abundances contributed to different degrees by the weak-s, mains, and r-processes of neutron capture, between Fe-peak elements and heavy elements. Data from the literature are also considered in order to better study the abundance pattern of peculiar stars. The stellar spectra were observed with FEROS/ESO. The stellar atmospheric parameters of the eight barium giant stars and six normal giants that we analyzed lie in the range 4300 < T eff /K < 5300, −0.7 < [Fe/H] ≤ 0.12 and 1.5 ≤ log g < 2.9. Carbon and nitrogen abundances were derived by spectral synthesis of the molecular bands of C 2 , CH, and CN. For all other elements we used the atomic lines to perform the spectral synthesis. A very large scatter was found mainly for the Mn abundances when data from the literature were considered. We found that [Zn/Fe] correlates well with the heavy element excesses, its abundance clearly increasing as the heavy element excesses increase, a trend not shown by the [Cu/Fe] and [Mn/Fe] ratios. Also, the ratios involving Mn, Cu, and Zn and heavy elements usually show an increasing trend toward higher metallicities. Our results suggest that a larger fraction of the Zn synthesis than of Cu is owed to massive stars, and that the contribution of the main-s process to the synthesis of both elements is small. We also conclude that Mn is mostly synthesized by SN Ia, and that a non-negligible fraction of the synthesis of Mn, Cu, and Zn is owed to the weak s-process.

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Hyperfinestructure-investigations in the mangan I configurations 3d 5 4s 4p and 4s 5s

Cited by 25 publications

References 11 publications

The elemental composition of the Sun

The elemental composition of the Sun

Manganese abundances in Galactic bulge red giants

Mn, Cu, and Zn abundances in barium stars and their correlations with neutron capture elements

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