Isotope shift in chromium

Furmann, B.; Jarosz, Andrzej; Stefańska, Danuta; Dembczyński, J.; Stachowska, E.

doi:10.1016/j.sab.2004.10.007

Cited by 14 publications

(6 citation statements)

References 17 publications

(30 reference statements)

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“…As a result, the nucleus of 52 Cr is very compact and stable. From spectroscopic studies, [8][9][10][11] it is confirmed that the mean-square charge radius, hr 2 i, of 52 Cr is the minimum of those of all Cr stable isotopes. Since the field shift is directly dependent on the isotopic difference in mean-square charge radius, hr 2 i, 5-7) the isotope fractionation of Cr may possibly be mass-independent due to its nuclear field shift effect.…”

Section: Introductionmentioning

confidence: 92%

Mass-Independent Isotope Fractionation in the Chemical Exchange Reaction of Chromium (III) Using a Crown Ether

Fujii

Moynier

Yin

et al. 2008

Journal of Nuclear Science and Technology

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Chromium isotopes were fractionated in a liquid-liquid extraction system using dycycrohexano-18-crown-6 at various hydrochloric acid concentrations. The isotopic ratios of 50 Cr/ 52 Cr and 53 Cr/ 52 Cr were measured precisely by the multi-collector inductively coupled plasma spectrometry (MC-ICP-MS). The isotope enrichment factor for 50 Cr-52 Cr isotope pair was shown to vary between 1:5$2:3‰ and changed as a function of acidity. The magnitudes of mass-independent isotope fractionation could be attributed to the nuclear field shift effect.

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Section: Introductionmentioning

confidence: 92%

Mass-Independent Isotope Fractionation in the Chemical Exchange Reaction of Chromium (III) Using a Crown Ether

Fujii

Moynier

Yin

et al. 2008

Journal of Nuclear Science and Technology

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“…The only data on the isotopic splitting of Cr  lines come from the recent LFS work of Furmann et al (2005) and the much older Fabry-Perot spectroscopy of Heilig & Wendlandt (1967); we use the former. HFS of 53 Cr  has been measured very accurately with ABMR by Jarosz et al (2007).…”

Section: Isotopic and Hyperfine Structurementioning

confidence: 99%

The elemental composition of the Sun

Scott

Asplund

Grevesse

et al. 2014

A&A

265

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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“…The only data on the isotopic splitting of Cr i lines come from the recent LFS work of Furmann et al (2005) and the much older Fabry-Perot spectroscopy of Heilig & Wendlandt (1967); we use the former. HFS of 53 Cr i has been measured very accurately with ABMR by Jarosz et al (2007).…”

Section: Isotopic and Hyperfine Structurementioning

confidence: 99%

The elemental composition of the Sun II. The iron group elements Sc to Ni

Scott,

Asplund,

Grevesse

et al. 2014

Preprint

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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, Grevesse, Sauval, & Scott (2009), including full line lists and details of all input data we employed.

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Isotope shift in chromium

Cited by 14 publications

References 17 publications

Mass-Independent Isotope Fractionation in the Chemical Exchange Reaction of Chromium (III) Using a Crown Ether

Mass-Independent Isotope Fractionation in the Chemical Exchange Reaction of Chromium (III) Using a Crown Ether

The elemental composition of the Sun

The elemental composition of the Sun II. The iron group elements Sc to Ni

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