Wavenumber and isotropic shifts of the 3P0-3Do1 transition of titanium

Cruz, Flávio C.; Mirage, A.; Gomide, João Victor Boechat; Scalabrin, A.; Pereira, D.

doi:10.1016/0030-4018(94)90057-4

Cited by 7 publications

(8 citation statements)

References 11 publications

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“…The data we use come from laser fluorescence spectroscopy (LFS, also known simply as laser-induced fluorescence, LIF; Gangrsky et al 1995). We prefer the data of Gangrsky et al over the less accurate work of Cruz et al (1994) and previous results from the same group (Anastassov et al 1994). Isotopic separations can be estimated for many of our our chosen Ti  lines using the LFS measurements of Nouri et al (2010).…”

Section: Isotopic and Hyperfine Structurementioning

confidence: 99%

The elemental composition of the Sun

Scott

Asplund

Grevesse

et al. 2014

A&A

258

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: Isotopic and Hyperfine Structurementioning

confidence: 99%

The elemental composition of the Sun

Scott

Asplund

Grevesse

et al. 2014

A&A

258

202

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“…2. Additionally King plots of our results versus the optical IS measurements of other authors [5][6][7]14] have been constructed; the agreement is generally good, in some cases even very good. The values of the electronic factors F G and M1+1 G , obtained from King plots of individual transitions versus 1r2 AA , are listed in Table 5.…”

Section: Separation Of the Specific Mass Shift And The Field Shiftmentioning

confidence: 99%

“…However, it is only recently that some results have been published [3][4][5][6][7]. Two of the articles mentioned, by Anastassov et al [5] and Gangrsky et al [7], contain new results for the changes of nuclear mean square charge radii, extracted from the optical data.…”

Section: Introductionmentioning

confidence: 96%

Isotope shift in titanium atom

Furmann

Stefańska

Krzykowski

et al. 1996

Zeitschrift f�r Physik D Atoms, Molecules and Clusters

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“…As a frequency marker for monitoring the linearity of the laser scanning we constructed a confocal Fabry-Perot interferometer with a free-spectral-range of 75MHz [16]. The frequency differences between the hyperfine components were measured with respect to the transmission peaks of this interferometer.…”

Section: -Experimental Details~mentioning

confidence: 99%

Hyperfine structure of theR(115) 20-1 line of127I2 at 570 nm

1994

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The hyperfme spectrum of the iodine R(115) 20-1 line, at 570 nm, was obtained by conventional saturated absorption spectroscopy. The differences of nuclear etectric-quadrupole (he Qq) and spin-rotation (AC) constants between the B and X states were determined by a least-square fit to the experimental data. This line may provide a good frequency reference in coincidence with the 1So-IP 1 resonant transition of magnesium, at 285 nm, when this one is investigated with frequency doubled lasers.PACS 32.70.Jz -Line shapes, widths, and shifts. PACS 35.10.Fk -Fine-and hyperfine-structure constants.

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Wavenumber and isotropic shifts of the 3P0-3Do1 transition of titanium

Cited by 7 publications

References 11 publications

The elemental composition of the Sun

The elemental composition of the Sun

Isotope shift in titanium atom

Hyperfine structure of theR(115) 20-1 line of127I2 at 570 nm

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