Determination of the oscillator strengths of Sn(I) in the ultraviolet (2400–4000 Å)

Lotrian, J; Cariou, J; Johannin-Gilles, A.

doi:10.1016/0022-4073(76)90012-1

Cited by 17 publications

(15 citation statements)

References 12 publications

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“…We adopt the g f -value obtained by Lotrian et al (1976) for this line, from lifetime and branching fraction measurements. The equivalent width of this very faint line (0.12 pm) has an uncertainty of order 20%, i.e.…”

Section: Tinmentioning

confidence: 99%

The elemental composition of the Sun

Grevesse

Scott

Asplund

et al. 2014

A&A

211

252

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We re-evaluate the abundances of the elements in the Sun from copper (Z = 29) to thorium (Z = 90). Our results are mostly based on neutral and singly-ionised lines in the solar spectrum. We use the latest 3D hydrodynamic solar model atmosphere, and in a few cases also correct for departures from local thermodynamic equilibrium (LTE) using non-LTE (NLTE) calculations performed in 1D. In order to minimise statistical and systematic uncertainties, we make stringent line selections, employ the highest-quality observational data and carefully assess oscillator strengths, hyperfine constants and isotopic separations available in the literature, for every line included in our analysis. Our results are typically in good agreement with the abundances in the most pristine meteorites, but there are some interesting exceptions. This analysis constitutes both a full exposition and a slight update of the relevant parts 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 that we have employed.

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Section: Tinmentioning

confidence: 99%

The elemental composition of the Sun

Grevesse

Scott

Asplund

et al. 2014

A&A

211

252

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“…Table 3 presents the branching fractions, computed from equations ( 13)-(25), by the reduction of the measured transition probabilities of Corliss and Bozman [4], and from other published experimental studies [6][7][8][9]. In Si I the agreement between the IC semiempirical values and the high-precision measurements of Smith et al [6] is quite striking, and gives additional credence to the single-configuration model for this system.…”

Section: Levelmentioning

confidence: 55%

“…SE denotes semiempirical estimates from this work, and CB denotes the measurements of [4]. Other measurements are from [3] for Si I, [7] for Ge I, [8] for Sn I and [9] between the semiempirical and measured values for Pb I, but it has been shown [14] that this occurs because of unusually large differences between the two relativistic radial transition integrals caused by fortuitous cancellation effects, and not because of any breakdown in the single-configuration approximation. The results of [4] generally agree quite well with both the semiempirical estimates and with subsequent experimental measurements.…”

Section: Levelmentioning

confidence: 97%

“…If there is no significant branching to other configurations the branching fractions can be specified from angular factors and the intermediate coupling (IC) mixing amplitudes, which can be determined from spectroscopic energy level data. The ns 2 np 2 -ns 2 np(n + 1)s manifold of transitions in Si I, Ge I, Sn I and Pb I provide such a case, and comprehensive measurements for this supermultiplet are contained both in the tabulation of Corliss and Bozman [4], and in more recent studies [6][7][8][9]. While the lack of configuration interaction (CI) in these systems simplifies the calculational specification of the branching fractions, the transitions cover a wide range of both wavelength regions and intensity ratios, and are no less challenging to experimental measurement than any other system studied in [4].…”

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confidence: 99%

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Use of intermediate coupling relationships to test measured branching fraction data

Curtis¹

1998

J. Phys. B: At. Mol. Opt. Phys.

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The extensive arc emission measurements of transition probabilities by Corliss and Bozman are known to contain errors due to flaws in the determination of level populations in the source. However, if no similar errors were present in the photometric calibration, then branching fractions from the same upper level deduced from these measurements should be valid. It is shown that the branching fractions for the ns 2 np 2 -ns 2 np(n + 1)s transitions in Si I, Ge I, Sn I and Pb I can be accurately estimated using intermediate coupling amplitudes obtained from spectroscopic data, and thus provide a test of the validity of these measurements. The results of Corliss and Bozman are examined in the context of comparisons with these estimated values and with other measurements, and it is demonstrated that branching fractions from the same upper level obtained from these data can be quite reliable.

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“…The only reasonable Sn line available is a very weak Sn i line in the near-UV (see Table 1). We adopt the g f -value obtained by Lotrian et al (1976) for this line, from lifetime and branching fraction measurements. The equivalent width of this very faint line (0.12 pm) has an uncertainty of order 20%, i.e.…”

Section: Tinmentioning

confidence: 99%

The elemental composition of the Sun III. The heavy elements Cu to Th

Grevesse,

Scott,

Asplund

et al. 2014

Preprint

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We re-evaluate the abundances of the elements in the Sun from copper (Z = 29) to thorium (Z = 90). Our results are mostly based on neutral and singly-ionised lines in the solar spectrum. We use the latest 3D hydrodynamic solar model atmosphere, and in a few cases also correct for departures from local thermodynamic equilibrium (LTE) using non-LTE (NLTE) calculations performed in 1D. In order to minimise statistical and systematic uncertainties, we make stringent line selections, employ the highest-quality observational data and carefully assess oscillator strengths, hyperfine constants and isotopic separations available in the literature, for every line included in our analysis. Our results are typically in good agreement with the abundances in the most pristine meteorites, but there are some interesting exceptions. This analysis constitutes both a full exposition and a slight update of the relevant parts of the preliminary results we presented in Asplund, Grevesse, Sauval & Scott (2009), including full line lists and details of all input data that we have employed.

show abstract

Determination of the oscillator strengths of Sn(I) in the ultraviolet (2400–4000 Å)

Cited by 17 publications

References 12 publications

The elemental composition of the Sun

The elemental composition of the Sun

Use of intermediate coupling relationships to test measured branching fraction data

The elemental composition of the Sun III. The heavy elements Cu to Th

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