A search for the solar Sr 87 content and the solar Rb/Sr ratio

Hauge, Ö.

doi:10.1007/bf00165268

Cited by 21 publications

(9 citation statements)

References 7 publications

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“…The line at 7070 A Ê though also very weak appears as a relatively clean line when the disc centre spectrum of Brault & Testermann (1972) is scaled up by a factor of 60. Hauge (1972) has shown that the theoretical log gf value for this line obtained by Gruzdev (1967) is midway between two empirical values, suggesting an uncertainty of^0X03. A section of spectrum containing this line is shown in Fig.…”

Section: Sr I Linesmentioning

confidence: 75%

Broadening of lines of Be II, Sr II and Ba II by collisions with hydrogen atoms and the solar abundance of strontium

Barklem¹,

O'Mara

2000

Monthly Notices of the Royal Astronomical Society

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In a previous paper by the present authors the theory of Anstee and O’Mara for the broadening of spectral lines of neutral atoms by collisions with hydrogen atoms was extended to singly ionized atoms. In this paper we apply the method to the resonance and triplet lines of ionized strontium, the infrared triplet of ionized barium, and the resonance lines of ionized beryllium. Analysis of five lines of ionized strontium, previously regarded as too strong for an abundance analysis, and two lines of neutral strontium results in a solar abundance of strontium of log(NSrNH)+12=2.92±0.05, which is entirely consistent with the meteoritic value.

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Section: Sr I Linesmentioning

confidence: 75%

Broadening of lines of Be II, Sr II and Ba II by collisions with hydrogen atoms and the solar abundance of strontium

Barklem¹,

O'Mara

2000

Monthly Notices of the Royal Astronomical Society

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“…We treat each Sr line as a single component in our abundance calculations, as isotopic splitting is small for Sr lines (Hauge 1972b) …”

Section: Strontiummentioning

confidence: 99%

The elemental composition of the Sun

Grevesse

Scott

Asplund

et al. 2014

A&A

213

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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“…Some 7% of all the 87 Rb produced to that time would thus already have decayed to 87 Sr, accounting for some 10% of the solar inventory of 87 Sr. This contribution might have been lower if the mean age of 87 Rb were lower than that assumed, or higher if the ISM value of Rb/Sr were higher (e.g., Hauge 1972). In addition, approximately 6% of solar 86 Sr, but a substantially smaller fraction of 87 Sr, was contributed by the p-process rather than the s-process (Käppeler et al 1990).…”

Section: Discussionmentioning

confidence: 89%

s‐Process Sr Isotopic Compositions in Presolar SiC from the Murchison Meteorite

Podosek

Prombo

Amari

et al. 2004

ApJ

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We have used thermal ionization mass spectrometry to measure the isotopic compositions of Sr in size-sorted samples (the KJ series) of interstellar SiC separated from the Murchison meteorite. The Sr compositions are radically anomalous in comparison to those in normal solar system materials. As for other heavy elements in presolar SiC, the anomalies can be understood to represent enrichment of s-process (slow neutron capture) nucleosynthetic products, plausibly occurring in asymptotic giant branch stars. The inferred s-process 88 Sr/ 86 Sr ratios are variable and correlate with grain size: this ratio decreases (suggesting lower effective neutron exposure) with increasing grain size. The sense of this trend is the same as that previously observed in Ba, but opposite to that previously observed in Kr, in the same samples. The Sr and Ba trends indicate covariation of the factors governing neutron exposure and grain growth kinetics in a manner not yet understood. The contrasting trend for Kr suggests that the mechanisms for the introduction of volatile (Kr) and refractory (Sr and Ba) elements into SiC produce a biased sampling of the population of different nucleosynthetic products. The relative abundances of s-process 86 Sr, 87 Sr, and 88 Sr in Murchison SiC are very close to those for early solar system Sr, but in view of the different s-process superpositions and other contributions to all three of these isotopes, the close agreement must be regarded as coincidental.

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A search for the solar Sr 87 content and the solar Rb/Sr ratio

Cited by 21 publications

References 7 publications

Broadening of lines of Be II, Sr II and Ba II by collisions with hydrogen atoms and the solar abundance of strontium

Broadening of lines of Be II, Sr II and Ba II by collisions with hydrogen atoms and the solar abundance of strontium

The elemental composition of the Sun

s‐Process Sr Isotopic Compositions in Presolar SiC from the Murchison Meteorite

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