A light carbon isotope composition for the Sun

Lyons, J. R.; Gharib-Nezhad, Ehsan; Ayres, Thomas R.

doi:10.1038/s41467-018-03093-3

Cited by 60 publications

(37 citation statements)

References 68 publications

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“…() would be −77‰, possibly acceptably close to Lyons et al. (). A Genesis solar wind 13 C/ 12 C measurement could distinguish between −77 and −48‰ and enable improved interpretations of lunar regolith C data.…”

Section: Future Opportunities In Genesis Sciencesupporting

confidence: 72%

“…Based on solar CO absorption lines, and using data processing models that give δ 18 O of −50 ± 11‰ (1 sigma error) in agreement with Genesis, Lyons et al. () report solar δ 13 C = −48 ± 7‰. Using a rough estimate of the solar wind C fractionation of 28‰, the inferred solar C isotopic composition from Hashizumi et al.…”

Section: Future Opportunities In Genesis Sciencementioning

confidence: 78%

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The future of Genesis science

Burnett

Jurewicz

Woolum

2019

Meteorit & Planetary Scien

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Solar abundances are important to planetary science since the prevalent model assumes that the composition of the solar photosphere is that of the solar nebula from which planetary materials formed. Thus, solar abundances are a baseline for planetary science. Previously, solar abundances have only been available through spectroscopy or by proxy (CI). The Genesis spacecraft collected and returned samples of the solar wind for laboratory analyses. Elemental and isotopic abundances in solar wind from Genesis samples have been successfully measured despite the crash of the re‐entry capsule. Here we present science rationales for a set of 12 important (and feasible postcrash) Science and Measurement Objectives as goals for the future (Table 1). We also review progress in Genesis sample analyses since the last major review (Burnett ). Considerable progress has been made toward understanding elemental fractionation during the extraction of the solar wind from the photosphere, a necessary step in determining true solar abundances from solar wind composition. The suitability of Genesis collectors for specific analyses is also assessed. Thus far, the prevalent model remains viable despite large isotopic variations in a number of volatile elements, but its validity and limitations can be further checked by several Objectives.

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Section: Future Opportunities In Genesis Sciencesupporting

confidence: 72%

Section: Future Opportunities In Genesis Sciencementioning

confidence: 78%

The future of Genesis science

Burnett

Jurewicz

Woolum

2019

Meteorit & Planetary Scien

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“…Hashizume et al (2004) argued on the basis of SIMS depth profile measurements of lunar soils that it is isotopically light relative to the Earth, with δ 13 C <-100 ‰. Recently, Lyons et al (2017) reported a spectroscopic measurement of CO in the solar photosphere, yielding δ 13 C = -48 ± 7‰. Thus, although the lunar measurement of Hashizume et al (2004) does not rule out as extreme a 13 C depletion in the Sun as observed in A7_60, the astronomical measurement argues against it.…”

Section: Organic Mattermentioning

confidence: 99%

High abundances of presolar grains and 15N-rich organic matter in CO3.0 chondrite Dominion Range 08006

Nittler

Alexander

Davidson

et al. 2018

Geochimica et Cosmochimica Acta

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NanoSIMS C-, N-, and O-isotopic mapping of matrix in CO3.0 chondrite Dominion Range (DOM) 08006 revealed it to have in its matrix the highest abundance of presolar O-rich grains (257 +76/-96 ppm, 2σ) of any meteorite. It also has a matrix abundance of presolar SiC of 35 (+25/-17, 2σ) ppm, similar to that seen across primitive chondrite classes. This provides additional support to bulk isotopic and petrologic evidence that DOM 08006 is the most primitive known CO meteorite. Transmission electron microscopy of five presolar silicate grains revealed one to have a composite mineralogy similar to larger amoeboid olivine aggregates and consistent with equilibrium condensation, two non-stoichiometric amorphous grains and two olivine grains, though one is identified as such solely based on its composition. We also found insoluble organic matter (IOM) to be present primarily as sub-micron inclusions with ranges of C- and N-isotopic anomalies similar to those seen in primitive CR chondrites and interplanetary dust particles. In contrast to other primitive extraterrestrial materials, H isotopic imaging showed normal and homogeneous D/H. Most likely, DOM 08006 and other CO chondrites accreted a similar complement of primitive and isotopically anomalous organic matter to that found in other chondrite classes and IDPs, but the very limited amount of thermal metamorphism experienced by DOM 08006 has caused loss of D-rich organic moieties, while not substantially affecting either the molecular carriers of C and N anomalies or most inorganic phases in the meteorite. One C-rich grain that was highly depleted in C andN was identified; we propose it originated in the Sun's parental molecular cloud.

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“…The results reported by Fujiya et al 1 therefore raise many questions about the origin of isotopic variations, such as the role of photochemical processes in producing 13 Cenrichments 17 , and the general structure of the protoplanetary disk. Future comparison of the present data with samples of hydrated B-and C-type asteroids expected to be returned to Earth by the OSIRIS-REx and Hayabusa 2 missions will thus be fundamental to further quantifying large-scale pertubations in the early Solar Sytem.…”

Section: Yves Marrocchi and Laurette Pianimentioning

confidence: 98%