Volatile element chemistry during accretion of the earth

Fegley, B.; Lodders, K.; Jacobson, Nathan

doi:10.1016/j.chemer.2019.125594

Cited by 29 publications

(29 citation statements)

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“…In addition to the implications the NC-CC dichotomy has on protoplanetary disk evolution models, the isotope dichotomy is starting to be used to decipher the source(s) of Earth's water and other volatiles such as C and N. For example, accretion of volatile-rich CC material towards the end of Earth's formationthrough the Moon-forming impactor and/or late accretion -has been argued for based on a comparison of the Mo-Ru isotope composition of meteorites and the bulk silicate Earth (Budde et al 2019;Hopp et al 2020). This seems consistent with the constraints provided by elemental com-positions, which require Earth to have accreted from at least two components, initially a reduced one, which now would be sampled by NC meteorites, and later a more oxidized and volatile-rich component, represented by CC meteorites (e.g., Rubie et al 2015; for a recent review, see Fegley et al 2020).…”

Section: Does the Nc-cc Dichotomy Extend To Major Highly-volatile Elements?supporting

confidence: 68%

“…These data require that Earth formed from a reservoir that is isotopically similar to enstatite chondrites (or a mixture of bodies that bracket the isotopic composition of Earth) (e.g., Clayton et al 1984;Lodders 2000;Dauphas 2017). Earth cannot have been constructed solely out of enstatite chondrites because of the resolvable chemical (including oxidation state) and mass-dependent isotopic differences between enstatite chondrites and Earth (e.g., McDonough and Sun 1995;Lodders 2000;Drake and Righter 2002;Fegley et al 2020). Dauphas (2017) proposed that enstatite meteorites and Earth formed from the same isotopic nebular reservoir, and the reason that the bodies differ in bulk chemical compositions is because their chemical evolution diverged due to fractionation via nebular and planetary processes.…”

Section: Implications For Volatile Accretion: Building Earth From Nc-and Cc-type Precursorsmentioning

confidence: 99%

“…Determining the role that NC-and CC-type bodies (and chondrites vs. achondrites) played in the accretionary history of Earth can become complicated when the isotopic and chemical characteristics of an object might be decoupled. Given the absence of meteoritic materials that match Earth's elemental and isotopic compositions, it is likely that Earth was primarily constructed out of building blocks that shared feeding zones with enstatite chondrites, but these materials are not sampled by the current meteorite collection (e.g., Drake and Righter 2002;Dauphas 2017; for a recent review, see Fegley et al 2020).…”

Section: Implications For Volatile Accretion: Building Earth From Nc-and Cc-type Precursorsmentioning

confidence: 99%

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The NC-CC Isotope Dichotomy: Implications for the Chemical and Isotopic Evolution of the Early Solar System

et al. 2020

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Understanding the formation of our planetary system requires identification of the materials from which it originated and the accretion processes that produced the planets. The compositional evolution of the solar system can be constrained by synthesizing astronomical datasets and numerical models with elemental and isotopic compositions from objects that directly sampled the disk: meteorites and their constituents (chondrules, refractory inclusions, and matrix). This contribution reviews constraints on early solar system evolution provided by the so-called non-carbonaceous (NC) and carbonaceous chondrite (CC) groups and their relationship to the volatile element characteristics of chondritic meteorites. In previous work, the NC or CC character of a parent body was used to infer its accretion location in the protoplanetary disk. The NC groups purportedly originated in the inner disk, and the CC groups were derived from the outer disk, where the NC and CC regions of the disk may have been separated early on by proto-Jupiter, a pressure maximum, or a dust trap in the disk. The tenet that all CC parent bodies accreted in the outer disk is, in part, based on evidence that a handful of CC meteorites are enriched in volatile species compared to NC meteorites. Here, it is reviewed if and how the volatile element and nucleosynthetic isotope compositions of meteorites can be linked to accretion locations within the disk. The nucleosynthetic isotope compositions of whole rock meteorite samples contrast the trends found for their major volatile element compositions (i.e., C, N, and O). Although there may be an increase in volatile abundances when comparing some stony NC and CC meteorites and their inferred accretion locations within the disk, this is not necessarily a general rule. The difficulties with inferring parent body accretion locations are discussed. It is found that it cannot always be assumed that parent bodies which formed in the CC reservoir are "volatile-rich" relative to those that formed in the NC reservoir which are "volatilepoor". Consequently, tracing the origin of terrestrial volatiles using the NC-CC isotope dichotomy remains challenging.

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Section: Does the Nc-cc Dichotomy Extend To Major Highly-volatile Elements?supporting

confidence: 68%

Section: Implications For Volatile Accretion: Building Earth From Nc-and Cc-type Precursorsmentioning

confidence: 99%

Section: Implications For Volatile Accretion: Building Earth From Nc-and Cc-type Precursorsmentioning

confidence: 99%

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The NC-CC Isotope Dichotomy: Implications for the Chemical and Isotopic Evolution of the Early Solar System

et al. 2020

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“…Long-lived magma ocean states may be directly observable with near-future astronomical instrumentation (Lupu et al, 2014;Hamano et al, 2015;Bonati et al, 2019) and link the presentday climates of extrasolar rocky planets with the ancient climate of Hadean Earth. This would allow crucial insights on the thermal and compositional state of young exoplanets and further help constrain the chronology of terrestrial planets in the Solar System (Fegley Jr. et al, 2020).…”

Section: Accepted Articlementioning

confidence: 99%

“…Long‐lived magma ocean states may be directly observable with near‐future astronomical instrumentation (Bonati et al., 2019; Hamano et al., 2015; Lupu et al., 2014) and link the present‐day climates of extrasolar rocky planets with the ancient climate of Hadean Earth. This would allow crucial insights on the thermal and compositional state of young exoplanets and further help constrain the chronology of terrestrial planets in the Solar System (Fegley et al., 2020). Connecting the thermo‐compositional chronology and histories of exoplanets with observations (Schaefer et al., 2016; Wordsworth et al., 2018) is an essential step to bridge astronomy and planetary science.…”

Section: Introductionmentioning

confidence: 99%

Vertically Resolved Magma Ocean–Protoatmosphere Evolution: H₂, H₂O, CO₂, CH₄, CO, O₂, and N₂as Primary Absorbers

et al. 2021

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Magma oceans with different volatiles display varying timescales of solidification, out-11 gassing, and atmospheric stratification 12 • Atmospheric blanketing and cooling time increase in three principle classes from N 2 , CO, 13 O 2 to H 2 O, CO 2 , CH 4 to H 2 14 • Coupled mantle-atmosphere systems display distinctive features that link the interior and 15 surface state to atmospheric spectrum and climate 16

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The sulfur species in hot rocky exoplanet atmospheres

Janssen,

Woitke,

Herbort

et al. 2023

Astron Nachr

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The first JWST observations of hot Jupiters showed an unexpected detection of SO in their hydrogen‐rich atmospheres. We investigate how much sulfur can be expected in the atmospheres of rocky exoplanets and which sulfur molecules can be expected to be most abundant and detectable by transmission spectroscopy. We run thermochemical equilibrium models at the crust–atmosphere interface, considering surface temperatures 500–5000 K, surface pressures 1–100 bar, and various sets of element abundances based on common rock compositions. Between 1000 and 2000 K, we find gaseous sulfur concentrations of up to 25% above the rock in our models. SO, SO, HS, and S are by far the most abundant sulfur molecules. SO shows potentially detectable features in transmission spectra at about 4 m, between 7 and 8 m, and beyond 15 m. In contrast, the sometimes abundant HS molecule is difficult to detect in these spectra, which are mostly dominated by HO and CO. Although the molecule PS only occurs with concentrations ppm, it can cause a strong absorption feature between 0.3 and 0.65 m in some of our models for high surface pressures. The detection of sulfur molecules would enable a better characterization of the planetary surface.

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Volatile element chemistry during accretion of the earth

Cited by 29 publications

References 528 publications

The NC-CC Isotope Dichotomy: Implications for the Chemical and Isotopic Evolution of the Early Solar System

The NC-CC Isotope Dichotomy: Implications for the Chemical and Isotopic Evolution of the Early Solar System

Vertically Resolved Magma Ocean–Protoatmosphere Evolution: H₂, H₂O, CO₂, CH₄, CO, O₂, and N₂as Primary Absorbers

The sulfur species in hot rocky exoplanet atmospheres

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Volatile element chemistry during accretion of the earth

Cited by 29 publications

References 528 publications

The NC-CC Isotope Dichotomy: Implications for the Chemical and Isotopic Evolution of the Early Solar System

The NC-CC Isotope Dichotomy: Implications for the Chemical and Isotopic Evolution of the Early Solar System

Vertically Resolved Magma Ocean–Protoatmosphere Evolution: H2, H2O, CO2, CH4, CO, O2, and N2as Primary Absorbers

The sulfur species in hot rocky exoplanet atmospheres

Contact Info

Product

Resources

About

Vertically Resolved Magma Ocean–Protoatmosphere Evolution: H₂, H₂O, CO₂, CH₄, CO, O₂, and N₂as Primary Absorbers