Erratum: “Inward Radial Mixing of Interstellar Water Ices in the Solar Protoplanetary Disk” (2016, ApJL, 827, L1)

Vacher, Lionel G.; Marrocchi, Yves; Verdier-Paoletti, M. J.; Villeneuve, Johan; Gounelle, M.

doi:10.3847/2041-8213/836/1/l16

Cited by 5 publications

(4 citation statements)

References 2 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The procedure was similar to that detailed in Vacher et al (2020). After crushing in an agate mortar, two aliquots (3.36 and 4.29 mg, respectively) were loaded into tin capsules, which were degassed for 48 hours at 120°C for removing adsorbed atmospheric water before hydrogen measurements (Vacher et al, 2016Piani et al, 2020).…”

Section: Bulk Hydrogen Carbon and Nitrogen Isotope Measurementsmentioning

confidence: 99%

See 1 more Smart Citation

The Tarda Meteorite: A Window into the Formation of D-type Asteroids

Marrocchi

Avice

Barrat

2021

ApJL

Self Cite

View full text Add to dashboard Cite

Dynamic models of solar system evolution suggest that D-type asteroids formed beyond Saturn's orbit and represent invaluable witnesses of the prevailing conditions in the outer solar system. Here, we report a comprehensive petrographic and isotopic characterization of the carbonaceous chondrite Tarda, a recent fall recovered in the Moroccan Sahara. We show that Tarda shares strong similarities with the D-type-derived chondrite Tagish Lake, implying that Tarda represents a rare sample of D-type asteroids. Both Tarda and Tagish Lake are characterized by the presence of rare 16 O-rich chondrules and chondrule fragments, high C/H ratios, and enrichments in deuterium, 15 N, and 13 C. By combining our results with literature data on carbonaceous chondrites related to C-type asteroids, we show that the outer solar system at that time was characterized by large-scale oxygen isotopic homogeneities in (i) the water-ice grains accreted by asteroids and (ii) the gas controlling the formation of FeO-poor chondrules. Conversely, the zone in which D-type asteroids accreted was significantly enriched in deuterium relative to the formation regions of C-type asteroids, features likely inherited from unprocessed, D-rich, molecular-cloud materials.

show abstract

Section: Bulk Hydrogen Carbon and Nitrogen Isotope Measurementsmentioning

confidence: 99%

“…Fig. 3:Comparison of the bulk D/H (as D) vs. C/H ratios of Tarda and Tagish Lake, as well as those of CM and CI chondrites (data measured after pre-degassing of the samples;Vacher et al, 2016Vacher et al, , 2020.…”

mentioning

confidence: 99%

The Tarda Meteorite: A Window into the Formation of D-type Asteroids

Marrocchi

Avice

Barrat

2021

ApJL

Self Cite

View full text Add to dashboard Cite

show abstract

“…The Paris meteorite exhibits enrichment in its bulk δD compared to the mean value of CM chondrites (120 ± 1‰ versus −69 ± 19‰, respectively; Vacher et al. , ). In addition, the oxygen isotope signatures in carbonates of the Paris meteorite require the mixing of 8–35% of outer disk water with the CM local fluid from which some of the 17,18 O‐rich Ca‐carbonates precipitated (Vacher et al.…”

Section: Introductionmentioning

confidence: 97%

Primordial heavy noble gases in the pristine Paris carbonaceous chondrite

Bekaert

Marrocchi

Meshik

et al. 2018

Meteorit & Planetary Scien

Self Cite

View full text Add to dashboard Cite

The Paris carbonaceous chondrite represents the most pristine carbonaceous chondrite, providing a unique opportunity to investigate the composition of early solar system materials prior to the onset of significant aqueous alteration. A dual origin (namely from the inner and outer solar system) has been demonstrated for water in the Paris meteorite parent body (Piani et al. 2018 ). Here, we aim to evaluate the contribution of outer solar system (cometary‐like) water ice to the inner solar system water ice using Xe isotopes. We report Ar, Kr, and high‐precision Xe isotopic measurements within bulk CM 2.9 and CM 2.7 fragments, as well as Ne, Ar, Kr, and Xe isotope compositions of the insoluble organic matter ( IOM ). Noble gas signatures are similar to chondritic phase Q with no evidence for a cometary‐like Xe component. Small excesses in the heavy Xe isotopes relative to phase Q within bulk samples are attributed to contributions from presolar materials. CM 2.7 fragments have lower Ar/Xe relative to more pristine CM 2.9 fragments, with no systematic difference in Xe contents. We conclude that Kr and Xe were little affected by aqueous alteration, in agreement with (1) minor degrees of alteration and (2) no significant differences in the chemical signature of organic matter in CM 2.7 and CM 2.9 areas (Vinogradoff et al. 2017 ). Xenon contents in the IOM are larger than previously published data of Xe in chondritic IOM , in line with the Xe component in Paris being pristine and preserved from Xe loss during aqueous alteration/thermal metamorphism.

show abstract

“…Largely present on Earth, they have also been detected at the surface of other solid bodies of the solar system from planets like Mars (e.g., Bandfield et al 2003;Ehlmann et al 2008;Morris et al 2010;Horgan et al 2020) to asteroids such as Bennu (Kaplan et al 2020) and Ryugu (Nakamura et al 2022;Pilorget et al 2022), via dwarf-planet Ceres (De Sanctis et al 2016;Raponi et al 2019). Accordingly, they have been found in hydrated interplanetary dust particles (e.g., Sandford 1986;Tomeoka & Buseck 1986;Bradley et al 1989;Germani et al 1990;Bradley et al 1992) and in meteorites (Mittlefehldt 1994;Scott et al 1998;Lee et al 2013;Alexander et al 2015;Vacher et al 2016Vacher et al , 2017Piani et al 2018;Ohtaki et al 2021), which are all fragments of the larger solid bodies. All these carbonates are geological materials and their formation proceeds by aqueous alteration of silicates.…”

Section: Introductionmentioning

confidence: 99%

Gas-phase Condensation of Carbonated Silicate Grains

Rouillé,

Schmitt,

Jäger

et al. 2024

ApJ

View full text Add to dashboard Cite

Reports on the detection of carbonates in planetary nebulae (PNe) and protostars have suggested the existence of a mechanism that produces these compounds in stellar winds and outflows. A subsequent laboratory study has reported a possible mechanism by presenting the non-thermodynamic-equilibrium (TE), gas-phase condensation of amorphous silicate grains with amorphous calcium carbonate inclusions. The authors concluded that water vapor was necessary for the formation of the carbonates. We present a laboratory study with pulsed laser ablation of a MgSi target in O2 and CO2 gases and report, in the absence of water vapor, the non-TE, gas-phase condensation of amorphous carbonated magnesium silicate dust. It consists of amorphous silicate grains with the formula MgSiO3, which comprise carbonate groups homogeneously dispersed in their structure. The IR spectra of the grains show the characteristic bands of amorphous silicates and two bands at ∼6.3 and ∼7.0 μm, which we assign to the carbonate groups. The silicate bands are not significantly affected at an estimated Si:C ratio of 9:1–9:2. Such grains could form in winds and outflows of evolved stars and PNe if C atoms are present during silicate condensation. Additionally, we find that Lyα radiation dissociates the carbonate groups at the surface of the carbonated silicate grains and we estimate the corresponding photodissociation cross section of (0.04 ± 0.02) ×10−16 cm2. Therefore, photodissociation would limit the formation of carbonate groups on grains in winds and outflows of stars emitting vacuum ultraviolet photons, and the carbonates observed in protostars have not formed by gas-phase condensation.

show abstract

Erratum: “Inward Radial Mixing of Interstellar Water Ices in the Solar Protoplanetary Disk” (2016, ApJL, 827, L1)

Cited by 5 publications

References 2 publications

The Tarda Meteorite: A Window into the Formation of D-type Asteroids

The Tarda Meteorite: A Window into the Formation of D-type Asteroids

Primordial heavy noble gases in the pristine Paris carbonaceous chondrite

Gas-phase Condensation of Carbonated Silicate Grains

Contact Info

Product

Resources

About