Presolar diamond, silicon carbide, and graphite in carbonaceous chondrites: implications for thermal processing in the solar nebula

Huss, G. R.; Meshik, A. P.; Smith, J. B.; Hohenberg, C. M.

doi:10.1016/j.gca.2003.07.019

Cited by 185 publications

(248 citation statements)

References 62 publications

(170 reference statements)

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“…An extensive discussion of the issues playing a role in presolar grains preservation was made by Huss & Lewis (1995). Obviously, the initial abundances of presolar grains in the different chondrite groups were not identical, as we expect that these materials consolidated at different heliocentric distances where the materials experienced different thermal processing (Huss et al 2003).…”

Section: Discussionmentioning

confidence: 96%

“…Moreover, the CV3 chondrites may have lost most of the fragile presolar grains before they ever accreted due to high temperatures in the nebula (e.g. Huss et al 2003;Huss 2004). Bonal, Quirico & Bourot-Denise (2004) and Bonal et al (2006) performed Raman spectroscopy of organic matter to better determine the petrologic type of some CVs.…”

Section: The CV Groupmentioning

confidence: 99%

“…Huss, Lewis & Hemkin (1996) expanded on the interpretation of these data by including the carrier of the 'normal planetary'noble gases. Huss et al (2003) expanded the database to include additional carbonaceous chondrites. While chemical procedures allow the separation of diamonds, SiC and other chemically resistant grains contained in chondrites (see e.g.…”

Section: Introduction: Abundances Of Presolar Grainsmentioning

confidence: 99%

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The Effect of Aqueous Alteration and Metamorphism in the Survival of Presolar Silicate Grains in Chondrites

Trigo‐Rodríguez

Blum

2009

Publ. – Astron. Soc. Aust

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Abstract:Relatively small amounts (typically between 2 and 200 ppm) of presolar grains have been preserved in the matrices of chondritic meteorites. The measured abundances of the different types of grains are highly variable from one chondrite to another, but are higher in unequilibrated chondrites that have experienced little or no aqueous alteration and/or metamorphic heating than in processed meteorites. A general overview of the abundances measured in presolar grains (particularly the recently identified presolar silicates) contained in primitive chondrites is presented. Here we will focus on the most primitive chondrite groups, as typically the highest measured abundances of presolar grains occur in primitive chondrites that have experienced little thermal metamorphism. Looking at the most aqueously altered chondrite groups, we find a clear pattern of decreasing abundance of presolar silicate grains with increasing levels of aqueous alteration. We conclude that measured abundances of presolar grains in altered chondrites are strongly biased by their peculiar histories. Scales quantifying the intensity of aqueous alteration and shock metamorphism in chondrites could correlate with the content of presolar silicates. To do this it would be required to infer the degree of destruction or homogenization of presolar grains in the matrices of primitive meteorites. To get an unbiased picture of the relative abundance of presolar grains in the different regions of the protoplanetary disk where first meteorites consolidated, future dedicated studies of primitive meteorites, IDPs, and collected materials from sample-return missions (like e.g. the planned Marco Polo) are urgently required.

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Section: Discussionmentioning

confidence: 96%

Section: The CV Groupmentioning

confidence: 99%

Section: Introduction: Abundances Of Presolar Grainsmentioning

confidence: 99%

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The Effect of Aqueous Alteration and Metamorphism in the Survival of Presolar Silicate Grains in Chondrites

Trigo‐Rodríguez

Blum

2009

Publ. – Astron. Soc. Aust

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“…Low-density graphite grains show 18 O enrichment in many of the grains that are taken as proof that they formed in core-collapse supernovae: 18 O is produced via 14 N(α,γ) 18 F(e + ν) 18 O in the partial He burning zone, resulting 18 O/ 16 O ratio of 1.68 in a 15M sun model by Rauscher et al [40]. Many low-density graphite grains show 28 Si excesses, similar to SiC X grains from supernovae, while a few show 29 Si and 30 Si excesses.…”

mentioning

confidence: 95%

“…SiC grains are present in various chemical types of meteorites [14,16]. Their abundance in the Murchison meteorite (CM2) is ~6 ppm relative to a bulk meteorite [17].…”

Section: Introductionmentioning

confidence: 99%

Nucleosynthetic Signatures in Presolar SiC and Graphite Grains

Amari¹

2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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Presolar SiC and graphite grains are the grain types whose isotopic signatures have been extensively studied. Isotopic compositions of light and intermediate elements in single grains have been analyzed mostly using secondary ion mass spectrometry. Detailed information about nucleosynthetic conditions can be obtained from isotopic compositions of heavy elements. Isotopic compositions of heavy elements in SiC and graphite grains have been analyzed using resonant ionization mass spectrometry. Analyses of heavy elements and noble gases are likely to produce new insights into presolar grains using newly-developed instruments.

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Primitive Asteroids

Weisberg¹,

Righter²

2014

Special Publications

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Presolar diamond, silicon carbide, and graphite in carbonaceous chondrites: implications for thermal processing in the solar nebula

Cited by 185 publications

References 62 publications

The Effect of Aqueous Alteration and Metamorphism in the Survival of Presolar Silicate Grains in Chondrites

The Effect of Aqueous Alteration and Metamorphism in the Survival of Presolar Silicate Grains in Chondrites

Nucleosynthetic Signatures in Presolar SiC and Graphite Grains

Primitive Asteroids

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