Fullerenes and Related Structural Forms of Carbon in Chondritic Meteorites and the Moon

Heymann, D.; Cataldo, Franco; Pontier-Johnson, Marie; Rietmeijer, Frans J. M.

doi:10.1007/1-4020-4135-7_8

Cited by 2 publications

(3 citation statements)

References 114 publications

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“…These results suffer, however, from many of the same deficiencies as their initial reports of fullerenes, including failures to reproduce the results on similar samples (Mukhopadhyay et al, 1998;Farley and Mukhopadhyay, 2001;Koeberl et al, 2004;Farley et al, 2005), questions regarding sample identity (Braun et al, 2001;Isozaki, 2001), and quantitative concerns about planetary gas contributions to the recorded fullerene gas signals (Koeberl et al, 2004;Heymann et al, 2006). The identity of fullerenes as the carrier of the gas isotope anomaly is also circumstantial, although the ability of C 60 to encapsulate helium-3 is well known and has become a powerful tool in studying C 60 chemistry (DiCamillo et al, 1996;Saunders et al, 1996;Cooper et al, 2002).…”

Section: Introductionmentioning

confidence: 49%

“…Their interpretation contrasts sharply with the expectations that Allende fullerenes have reached or approached equilibrium during their formation or in post-formation processing. Allende has been exposed both to thermal metamorphosis (Rouzaud et al, 2005;Bonal et al, 2006Bonal et al, , 2007 and to high temperatures during Rouzaud atmospheric flight and collision with earth (Heymann et al, 2006;Braun et al, 2001). Thus, it might be expected that the fullerene envelope would have a more uneven distribution (Slanina et al, 2000).…”

Section: Fig 2 Presents the Results From Ldms Investigations Ofmentioning

confidence: 95%

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Identifying the source of a strong fullerene envelope arising from laser desorption mass spectrometric analysis of meteoritic insoluble organic matter

Hammond

Zare

2008

Geochimica et Cosmochimica Acta

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Section: Introductionmentioning

confidence: 49%

Section: Fig 2 Presents the Results From Ldms Investigations Ofmentioning

confidence: 95%

Identifying the source of a strong fullerene envelope arising from laser desorption mass spectrometric analysis of meteoritic insoluble organic matter

Hammond

Zare

2008

Geochimica et Cosmochimica Acta

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“…Their morphology includes an exterior shell around a highly vesicular interior, identical to YDB spherules and carbon spherules found in Europe. Carbon spherules have also been reported from experiments using hypervelocity impacts into carbonrich substrates, duplicating cosmic-impact conditions (Heymann et al 2006). Furthermore, carbon spherules containing NDs have been demonstrated to form from tree sap under laboratory conditions that duplicate the temperature, pressure, and redox values within an impact fireball (Israde-Alcá ntara et al 2012b).…”

Section: Introductionmentioning

confidence: 96%

Nanodiamond-Rich Layer across Three Continents Consistent with Major Cosmic Impact at 12,800 Cal BP

Kinzie¹,

Hee

Stich

et al. 2014

The Journal of Geology

170

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JSTOR is a not-for-profit service that helps scholars, researchers, and students discover, use, and build upon a wide range of content in a trusted digital archive. We use information technology and tools to increase productivity and facilitate new forms of scholarship. For more information about JSTOR, please contact support@jstor.org. A B S T R A C TA major cosmic-impact event has been proposed at the onset of the Younger Dryas (YD) cooling episode at ≈12,800 ‫ע‬ 150 years before present, forming the YD Boundary (YDB) layer, distributed over 150 million km 2 on four continents. In 24 dated stratigraphic sections in 10 countries of the Northern Hemisphere, the YDB layer contains a clearly defined abundance peak in nanodiamonds (NDs), a major cosmic-impact proxy. Observed ND polytypes include cubic diamonds, lonsdaleite-like crystals, and diamond-like carbon nanoparticles, called n-diamond and i-carbon. The ND abundances in bulk YDB sediments ranged up to ≈500 ppb (mean: 200 ppb) and that in carbon spherules up to ≈3700 ppb (mean: ≈750 ppb); 138 of 205 sediment samples (67%) contained no detectable NDs. Isotopic evidence indicates that YDB NDs were produced from terrestrial carbon, as with other impact diamonds, and were not derived from the impactor itself. The YDB layer is also marked by abundance peaks in other impact-related proxies, including cosmic-impact spherules, carbon spherules (some containing NDs), iridium, osmium, platinum, charcoal, aciniform carbon (soot), and high-temperature melt-glass. This contribution reviews the debate about the presence, abundance, and origin of the concentration peak in YDB NDs. We describe an updated protocol for the extraction and concentration of NDs from sediment, carbon spherules, and ice, and we describe the basis for identification and classification of YDB ND polytypes, using nine analytical approaches. The large body of evidence now obtained about YDB NDs is strongly consistent with an origin by cosmic impact at ≈12,800 cal BP and is inconsistent with formation of YDB NDs by natural terrestrial processes, including wildfires, anthropogenesis, and/or influx of cosmic dust.

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Fullerenes and Related Structural Forms of Carbon in Chondritic Meteorites and the Moon

Cited by 2 publications

References 114 publications

Identifying the source of a strong fullerene envelope arising from laser desorption mass spectrometric analysis of meteoritic insoluble organic matter

Identifying the source of a strong fullerene envelope arising from laser desorption mass spectrometric analysis of meteoritic insoluble organic matter

Nanodiamond-Rich Layer across Three Continents Consistent with Major Cosmic Impact at 12,800 Cal BP

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