Organic matter and metamorphic history of CO chondrites

Bonal, L.; Bourot-Denise, M.; Quirico, E.; Montagnac, Gilles; Lewin, É.

doi:10.1016/j.gca.2006.12.014

Cited by 163 publications

(235 citation statements)

References 62 publications

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“…We assumed that (1) 26 Al was the only heat source of a chondrite parent body, and was uniformly distributed in the protoplanetary disk with the canonical 26 Al/ 27 Al ratio of 5.25 Â 10 À 5 ; (2) some regions of these parent bodies reached 100 À 200°C (temperature range of fayalite formation 28 ) at the time of fayalite formation; and (3) that these regions avoided subsequent heating above 300°C (to preclude Fe-Mg diffusion in secondary fayalite). Supplementary Table 6 (part 1) defines parameters specific to the parent bodies from which the L, CV and CO chondrites were derived, such as the fayalite formation ages (Figs 4 and 5) and peak metamorphic temperatures experienced by these parent bodies 23,31,32 . We note that using an initial 26 Al/ 27 Al ratio of 5.25 Â 10 À 5 , rather than 5 Â 10 À 5 , corresponds to 0.05 Myr, which is well within the uncertainty of our isotope measurements (0.4 À 1.8 Myr).…”

Section: Methodsmentioning

confidence: 99%

Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite

et al. 2015

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Chronology of aqueous activity on chondrite parent bodies constrains their accretion times and thermal histories. Radiometric 53 Cr dating has been successfully applied to aqueously formed carbonates in CM carbonaceous chondrites. Owing to the absence of carbonates in ordinary (H, L and LL), and CV and CO carbonaceous chondrites, and the lack of proper standards, there are no reliable ages of aqueous activity on their parent bodies. Here we report the first 53 Mn-53 Cr ages of aqueously formed fayalite in the L3 chondrite Elephant Moraine 90161 as 2:4 þ 1:8 À 1:3 Myr after calcium-aluminium-rich inclusions (CAIs), the oldest Solar System solids. In addition, measurements using our synthesized fayalite standard show that fayalite in the CV3 chondrite Asuka 881317 and CO3-like chondrite MacAlpine Hills 88107 formed 4:2 þ 0:8 À 0:7 and 5:1 þ 0:5 À 0:4 Myr after CAIs, respectively. Thermal modelling, combined with the inferred conditions (temperature and water/rock ratio) and 53 Cr ages of aqueous alteration, suggests accretion of the L, CV and CO parent bodies B1.8 À 2.5 Myr after CAIs.

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Section: Methodsmentioning

confidence: 99%

Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite

et al. 2015

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“…Differences in the molecular structure of IOM between different classes of carbonaceous chondrites have been interpreted as consequences of parent-body heating and/or aqueous reactions. In particular, heating processes increase ordering and size of aromatic units and loss of the most labile constituents (Bonal et al 2007;Bonal et al 2006;Cody et al 2008;Remusat et al 2008;Sephton et al 2003), whereas hydrothermal alteration oxidizes IOM, adding hydroxyl groups and lowering the aliphatic component (Cody & Alexander 2005;Remusat et al 2005;Yabuta et al 2005). Nevertheless, very high D/H ratios in ordinary chondrites relative to other groups that appear to have undergone similar heating (CO and CV) are difficult to understand in the context of this interpretation of the origins of diversity among IOM components in chondritic meteorites (Alexander et al 2007).…”

Section: Introductionmentioning

confidence: 99%

Accretion and Preservation of D-Rich Organic Particles in Carbonaceous Chondrites: Evidence for Important Transport in the Early Solar System Nebula

Rémusat

Guan

Wang

et al. 2010

ApJ

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We have acquired NanoSIMS images of the matrices of CI, CM, and CR carbonaceous chondrites to study, in situ, the organic matter trapped during the formation of their parent bodies. D/H ratio images reveal the occurrence of D-rich hot spots, constituting isolated organic particles. Not all the organic particles are D-rich hot spots, indicating that at least two kinds of organic particles have been accreted in the parent bodies. Ratio profiles through D-rich hot spots indicate that no significant self-diffusion of deuterium occurs between the D-rich organic matter and the depleted hydrous minerals that are surrounding them. This is not the result of a physical shielding by any constituent of the chondrites. Ab initio calculations indicate that it cannot be explained by isotopic equilibrium. Then it appears that the organic matter that is extremely enriched in D does not exchange with the hydrous minerals, or this exchange is so slow that it is not significant over the 4.5 billion year history on the parent body. If we consider that the D-rich hot spots are the result of an exposure to intense irradiation, then it appears that carbonaceous chondrites accreted organic particles that have been brought to different regions of the solar nebula. This is likely the result of important radial and vertical transport in the early solar system.

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“…As shown by Raman spectrometry, the structural order of the carbonaceous matter increases with temperature [92,93]. There is a clear trend in losing the heteroelements, evidenced by a decrease in H/C, N/C and O/C elemental ratios, and in increasing the size of aromatic units [77,94].…”

Section: Diversity Among the Different Types Of Chondrites: Influencementioning

confidence: 95%

Organic and volatile elements in the solar system

Rémusat

2011

EPJ Web of Conferences

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Abstract. Chondrites and comets have accreted primitive materials from the early solar system. Those materials include organics, water and other volatile components. The most primitive chondrites and comets have undergone few modifications on their respective parent bodies and can deliver to laboratories components that were present at the origin of the protosolar nebula. Here I present a review of the organic material and volatile components that have been studied in the most primitive chondrites, and the last data from the stardust mission about the cometary record. This paper focuses on materials that can be studied in laboratories, by mass spectrometry, ion probes or organic chemistry techniques.

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Organic matter and metamorphic history of CO chondrites

Cited by 163 publications

References 62 publications

Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite

Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite

Accretion and Preservation of D-Rich Organic Particles in Carbonaceous Chondrites: Evidence for Important Transport in the Early Solar System Nebula

Organic and volatile elements in the solar system

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