Solid-state<sup>13</sup>C NMR characterization of insoluble organic matter from Antarctic CM2 chondrites: Evaluation of the meteoritic alteration level

Yabuta, Hikaru; Naraoka, Hiroshi; Sakanishi, Kinya; Kawashima, Hiroyuki

doi:10.1111/j.1945-5100.2005.tb00979.x

Cited by 39 publications

(47 citation statements)

References 37 publications

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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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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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“…Many analyses have been carried out on such meteorites with the aim of gaining some understanding of the dehydration process from the viewpoint of mineralogy and petrology (Akai, 1988;Tomeoka et al, 1989a, b;Akai, 1990;Tomeoka, 1990a, b;Bischoff and Metzler, 1991;Ikeda, 1991), inorganic and organic chemistry (Kitajima et al, 2002;Yabuta et al, 2005), and noble gases (Nagao et al, 1984;Nakamura et al, 2006). The results have led to the classification of heated hydrous chondrites into classes based on the degree of heating (Nakamura, 2005).…”

Section: Introductionmentioning

confidence: 99%

Evaluation of dehydration mechanism during heating of hydrous asteroids based on mineralogical and chemical analysis of naturally and experimentally heated CM chondrites

et al. 2008

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Based on the evidence derived from spectroscopic observation and meteorite analysis, some hydrous asteroids were heated and dehydrated for a certain period of time after aqueous alteration. In order to reproduce the dehydration processes, we experimentally heated Murchison CM chondrite at 600°C for 1 h (600°C/1 h), 600°C/96 h, 900°C/1 h, and 900°C/96 h under controlled oxygen partial pressures. The experimental products were compared with Belgica (B-)7904 CM chondrite, a meteorite from a dehydrated asteroid in terms of characteristic mineralogical and compositional properties. B-7904 shows properties intermediate between the two experimental products heated at 900°C/1 h and 900°C/96 h. In addition, the presence or the absence of some temperature-sensitive minerals in B-7904 suggests that it experienced heating at a temperature higher than 700°C but lower than 890°C. The duration of heating, based on the diffusion time needed to achieve the Fe-Mg zoning profile in olivine in B-7904, was estimated to be between 10 and 103 days at 700°C and between 1 to 102 h at 890°C. The obtained durations are much shorter than those expected from the internal heating model which requires prolonged heating over million years. Therefore, it is unlikely that the short-lived radionuclide of 26Al is a heat source for the dehydration of B-7904. Instead, short-duration local heating, such as that from impacts or solar radiation, is a more promising heat source.

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“…The origin of the soluble organic matter (SOM) -i.e. molecules released with organic solvents or water -has been attributed to the effects of hydrothermal processes in the parent body (Alexander et al 1998;Yabuta et al 2005), in which SOM could be the hydrolysis product of IOM. An alternative view considers SOM as a component of the ices that were accreted along with refractory phases, and therefore with no connection with IOM (Remusat et al 2005).…”

Section: Structural and Chemical Characterization Of Organic Matter Imentioning

confidence: 99%

“…These variations are controlled by heterogeneities in the precursors accreted by the parent bodies and by the effects of post-accretion processes (Cody & Alexander 2005;Quirico et al 2009). Post-accretion processes include low-temperature hydrothermalism (Cody & Alexander 2005;Yabuta et al 2005;Orthous-Daunay et al 2010a), long-duration radiogenic thermal metamorphism (Bonal et al 2006a(Bonal et al , 2007Busemann et al 2007), and short-duration thermal metamorphism (Yabuta et al 2010). IOM in interplanetary dust particules (IDPs) and antarctic micrometeorites (AMMs) has a fairly, but not strictly, similar polyaromatic structure to that of chondrites (Quirico et al 2005;Bonal et al 2006b;Dobrica et al 2009).…”

Section: Structural and Chemical Characterization Of Organic Matter Imentioning

confidence: 99%

Organic materials in planetary and protoplanetary systems: nature or nurture?

Ore

Fulchignoni

Cruikshank

et al. 2011

A&A

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Aims. The objective of this work is to summarize the discussion of a workshop aimed at investigating the properties, origins, and evolution of the materials that are responsible for the red coloration of the small objects in the outer parts of the solar system. Because of limitations or inconsistencies in the observations and, until recently, the limited availability of laboratory data, there are still many questions on the subject. Our goal is to approach two of the main questions in a systematic way: -Is coloring an original signature of materials that are presolar in origin ("nature") or stems from post-formational chemical alteration, or weathering ("nurture")? -What is the chemical signature of the material that causes spectra to be sloped towards the red in the visible? We examine evidence available both from the laboratory and from observations sampling different parts of the solar system and circumstellar regions (disks). Methods. We present a compilation of brief summaries gathered during the workshop and describe the evidence towards a primordial vs. evolutionary origin for the material that reddens the small objects in the outer parts of our, as well as in other, planetary systems. We proceed by first summarizing laboratory results followed by observational data collected at various distances from the Sun. Results. While laboratory experiments show clear evidence of irradiation effects, particularly from ion bombardment, the first obstacle often resides in the ability to unequivocally identify the organic material in the observations. The lack of extended spectral data of good quality and resolution is at the base of this problem. Furthermore, that both mechanisms, weathering and presolar, act on the icy materials in a spectroscopically indistinguishable way makes our goal of defining the impact of each mechanism challenging. Conclusions. Through a review of some of the workshop presentations and discussions, encompassing laboratory experiments as well as observational data, we infer that both "nature" and "nurture" are instrumental in the coloration of small objects in the outer parts Article published by EDP Sciences A98, page 1 of 14 A&A 533, A98 (2011) of the solar system. While in the case of some observations it is clear that the organic reddening material originated before the solar nebula (i.e. presolar grains found in meteorites), for many other cases pointers are not as clear and indicate a concurrence of both processes.

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Solid-state¹³C NMR characterization of insoluble organic matter from Antarctic CM2 chondrites: Evaluation of the meteoritic alteration level

Cited by 39 publications

References 37 publications

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

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

Evaluation of dehydration mechanism during heating of hydrous asteroids based on mineralogical and chemical analysis of naturally and experimentally heated CM chondrites

Organic materials in planetary and protoplanetary systems: nature or nurture?

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Solid-state13C NMR characterization of insoluble organic matter from Antarctic CM2 chondrites: Evaluation of the meteoritic alteration level

Cited by 39 publications

References 37 publications

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

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

Evaluation of dehydration mechanism during heating of hydrous asteroids based on mineralogical and chemical analysis of naturally and experimentally heated CM chondrites

Organic materials in planetary and protoplanetary systems: nature or nurture?

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Solid-state¹³C NMR characterization of insoluble organic matter from Antarctic CM2 chondrites: Evaluation of the meteoritic alteration level