scholarly journals Oxygen isotope characteristics of chondrules from the Yamato-82094 ungrouped carbonaceous chondrite: Further evidence for common O-isotope environments sampled among carbonaceous chondrites

2016 ◽  
Vol 52 (2) ◽  
pp. 268-294 ◽  
Author(s):  
T. J. Tenner ◽  
M. Kimura ◽  
N. T. Kita
Keyword(s):  
Oxygen Isotope ◽  
Carbonaceous Chondrite ◽  
Carbonaceous Chondrites ◽  
O Isotope

scholarly journals Insights into the origin of carbonaceous chondrite organics from their triple oxygen isotope composition

2018 ◽  
Vol 115 (34) ◽  
pp. 8535-8540 ◽  
Author(s):  
Romain Tartèse ◽  
Marc Chaussidon ◽  
Andrey Gurenko ◽  
Frédéric Delarue ◽  
François Robert
Keyword(s):  
Organic Matter ◽  
Oxygen Isotope ◽  
Carbonaceous Chondrite ◽  
Isotope Composition ◽  
Isotopic Fractionation ◽  
Oxygen Isotope Composition ◽  
Insoluble Organic Matter ◽  
O Isotope ◽  
Protosolar Nebula ◽  
Mass Dependent

Dust grains of organic matter were the main reservoir of C and N in the forming Solar System and are thus considered to be an essential ingredient for the emergence of life. However, the physical environment and the chemical mechanisms at the origin of these organic grains are still highly debated. In this study, we report high-precision triple oxygen isotope composition for insoluble organic matter isolated from three emblematic carbonaceous chondrites, Orgueil, Murchison, and Cold Bokkeveld. These results suggest that the O isotope composition of carbonaceous chondrite insoluble organic matter falls on a slope 1 correlation line in the triple oxygen isotope diagram. The lack of detectable mass-dependent O isotopic fractionation, indicated by the slope 1 line, suggests that the bulk of carbonaceous chondrite organics did not form on asteroidal parent bodies during low-temperature hydrothermal events. On the other hand, these O isotope data, together with the H and N isotope characteristics of insoluble organic matter, may indicate that parent bodies of different carbonaceous chondrite types largely accreted organics formed locally in the protosolar nebula, possibly by photochemical dissociation of C-rich precursors.

Mineralogical characterization of a unique material having heavy oxygen isotope anomaly in matrix of the primitive carbonaceous chondrite Acfer 094

2008 ◽  
Vol 72 (11) ◽  
pp. 2723-2734 ◽  
Author(s):  
Yusuke Seto ◽  
Naoya Sakamoto ◽  
Kiyoshi Fujino ◽  
Takashi Kaito ◽  
Tetsuo Oikawa ◽  
...  
Keyword(s):  
Oxygen Isotope ◽  
Carbonaceous Chondrite ◽  
Mineralogical Characterization ◽  
Unique Material

scholarly journals Arrival and magnetization of carbonaceous chondrites in the asteroid belt before 4562 million years ago

2020 ◽  
Vol 1 (1) ◽  
Author(s):  
Timothy O’Brien ◽  
John A. Tarduno ◽  
Atma Anand ◽  
Aleksey V. Smirnov ◽  
Eric G. Blackman ◽  
...  
Keyword(s):  
Solar System ◽  
Arrival Time ◽  
Carbonaceous Chondrite ◽  
Parent Body ◽  
Asteroid Belt ◽  
Carbonaceous Chondrites ◽  
Early Solar System ◽  
Outer Disk ◽  
Main Asteroid Belt ◽  
Insight Into

AbstractMeteorite magnetizations can provide rare insight into early Solar System evolution. Such data take on new importance with recognition of the isotopic dichotomy between non-carbonaceous and carbonaceous meteorites, representing distinct inner and outer disk reservoirs, and the likelihood that parent body asteroids were once separated by Jupiter and subsequently mixed. The arrival time of these parent bodies into the main asteroid belt, however, has heretofore been unknown. Herein, we show that weak CV (Vigarano type) and CM (Mighei type) carbonaceous chondrite remanent magnetizations indicate acquisition by the solar wind 4.2 to 4.8 million years after Ca-Al-rich inclusion (CAI) formation at heliocentric distances of ~2–4 AU. These data thus indicate that the CV and CM parent asteroids had arrived near, or within, the orbital range of the present-day asteroid belt from the outer disk isotopic reservoir within the first 5 million years of Solar System history.

scholarly journals A primordial 15N-depleted organic component detected within the carbonaceous chondrite Maribo

2020 ◽  
Vol 10 (1) ◽  
Author(s):  
Christian Vollmer ◽  
Jan Leitner ◽  
Demie Kepaptsoglou ◽  
Quentin M. Ramasse ◽  
Ashley J. King ◽  
...  
Keyword(s):  
Organic Matter ◽  
Interstellar Medium ◽  
Structural Information ◽  
Carbonaceous Chondrite ◽  
Carbonaceous Chondrites ◽  
Local Interstellar Medium ◽  
Edge Structure ◽  
Electron Energy Loss ◽  
Cm Chondrite ◽  
X Ray Absorption

AbstractWe report on the detection of primordial organic matter within the carbonaceous chondrite Maribo that is distinct from the majority of organics found in extraterrestrial samples. We have applied high-spatial resolution techniques to obtain C-N isotopic compositions, chemical, and structural information of this material. The organic matter is depleted in 15N relative to the terrestrial value at around δ15N ~ -200‰, close to compositions in the local interstellar medium. Morphological investigations by electron microscopy revealed that the material consists of µm- to sub-µm-sized diffuse particles dispersed within the meteorite matrix. Electron energy loss and synchrotron X-ray absorption near-edge structure spectroscopies show that the carbon functional chemistry is dominated by aromatic and C=O bonding environments similar to primordial organics from other carbonaceous chondrites. The nitrogen functional chemistry is characterized by C-N double and triple bonding environments distinct from what is usually found in 15N-enriched organics from aqueously altered carbonaceous chondrites. Our investigations demonstrate that Maribo represents one of the least altered CM chondrite breccias found to date and contains primordial organic matter, probably originating in the interstellar medium.

Apatite Texture, Composition, and O-Sr-Nd Isotope Signatures Record Magmatic and Hydrothermal Fluid Characteristics at the Black Mountain Porphyry Deposit, Philippines

2021 ◽  
Author(s):  
Ming Jian Cao ◽  
Noreen J. Evans ◽  
Pete Hollings ◽  
David R. Cooke ◽  
Brent I.A. McInnes ◽  
...  
Keyword(s):  
Phase Separation ◽  
High Temperature ◽  
Oxygen Isotope ◽  
Hydrothermal Alteration ◽  
Hydrothermal Fluid ◽  
Isotope Composition ◽  
Hydrothermal Fluids ◽  
Nd Isotope ◽  
O Isotope ◽  
Black Mountain

Abstract The trace elemental and isotopic signatures in apatite can be modified during hydrothermal alteration. This study investigates the suitability of apatite as an indicator of the source, chemistry, and evolution of magma and hydrothermal fluids. In situ textural, elemental, and O-Sr-Nd isotope analyses were performed on apatite in thin sections, from fresh and propylitically altered pre- and synmineralized dioritic porphyries from the Black Mountain porphyry Cu deposit in the Philippines. All studied apatite crystals have similar subhedral to euhedral shapes and are homogeneous in the grayscale in backscattered electron images. In cathodoluminescence images, the apatite in fresh and altered rocks displays yellow to yellow-green and green to brown luminescence, respectively. Apatite in fresh rocks has a higher Cl and Mn content, and lower Fe, Mg, Sr, Pb, and calculated XOH-apatite, compared to apatite in altered rocks. The content of F, rare earth elements (REEs), Y, U, Th, and Zr, and the Sr-Nd isotope signatures of apatite from fresh and altered rocks are similar in all apatite grains (87Sr/86Sr = 0.7034–0.7042 vs. 0.7032–0.7043, εNd(t) = 5.3–8.0 vs. 5.1–8.4). The X-ray maps and elemental and oxygen isotope signatures across individual apatite crystals are typically homogeneous in apatite from both fresh and altered rocks. The distinct luminescence colors, coupled with distinct mobile element compositions (Cl, OH, Mn, Mg, Fe, Sr, Pb), indicate modification of primary magmatic apatite during interaction with hydrothermal fluids. The similarities in Sr isotope ratios (87Sr/86Sr = 0.7032–0.7043) but slight differences in O isotope signatures (δ18O = 6.0 ± 0.3‰ vs. 6.6 ± 0.3‰) in apatite from fresh and altered rocks are consistent with the magma and hydrothermal fluids having the same source and suggest significant phase separation in the hydrothermal fluids given that 18O preferentially fractionates into the residual liquid relative to 16O during phase separation. The similarity of immobile element (REE, Y, U, Th, and Zr) contents in both populations of apatite, consistency of textures and Nd isotope compositions, and absence of obvious dissolution-reprecipitation features all suggest that altered apatite retains some magmatic characteristics. The apatite in fresh rocks has oxygen isotope compositions similar to that of zircons from the same sample (δ18O = 5.9 ± 0.3‰), indicating little to no oxygen isotope fractionation between zircon and apatite and that apatite can be a good proxy for the oxygen isotope composition of the magma. Based on the Cl contents of the magmatic and replacement apatite, and assuming their equilibrium with high-temperature magma fluid and replacement hydrothermal fluid, respectively, the calculated Cl content of the early magmatic fluid and the later replacement fluid can be estimated to be 6.4 to 15.1 wt % and ~0.25 ± 0.03 wt %, respectively. This indicates a depletion of Cl from the early high-temperature fluid to the replacement fluid, consistent with phase separation. This study demonstrates that cathodoluminescence, elemental compositions (such as Cl, Mn, Mg, Fe, Sr, Pb) and Sr-O isotope signatures in apatite can be modified during hydrothermal alteration, whereas other components (REE, Y, U, Th, and Zr) and the Nd isotope composition are preserved. These features can be used to constrain the origin, chemistry, and evolution of the primary magma and ore-forming hydrothermal fluids.

Carbonaceous chondrite meteorites as a record of protoplanetary disk conditions

2019 ◽  
Vol 15 (S350) ◽  
pp. 135-138
Author(s):  
Sara S. Russell ◽  
Enrica Bonato ◽  
Helena Bates ◽  
Ashley J. King ◽  
Natasha V. Almeida ◽  
...  
Keyword(s):  
Organic Molecules ◽  
Carbonaceous Chondrite ◽  
Protoplanetary Disk ◽  
Parent Body ◽  
Carbonaceous Chondrites ◽  
Aqueous Processing ◽  
Chondritic Meteorites ◽  
Dust Component ◽  
Key Features ◽  
Complex Organic

AbstractChondritic meteorites, and especially the most volatile-rich chondrites, the carbonaceous chondrites, preserve a record of the solar protoplanetary disk dust component and how it has been changed both in the disk environment itself and in its asteroidal parent body. Here we review some of the key features of carbonaceous chondrites and report some new data on their organics component. These show that the nebula reached temperature of >10000C, but only very locally, to produce chondrules. Most meteoritic material underwent thermal and/or aqueous processing, but some retain delicate nebular components such as complex organic molecules and amorphous silicates.

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