Meteoritics & Planetary Science最新文献

{"title":"CM carbonaceous chondrite petrofabrics and their implications for understanding the relative chronologies of parent body deformation and aqueous alteration","authors":"C. J. Floyd,&nbsp;L. E. Jenkins,&nbsp;P.-E. Martin,&nbsp;L. Daly,&nbsp;M. R. Lee","doi":"10.1111/maps.14303","DOIUrl":"https://doi.org/10.1111/maps.14303","url":null,"abstract":"<p>CM chondrites have been subjected to numerous alteration processes including brecciation and ductile deformation. Here, we present the results of 2D and 3D petrofabric analysis across a suite of meteorites: Aguas Zarcas, Cold Bokkeveld, Lewis Cliff (LEW) 85311, Murchison, and Winchcombe. We find that chondrule-defined petrofabrics are commonplace, but not ubiquitous. Where petrofabrics are present, alignment is typically observed in the chondrule long axes defining foliation fabrics. Alongside previous authors we interpolate the shock pressures to generate such fabrics between 27.8 and 41.8 GPa. Impacts capable of generating these shock pressures should ordinarily produce shock microstructures in olivine something not observed in the CMs. Whilst high calculated pre-compaction porosities may have had a role in attenuating energy transfer during collisions, we suggest the assumption of chondrule sphericity used in these calculations is misplaced and that a non-spherical pre-deformation chondrule shape is likely responsible for the dichotomy. We also reveal that the relative timings of aqueous alteration, brecciation, and deformation vary between CMs. Within Aguas Zarcas, we find multiple lithic clasts interpreted as having experienced different degrees of aqueous alteration, with opposing fabrics that formed after water/rock interaction but prior to brecciation. Meanwhile, within Cold Bokkeveld, we find a consistent fabric between clasts suggesting the fabric was imposed after both aqueous alteration and brecciation.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"324-346"},"PeriodicalIF":2.2,"publicationDate":"2025-01-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14303","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143424125","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Tissintite-II in lunar meteorite Northwest Africa 13967: Implications for the high pressure/temperature mineralogy of the lunar regolith","authors":"Axel Wittmann,&nbsp;Christian R. Kroemer,&nbsp;Meenakshi Wadhwa,&nbsp;Thomas G. Sharp,&nbsp;Matthijs Van Soest,&nbsp;Trevor Martin,&nbsp;Tyler Goepfert","doi":"10.1111/maps.14311","DOIUrl":"https://doi.org/10.1111/maps.14311","url":null,"abstract":"<p>We studied lunar regolith breccia meteorite Northwest Africa (NWA) 13967 to explore its mineral and clast inventory with special focus on the ubiquitous occurrence of tissintite-II, a newly recognized, vacancy-rich high-pressure clinopyroxene with a feldspathic, Fe- and Mg-enriched composition. Lithic clasts in NWA 13967 indicate a provenance in the Feldspathic Highlands Terrane on the Moon. Most abundant are cumulate impact melt clasts (“poikilitic granulitic breccias”), granular impact melt rocks, vitric impact melt clasts including impact spherules, and anorthositic clasts, while basalt clasts are rare. The breccia groundmass is mostly fused to flow-textured, vesicular, crystallized impact melt that includes 1 μm corundum crystals and up to 5 μm tissintite-II near the contact with lithic clasts. Rare coesite occurs in moganite clasts entrained in the shock-melted groundmass and rimmed by tissintite-II. Petrographic features of NWA 13967 and its bulk rock chemical composition are most similar to the NWA 8046 clan of lunar meteorites, the largest known lunar meteorite. We discuss mineralogical and petrological characteristics of NWA 13967 to unravel chemical and structural changes of the lunar regolith during shock lithification, which may inform the ongoing exploration of the lunar surface.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"484-505"},"PeriodicalIF":2.2,"publicationDate":"2025-01-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143632823","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Using X-ray computed microtomography (μCT) to determine subsample-specific cosmogenic noble gas production rates of E (enstatite) chondrites","authors":"M. Mijjum,&nbsp;B. J. Andrews,&nbsp;T. J. McCoy,&nbsp;C. M. Corrigan,&nbsp;M. W. Caffee,&nbsp;M. M. Tremblay","doi":"10.1111/maps.14309","DOIUrl":"https://doi.org/10.1111/maps.14309","url":null,"abstract":"<p>Cosmic ray exposure (CRE) ages provide information about the parent bodies and source regions of meteorite classes. Cosmogenic noble gases are often used to quantify exposure time scales ranging from tens of ka to hundreds of Ma. The production rate of cosmogenic noble gases is primarily controlled by a meteorite's chemical composition. Historically, an average chemical composition for an entire meteorite class or subgroup was used to calculate production rates. At the scale needed for noble gas measurements, however, some meteorites exhibit mineral abundance variabilities that translate into chemical heterogeneities, necessitating subsample-specific production rates. We find that the metal and sulfide content can vary significantly between ~100 and 300 mg subsamples of the same enstatite (E) chondrite, leading to &gt;10% differences in cosmogenic ²¹Ne production rates between subsamples. We demonstrate an approach to determining subsample-specific production rates using E chondrites. We use electron microprobe analysis and X-ray computed microtomography to quantify the chemical composition and abundances, respectively, of metal, sulfide, and silicate minerals in six E chondrites and calculate subsample-specific production rates of ³He and ²¹Ne. By applying this method to more E chondrite subsamples alongside noble gas measurements, we may begin to address broader questions, such as whether peaks in the E chondrite CRE age distribution can be attributed to distinct impact events.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"442-463"},"PeriodicalIF":2.2,"publicationDate":"2025-01-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14309","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143632941","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Systematic meteorite collection in the Catalina Dense Collection area (Chile): Description and statistics","authors":"Carine Sadaka,&nbsp;Jérôme Gattacceca,&nbsp;Matthieu Gounelle,&nbsp;Mathieu Roskosz,&nbsp;Anthony Lagain,&nbsp;Romain Tartese,&nbsp;Lydie Bonal,&nbsp;Clara Maurel,&nbsp;Rodrigo Martinez,&nbsp;Millarca Valenzuela","doi":"10.1111/maps.14307","DOIUrl":"https://doi.org/10.1111/maps.14307","url":null,"abstract":"<p>We present the outcome of search campaigns conducted in the Catalina Dense Collection area (DCA) located in the central depression of the Atacama Desert, Chile. The “Catalina Systematic Collection” (CSC) was assembled through systematic on-foot searches, resulting in a total of 1599 meteorites, before pairing, collected over a surface of 6.80 km². This yielded a recovery density of 235 meteorites per km² (67 meteorites &gt;20 g per km²), making it the densest among hot deserts, even higher than the neighboring El Médano DCA collection. This confirms that the central depression of the Atacama Desert holds the highest meteorite density among hot deserts. We classified 457 meteorites weighing more than 20 g. After correcting for various recovery biases, we estimated a true meteorite density on the ground of 131 meteorites per km² for meteorites &gt;20 g before pairing. Using a probabilistic approach, we calculated an average pairing likelihood, yielding 71 meteorites &gt;20 g per km² after pairing. This high density is likely linked to an old age of the CSC, which would also explain the absence of carbonaceous chondrites, as they are more prone to alteration by abrasion. This long meteorite accumulation period is related to the long-term hyper-aridity and surface stability of the Atacama Desert, which have persisted for several million years. Meteorites from the CSC show less chemical weathering on average than in other hot deserts, despite the long accumulation period. The H/L ratio in the CSC is higher than in meteorites from other hot deserts, Antarctica, and falls, but similar to the El Médano collection, potentially reflecting variations in the composition of the meteorite flux over the past Myr.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"308-323"},"PeriodicalIF":2.2,"publicationDate":"2025-01-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14307","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423525","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Revised chronology and expanded insights: Geologic perspective on the Luna impact event and its influence on the Harappan Civilization","authors":"G. K. Indu,&nbsp;S. James,&nbsp;Sachana Sathyan,&nbsp;J. Aswathi,&nbsp;V. R. Rani,&nbsp;V. M. Nair,&nbsp;Libiya M. Varghese,&nbsp;K. S. Sajinkumar,&nbsp;Nayan Sharma,&nbsp;Mitthu Dhali,&nbsp;Aryavart Anand,&nbsp;V. J. Rajesh,&nbsp;M. N. Praveen,&nbsp;Anil Chavan,&nbsp;Subhash Bhandari,&nbsp;Javed N. Malik","doi":"10.1111/maps.14308","DOIUrl":"https://doi.org/10.1111/maps.14308","url":null,"abstract":"<p>Luna is a potential impact crater located in the Banni Plains of the Kutch Basin in western India. The suspected impactites, collected from a 1-m deep trench near the vicinity of the Luna structure, possess a range of physical (porosity and magnetism) properties. Petrographic studies reveal that these impactites are dominated by wüstite, kirschsteinite, spinel, olivine, and quartz (in decreasing order of abundance), with a few silica grains exhibiting potential planar fractures (PF). These impactites can be grouped into three distinct melt classes based on their wüstite and kirschsteinite content (classified as Ca-rich, Ca-poor, and transitional type). Spectroscopic analysis indicates a higher concentration of wüstite in magnetic samples, whereas weakly magnetic to non-magnetic samples have an elevated presence of kirschsteinite. Major oxide geochemistry comparison between the impactites and the surrounding Banni Plain sediments show that some Luna impactites have a chemical affinity with a terrestrial or transitional setting, whereas the remaining samples portray a non-terrestrial trend suggesting notable mixing of target rock and projectile material. Optically stimulated luminescence dating of the sediment layer containing the impactites yielded an age of 4045 ± 182 years for the impact, consistent with the earlier proposed age of &lt;6900 years based on radiocarbon dating. The revised age places the Luna impact event much closer to the time frame of the Harappan Civilization's decline, suggesting that it may have had a greater impact on the Harappan Civilization than previously thought.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"422-441"},"PeriodicalIF":2.2,"publicationDate":"2025-01-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143632763","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Cover","authors":"","doi":"10.1111/maps.14195","DOIUrl":"https://doi.org/10.1111/maps.14195","url":null,"abstract":"<p>\u0000 \u0000 <figure>\u0000 <div><picture>\u0000 <source></source></picture><p></p>\u0000 </div>\u0000 </figure>\u0000 </p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 1","pages":"i"},"PeriodicalIF":2.2,"publicationDate":"2025-01-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14195","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143114005","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Petrology and shock history of hybrid lunar feldspathic–troctolitic breccia Northwest Africa 11515","authors":"Y. Li,&nbsp;P. J. A. McCausland,&nbsp;R. L. Flemming,&nbsp;G. R. Osinski","doi":"10.1111/maps.14301","DOIUrl":"https://doi.org/10.1111/maps.14301","url":null,"abstract":"<p>Lunar impact breccia meteorites contain clasts from unknown lunar regions, including areas not studied by past missions. These meteorites offer a unique opportunity to expand our knowledge of the Moon's crustal and mantle composition and processes. The recently classified lunar meteorite Northwest Africa (NWA) 11515 is a moderately shocked feldspathic breccia with anorthite plagioclase and mafic minerals. In this work, we report the shock history of lithic clasts using 2-D micro-X-ray diffraction, detailed mineralogy from micro-X-ray fluorescence, and electron probe microanalysis. NWA 11515 shows moderately shocked anorthite and highly shocked olivine and pyroxene. The plagioclase composition is invariant (An96.4 ± 0.7, <i>n</i> = 52), with variable mafic clasts overlapping Mg- and FAN-suite lithologies (Mg# 84.5 to 45.6 for olivine; Mg# 85.6 to 32.2 for pyroxene), similar to KREEP-depleted troctolites in Allan Hills A81005. Spinel-group oxides vary from aluminous spinel to chromite and ulvöspinel. We also observed slow-cooled augite Ca-poor pyroxene exsolution clasts and fast-quenched fine-grained anorthite–olivine co-crystallized clasts (&lt;5 μm), indicating different cooling histories. Combining petrological observations with published geochemical data, we show NWA 11515 has the mixed lithology of ferroan anorthosites with KREEP-poor magnesian rock fragments. With shock analysis, the materials are likely from a crater with minimum size of 7 km. Finally, we examined the published geochemical data for other lunar meteorites and hypothesize that other typical feldspathic breccias could contain magnesian clasts, suggesting the subdivision of typical feldspathic breccia into magnesian clast-hosting breccia and ferroan feldspathic breccia. This implies that non-KREEP magnesian magmatism might be more widespread in the post-LMO era on lunar highlands.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"347-370"},"PeriodicalIF":2.2,"publicationDate":"2025-01-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423720","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Search for pre-accretionary irradiation effects in calcium-aluminum inclusions from the CV3 chondrite Allende","authors":"P. Ghaznavi,&nbsp;C. Burkhardt,&nbsp;F. L. H. Tissot,&nbsp;I. Leya","doi":"10.1111/maps.14300","DOIUrl":"https://doi.org/10.1111/maps.14300","url":null,"abstract":"<p>Calcium-aluminum-rich inclusions (CAIs) are the first objects that formed in the solar accretion disk and therefore provide valuable insights into the evolution of the early solar system. A long-standing question regarding this earliest formative period relates to the storage of CAIs in the 1–4 Myr time period between their formation and later accretion into chondrite parent bodies. Were the CAIs stored in a pre-existing parent body, or in distant parts of the solar accretion disk? In the latter scenario, CAIs might have been exposed to cosmic rays, either from the galaxy or from the Sun and such pre-accretion irradiation effects might be detectable. We searched for such pre-accretional irradiation effects in 7 fine- and 11 coarse-grained CAIs from the CV 3.6 carbonaceous chondrite Allende. The extracted samples were analyzed for their major chemical composition and all samples were analyzed using μCT techniques. Using physical model calculations, ²¹Ne_cos and (²²Ne/²¹Ne)_cos production rate ratios were calculated for each CAI by fully considering their individual chemical composition. Measured He, Ne, Ar, and Kr isotope compositions of the CAIs show cosmogenic signals; clear signals for He and Ne isotopes; and detectable signals for some of the Ar and Kr isotopes. In addition, most samples show clear indications for radiogenic ⁴He and some samples show evidence for radiogenic ⁴⁰Ar. Higher ³⁶Ar/³⁸Ar, ²²Ne/²¹Ne, ⁸⁰Kr/⁸⁴Kr, and ⁸²Kr/⁸⁴Kr ratios together with lower cosmogenic ³⁸Ar_cos concentrations in fine-grained CAIs compared to coarse-grained CAIs are consistent with more alteration of the former compared to the latter. The CRE ages for the CAIs range between 4.12 ± 0.41 Myr and 6.40 ± 0.63 Myr. Statistical tests indicate that the data are normally distributed with no outliers, indicating that all CAIs share a common irradiation history, likely the irradiation in the Allende meteoroid. The average CRE age of 4.87 ± 0.19 Myr agrees with the nominally accepted CRE age of Allende of ~5.2 Myr. There is no correlation between ²¹Ne_cos concentrations and indicators of aqueous alteration like Na and/or U concentrations. The lack of correlation together with the finding of normally distributed modeled CRE ages indicates that either none of the studied CAIs experienced a pre-accretion irradiation before parent body compaction and/or that any pre-accretion irradiation effects have been completely erased during aqueous alteration events. Taking alteration aside, the findings are not in favor of X-wind type models but are more consistent with the idea of CAI outward transport in an expanding disk.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"247-272"},"PeriodicalIF":2.2,"publicationDate":"2025-01-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14300","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423523","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Geology, gravity, and numerical modeling of the Nova Colinas impact structure, Parnaíba Basin, Brazil","authors":"Pietro Demattê Avona,&nbsp;Alvaro Penteado Crósta,&nbsp;Marcos Alberto Rodrigues Vasconcelos,&nbsp;Evan Bjonnes,&nbsp;Fernando Lessa Pereira,&nbsp;Ana Maria Góes","doi":"10.1111/maps.14306","DOIUrl":"https://doi.org/10.1111/maps.14306","url":null,"abstract":"<p>Nova Colinas, centered at 07°09′33″ S/46°06′30″ W, is the ninth confirmed complex impact structure in Brazil and the fifth in the Parnaíba Basin, with a diameter of ~6.5–7 km and a nearly circular shape. Impactites include shocked siltstones from the Pedra de Fogo Fm. found at the central peak, brecciated sandstone from the Sambaíba Fm. bearing microscopic shock features, and brecciated basalt from the Mosquito Fm. bearing shatter cones. The impact event's age has been constrained to the interval from ~130 to ~199 Ma based on the local stratigraphy. Due to its moderate to advanced stage of erosion, geophysical modeling combined with geological field data were employed for its characterization. A new geological map was produced through field observations and remote sensing image interpretation, as well as a 3-D model based on ground gravity data and numerical modeling. iSALE2D shock physics code was employed to simulate the formation of Nova Colinas crater. The results revealed its main structural zones: the central uplift, annular basin, and outer rim, each associated with specific lithostratigraphic units from the Parnaíba Basin. Bouguer residual anomalies ranged from −3.6 to 1.2 mGal, with a nearly circular positive anomaly at the center of the structure, surrounded by a negative anomaly. 3-D gravity data inversion indicated a buried high-density body, likely due to the uplift of a diabase sill. Results of the numerical modeling point out that the final crater reached gravitational stability with a diameter of ~7 km and a depth of ~240 m, suggesting that a narrow outcrop strip of the Motuca Fm. was uplifted to a higher level compared to the Sambaíba Fm. strata, forming an antiform-like “arch” that creates an inner ring that exposes rocks of the Motuca Formation.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"286-307"},"PeriodicalIF":2.2,"publicationDate":"2025-01-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423522","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Petrologic characterization of CO3.0 chondrites: Implications for 60Fe-60Ni analyses","authors":"Myriam Telus,&nbsp;Tyler D. Wickland,&nbsp;Kyle Kim,&nbsp;Steven Simon","doi":"10.1111/maps.14299","DOIUrl":"https://doi.org/10.1111/maps.14299","url":null,"abstract":"<p>Samples in which Fe and Ni isotopes have not been disturbed by secondary processing are essential for constraining the initial solar system abundance of short-lived radionuclide ⁶⁰Fe, (⁶⁰Fe/⁵⁶Fe)_SS. However, Fe- and Ni-enriched veins and fractures within chondrules in unequilibrated ordinary chondrites (UOCs) imply late-stage open-system alteration that poses a potential problem for both bulk and <i>in situ</i> ⁶⁰Fe-⁶⁰Ni systematics. This study focuses on petrologic characterization of CO3.0s, which show significantly less secondary alteration than UOCs, potentially making them better targets for studying ⁶⁰Fe-⁶⁰Ni systematics. We determined the petrologic type of several CO3.0 meteorites with two independent approaches, Raman spectroscopy of matrix material and Cr₂O₃ content of FeO-rich olivine grains. CO3 chondrites analyzed in this study range from 3.00 to 3.2 in petrologic type with slight variations between results from the two different methods. Upon analyzing two thin sections of DOM 08006, one of the most pristine CO3 chondrites known, we found a chemically anomalous region, indicative of parent body hydrothermal alteration. Using the X-ray fluorescence microscopy beamline at the Australian Synchrotron, we collected high-resolution quantitative element maps to evaluate Fe and Ni mobilization for several CO3.0s. These results indicate that late-stage Fe and Ni mobilization like that observed in UOC samples is minor for most CO3 chondrites, highly localized and mostly limited to chondrule rims. Our results support that CO3.0s are well suited for further investigation of ⁶⁰Fe-⁶⁰Ni systematics and that detailed characterization of both the petrologic type and late-stage Fe and Ni mobilization of samples is important for further development of this short-lived radionuclide system.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"225-246"},"PeriodicalIF":2.2,"publicationDate":"2025-01-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14299","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143424020","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"地球科学","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}