Meteoritics & Planetary Science最新文献

{"title":"Cover","authors":"","doi":"10.1111/maps.14205","DOIUrl":"https://doi.org/10.1111/maps.14205","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 6","pages":""},"PeriodicalIF":2.2,"publicationDate":"2025-06-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14205","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144292908","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":"Characterization of iron meteorites by scanning electron microscopy, X-ray diffraction, magnetization measurements, and Mössbauer spectroscopy: Kayakent IIIAB","authors":"M. V. Goryunov,&nbsp;G. Varga,&nbsp;Z. Dankházi,&nbsp;A. V. Chukin,&nbsp;I. Felner,&nbsp;E. Kuzmann,&nbsp;Z. Homonnay,&nbsp;R. F. Muftakhetdinova,&nbsp;V. I. Grokhovsky,&nbsp;M. I. Oshtrakh","doi":"10.1111/maps.14363","DOIUrl":"https://doi.org/10.1111/maps.14363","url":null,"abstract":"<p>A fragment of the Kayakent IIIAB iron meteorite was analyzed using optical microscopy, scanning electron microscopy (SEM) with energy-dispersive spectroscopy (EDS) and electron backscatter diffraction (EBSD), X-ray diffraction (XRD), magnetization measurements, and Mössbauer spectroscopy. Optical microscopy and SEM show the presence of (i) the pure α₂-Fe(Ni, Co) grains, (ii) the γ-Fe(Ni, Co) phase grains, (iii) the γ-Fe(Ni, Co) rims around the α₂-Fe(Ni, Co) phase areas, (iv) the cloudy zone (a mixture of the γ-FeNi(Co) and α₂-Fe(Ni, Co) phases), (v) plessite structures, and (vi) schreibersite inclusions in the α-Fe(Ni, Co) phase. The α-Fe(Ni, Co) phase demonstrates the ε-structure α_ε-Fe(Ni, Co) with the presence of at least three different orientations of the α_ε-Fe(Ni, Co) microcrystals, as shown by EBSD. EDS indicates variations in the Ni concentrations in the following ranges: (i) ~5.4–7.2 atom% in the α-Fe(Ni, Co) phase, (ii) ~15–18 atom% in the α₂-Fe(Ni, Co) phase, and (iii) ~29–47 atom% in the γ-Fe(Ni, Co) phase grains. Schreibersite inclusions contain ~23.5–23.6 atom% of P, ~45.1–46.5 atom% of Fe, and ~28.8–31.4 atom% of Ni. The presence of ~98.1 wt% of the α-Fe(Ni, Co) phase and ~1.9 wt% of the γ-Fe(Ni, Co) phase is found by XRD in the powdered sample, while schreibersite is detected by XRD in the surface of the section only. Magnetization measurements show ferromagnetic multiphase material and a magnetic saturation moment of 175 emu g⁻¹. The room temperature Mössbauer spectrum of the powdered Kayakent IIIAB sample demonstrates six magnetic sextets related to the ferromagnetic α₂-Fe(Ni, Co), α-Fe(Ni, Co), and γ-Fe(Ni, Co) phases and one singlet assigned to the paramagnetic γ-Fe(Ni, Co) phase. In addition, the Mössbauer spectrum shows six minor magnetic sextets associated with ⁵⁷Fe in the M1, M2, and M3 sites in schreibersite and one minor doublet shape assigned to the superparamagnetic rhabdite microcrystals. The iron fractions in the detected phases can be roughly estimated as follows: (i) ~11.9% in the α₂-Fe(Ni, Co) phase, (ii) ~75.6% in the α-Fe(Ni, Co) phase, (iii) ~5.7% in the disordered γ-Fe(Ni, Co) phase with Ni content of ~34–40 atom%, (iv) ~1.5% in the more ordered γ-Fe(Ni, Co) phase with a higher Ni content (~46–47 atom%), (v) ~0.5% in the paramagnetic γ-Fe(Ni, Co) phase (~29–33 atom% of Ni), (vi) ~3% in schreibersite, and (vii) ~2% in rhabdite.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 6","pages":"1421-1432"},"PeriodicalIF":2.2,"publicationDate":"2025-05-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144292734","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":"2025 Nier Prize for Nicole Xike Nie","authors":"Nicolas Dauphas","doi":"10.1111/maps.14365","DOIUrl":"https://doi.org/10.1111/maps.14365","url":null,"abstract":"","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 6","pages":"E11-E12"},"PeriodicalIF":2.2,"publicationDate":"2025-05-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144292729","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.14203","DOIUrl":"https://doi.org/10.1111/maps.14203","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 5","pages":"i"},"PeriodicalIF":2.2,"publicationDate":"2025-05-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14203","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930211","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":"Textural coarsening as the cause for impact-melt like plagioclase crystal size distributions and subtle layering in high-Al basalt 14053","authors":"Stu Webb,&nbsp;Clive R. Neal,&nbsp;Bridget Guiza,&nbsp;James M. D. Day","doi":"10.1111/maps.14362","DOIUrl":"https://doi.org/10.1111/maps.14362","url":null,"abstract":"<p>High-Al Apollo 14 basalt 14053 has been identified as an endogenous partial melt product from the lunar interior based on geochemical analyses, specifically low abundances of highly siderophile elements, but exhibits textural characteristics similar to those of impact melts. Prior studies of this sample have described mineralogical differences between “interior” and “exterior” portions, which have been attributed to exposure at the lunar surface and subsequent metamorphism through subsolidus reheating within or in proximity to an impact-ejecta blanket. It has been demonstrated that quantitative textural analysis is a useful tool for distinguishing between lunar rocks altered by impact processes and those produced by endogenic magmatic processes. Such an approach is used in this study to analyze multiple thin sections cut from interior and exterior portions of 14053. The textural heterogeneity of plagioclase crystals among thin sections revealed in this study suggests that an impact-ejecta blanket likely impinged on the western side of 14053. This thermal metamorphism coarsened the plagioclase grains within that portion of 14053 so intensely that components diffused to form subtle layering and moderate textural heterogeneity that was quantifiable. These results also support previous conclusions that suggest the differences in reduction textures within this sample are due to the limited penetration depth of solar-wind implanted hydrogen prior to reheating. Thermal metamorphism can produce textural changes in lunar samples even if below the solidus temperature, such that the plagioclase texture of an endogenous basalt is sufficiently altered to that resembling an impact melt. These results highlight the significance of quantitative petrographic observations of lunar samples to reveal important petrogenetic information that has to be placed in proper spatial context to be understood.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 6","pages":"1411-1420"},"PeriodicalIF":2.2,"publicationDate":"2025-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14362","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144292420","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":"Multiple CV chondrite lithologies in Camel Donga 003 (CK3): Implications for the CV and CK parent bodies","authors":"Elana G. Alevy,&nbsp;Tasha L. Dunn,&nbsp;Alexander N. Krot,&nbsp;Paul Cardon-Pilotaz,&nbsp;Juliane Gross","doi":"10.1111/maps.14358","DOIUrl":"https://doi.org/10.1111/maps.14358","url":null,"abstract":"<p>Camel Donga 003 (CD 003) was originally classified as a CK3 chondrite based on its coarse-grained matrix, Ni-rich sulfides, Cr-rich magnetite, and CK-like silicate mineralogy. However, after preliminary backscattered electron imaging and elemental mapping of a 400 mm² thin section of CD 003, subsequent mineral chemistry analysis confirmed that the sample is a fragmental breccia consisting of three oxidized CV lithologies. In the two largest lithologies, both mineralogically pristine and metasomatically altered refractory inclusions are commonly found in close proximity to one another. This suggests that brecciation and mixing of different lithologies in CD 003 occurred on a submillimeter scale. The least abundant lithology—an 8 × 3 mm clast—is distinguished from the other lithologies by its recrystallized matrix, poorly defined chondrules, and equilibrated olivine (Fa₄₂). The homogeneity of matrix and chondrule olivine indicates that this lithology has been metamorphosed to at least petrologic subtype 3.8 conditions. We can trace the provenance of our sample to the main mass of CD 003, which must contain the CK material described in its original classification. Therefore, the presence of the three oxidized CV lithologies suggests that CD 003 is the first CV/CK3 chondrite breccia.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 6","pages":"1336-1364"},"PeriodicalIF":2.2,"publicationDate":"2025-05-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144291923","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":"A complete inventory of institutional and public meteorite collections in Switzerland","authors":"J. Eschrig,&nbsp;M. M. M. Meier,&nbsp;B. A. Hofmann","doi":"10.1111/maps.14361","DOIUrl":"https://doi.org/10.1111/maps.14361","url":null,"abstract":"<p>Museums and universities are important for collecting, maintaining, and curating meteorites. To make specimens known and available for research, inventorying and optimal curation are important. However, not all meteorite collections are well curated, especially in smaller institutions. During a 12-month project supported by the Swiss Confederacy under the “SwissCollNet” framework, we viewed, photographed, and inventoried all public and institutional meteorite collections in Switzerland. In total, the 27 collections contain 7616 specimens, derived from 3469 different meteorites. New, switched, and missing specimens were found in many collections. More than half of the collections contained specimens without inventory numbers and unknown or unofficial specimens, several of which could be assigned to a known meteorite fall or find during this project. The identification of switched or unknown samples was done using handheld X-ray fluorescence spectrometry and magnetic susceptibility measurements. In total, 201 specimens were attributed a preliminary classification. We demonstrate the importance of smaller collections, which often hold fragments of rare meteorite types. We underline how large-scale projects like the one presented here allow for unique data, for example, finding specimens missing from one collection in another. By tracking the origin of specimens using historic labels, we show that the history of meteoritics is reflected in the composition of the Swiss collections. During the inventorying process, several prehistoric and modern artifacts made of meteoritic material were found, underlining the potential of analyzing non-geological specimens in museums.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 6","pages":"1384-1410"},"PeriodicalIF":2.2,"publicationDate":"2025-05-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14361","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144291924","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":"Correction to “Corundum ± Magnesium-Deltalumite ± Hibonite-Bearing Objects in the CH Chondrite Sayh Al Uhaymir 290”","authors":"","doi":"10.1111/maps.14364","DOIUrl":"https://doi.org/10.1111/maps.14364","url":null,"abstract":"<p>Ryazantsev, K.M., Krot, A.N., Ma, C., Ivanova, M.A., Lorenz, C.A. and Shcherbakov, V.D. (2024), Corundum ± magnesium-deltalumite ± hibonite-bearing Objects in the CH Chondrite Sayh al Uhaymir 290. <i>Meteorit Planet Sci</i>, 59: 2608–2621. https://doi.org/10.1111/maps.14238</p><p>Figures 5 and 6 were reversed. The order of the captions was correct.</p><p>We apologize for this error.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 6","pages":""},"PeriodicalIF":2.2,"publicationDate":"2025-05-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14364","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144291789","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":"Bulk major and trace element abundances of barred olivine chondrules: Evidence about the physicochemical conditions in their region of nebular formation","authors":"M. E. Varela,&nbsp;J. Roszjar,&nbsp;P. Sylvester,&nbsp;L. Garcia","doi":"10.1111/maps.14360","DOIUrl":"https://doi.org/10.1111/maps.14360","url":null,"abstract":"<p>Barred olivine (BO) chondrules are present in ordinary and carbonaceous chondrites. We focus on the bulk major and trace element abundance composition of BO chondrules from carbonaceous, unequilibrated ordinary, and Rumuruti chondrites. Their bulk Fe/(FeO + MgO) wt% content versus the FeO wt% in olivine was used to divide these objects into FeO-poor and FeO-rich BO chondrules. The trace element content of bulk BO chondrules reveals the absence of fractionation among the abundances of elements having different geochemical behavior (e.g. Yb and [La-Ce]). This points to the predominance of a cosmochemical (e.g. gas/liquid or gas/solid condensation) instead of a geochemical process determining their elemental abundances. In addition, their bulk trace element content provides evidence for the physicochemical conditions that prevailed in the solar nebula during their formation. In general, such nebular regions are governed by local redox variations coupled with overall falling temperatures. The bulk chemical composition of the studied BO objects (e.g., Mg/Si bulk) suggests a time scale in which FeO-poor BO chondrules formed first in a chondrule-forming region rich in refractory trace elements. The progressive removal of refractory phases (e.g., hibonite, fassaite, melilite) led to a nebular reservoir depleted in the very refractory elements (e.g., Zr and Y) in which the rare earth elements (REEs) tend to reach equilibrium with the chondritic reservoir. From such a reservoir, the FeO-rich BO chondrules could have formed and were subsequently processed by metasomatic exchange reactions that equilibrated their moderately volatile V and Cr around chondritic values. The observed chemical variations are only possible if the studied BO chondrules behave as open systems exchanging elements with the cooling vapor. The inferred local redox variations coupled with overall falling temperatures could have taken place during the evolution of a single heterogeneous nebular reservoir in which Fe-poor and FeO-rich BO chondrules formed.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 6","pages":"1365-1383"},"PeriodicalIF":2.2,"publicationDate":"2025-04-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144292757","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":"Petrogenesis of the Rantila meteorite fall and implications for the origin of aubrites","authors":"Yash Srivastava,&nbsp;Amit Basu Sarbadhikari,&nbsp;Varsha M. Nair,&nbsp;Avadh Kumar,&nbsp;Yogita Kadlag,&nbsp;Ramakant R. Mahajan,&nbsp;Neeraj Srivastava,&nbsp;Neha Panwar,&nbsp;Aditya Das,&nbsp;Ryoji Tanaka,&nbsp;James M. D. Day,&nbsp;Anil D. Shukla,&nbsp;Dwijesh Ray,&nbsp;Abhishek J. Verma,&nbsp;Alka Rani,&nbsp;Garima Arora,&nbsp;Dipak K. Panda,&nbsp;S. Vijayan,&nbsp;Anil Bhardwaj","doi":"10.1111/maps.14357","DOIUrl":"https://doi.org/10.1111/maps.14357","url":null,"abstract":"<p>Aubrites are rare meteorites from highly reduced differentiated parent bodies. The Rantila meteorite was recovered soon after falling on 17 August 2022 at Rantila and Ravel villages in Gujarat state, India. We report the petrography, mineralogy, chemical composition, oxygen- and chromium-isotope compositions, along with reflectance spectroscopy, all showing that Rantila is an aubrite. Coarse enstatite and diopside grains constitute the main mass of Rantila, while mm-wide fracture domains pervade the coarse enstatites. In the fractures, comminuted enstatite, diopside blebs, olivine, a plagioclase–silica assemblage, sulfides, and metals occur. Rantila consists of enstatite (&gt;85 vol%), diopside (~8 vol%), forsterite, albite, and silica along with various sulfides and Fe-Ni alloys. The concentration of rare earth elements is ~1–2 × CI, consistent with main group aubrites. Noble gas and nitrogen isotopic analyses reveal young exposure ages (13.81 ± 6.47 Ma), a heterogeneous nitrogen isotopic composition, and a major K-Ar resetting event around 3.2 ± 0.4 Ga in the parent body of Rantila. The bulk oxygen isotope values are within the range of aubrites. The chromium isotopic values of Rantila are consistent with main group aubrites. The mineral assemblages, texture, and crystallization modeling suggest that Rantila had an igneous origin. The mineral assemblages in fractures indicate the involvement of external melt possibly during an impact-fracturing event, which aligns well with the heterogeneous N isotopic composition. Additionally, Rantila shows a wider range of oxygen isotopes than other aubrites suggesting some extent of O isotopic heterogeneity, likely stemming from exogenous processes. The variation in intra-sample bulk O and N isotope values implies inherent heterogeneity within the main group aubrites, potentially caused by late-stage impact contamination.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 6","pages":"1318-1335"},"PeriodicalIF":2.2,"publicationDate":"2025-04-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144292731","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}