Meteoritics & Planetary Science最新文献

{"title":"Microtextures and structures in metal–sulfide grains in NWA 869 meteorite and their relation to thermal history of L-chondrite parent body","authors":"Paulina Skirak,&nbsp;Gabriela Opiła,&nbsp;Adam Piestrzyński,&nbsp;Gabriela Kozub-Budzyń,&nbsp;Czesław Kapusta","doi":"10.1111/maps.14318","DOIUrl":"https://doi.org/10.1111/maps.14318","url":null,"abstract":"<p>Results of microanalysis study of NWA 869 meteorite, an ordinary chondrite, where silicates, Fe-Ni alloys, and troilite are major constituents, are reported. The presented study of microtextures in metallic and sulfide grains provides information on processes occurring from the asteroid's accretion, through the impacts until cooling. The presence of metal–silicate emulsion, swiss-cheese texture, and polycrystalline kamacite–troilite aggregates observed indicates very rapid increase in temperature due to impact. Fizzed troilite, slightly homogenized taenite domains, and intergrowth of native copper in plessite imply rapid cooling in isolated regions in space. Agrell effect on the interface of kamacite–taenite grains and non-corroded tetrataenite rims indicates that the sample contains rock fragments from a region unaffected directly by the impact or rapid heating. Diversity of petrological types, lithic clasts with shock grade higher than S3, shock-darkened clasts or impact melting rocks, and variation of microtextures suggest that the parent body of L-type chondrites after accretion, radiogenic metamorphism, and consequent formation of the onion–shell model broke up into debris after the impact of eucrite body.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"616-631"},"PeriodicalIF":2.2,"publicationDate":"2025-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14318","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143632876","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 and compositional characteristics of metallic spherules in impact melt from Monturaqui crater, Chile","authors":"Daniel O. Cukierski,&nbsp;David W. Peate,&nbsp;Ingrid A. Ukstins,&nbsp;Christy Kloberdanz,&nbsp;C. Tom Foster,&nbsp;Chungwan Lim","doi":"10.1111/maps.14322","DOIUrl":"https://doi.org/10.1111/maps.14322","url":null,"abstract":"<p>Samples of impactite from the small (~350 m diameter) Monturaqui crater in northern Chile contain Fe-Ni metallic spherules sourced from the iron meteorite impactor. Textural characterization and quantification were done using SEM and μCT data. Two textural types are distinguished, with different size distributions. The smaller spherical objects (mostly &lt;100 μm in diameter) follow a power law size distribution, while larger objects are mostly irregular-shaped patches. These are analogous to the small (nm to 50 μm) immiscible spherical metal droplets and large (150–500 μm) irregular partly fused pieces of the iron meteorite projectile observed in highly shocked ejecta fragments during hypervelocity impact experiments. Compositions of both spherule types were determined using in situ methods (electron microprobe, LA-ICP-MS), as well as solution ICP-MS on individual spherules separated from impact melt glass using electric pulse disintegration. Spherules are enriched in Ni and Co relative to Fe and W and relative to the inferred iron meteorite impactor composition, and PGEs show similar enrichments with limited fractionation between different PGEs, all consistent with selective oxidation processes. All spherules have similar chondrite-normalized patterns that are also broadly similar to weathered fragments of the iron meteorite impactor. Ni-Ge and Ni-Ir data on large (&gt;300 μm) spherules and weathered meteorite fragments suggest that the Monturaqui impactor was a group IAB iron meteorite.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"646-662"},"PeriodicalIF":2.2,"publicationDate":"2025-02-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14322","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143632871","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":"A primitive asteroid that lived fast and died young sampled by a xenolith in the Cold Bokkeveld CM2 carbonaceous chondrite","authors":"Martin R. Lee,&nbsp;Cameron J. Floyd,&nbsp;Robin Haller,&nbsp;Sammy Griffin","doi":"10.1111/maps.14310","DOIUrl":"https://doi.org/10.1111/maps.14310","url":null,"abstract":"<p>Xenoliths in carbonaceous chondrites include lithologies that are unrepresented in the meteorite record and so are a rich source of information on asteroid diversity. Cold Bokkeveld is a CM2 regolith breccia that contains both hydrous and anhydrous lithic clasts. Here, we describe a hydrous clast with a fine-grained rim. This rim shows that the clast is a xenolith that interacted with dust in the protoplanetary disk between liberation from its protolith and incorporation into Cold Bokkeveld's parent body. Prior to its fragmentation, the xenolith's protolith had undergone brittle deformation, with the fractures produced being cemented by carbonates to make veins. After being incorporated into Cold Bokkeveld's parent body, the veined xenolith experienced a second phase of aqueous alteration leading to hydration of its fine-grained rim, replacement of carbonate by tochilinite–cronstedtite intergrowths, and formation of magnetite within its fine-grained matrix. The veined xenolith's protolith underwent its entire geological evolution (accretion–aqueous alteration–fracturing–fragmentation) before Cold Bokkeveld's parent body had accreted. Such a short lifespan may be explained by explosive breakup of the protolith due to overpressure from gases produced internally during water–rock interaction. Early fragmentation effectively acted as a thermostat to limit runaway heating that may have otherwise resulted from the body's high concentrations of ²⁶Al. Many other hydrous lithic clasts in CM carbonaceous chondrite meteorites could be the remains of such ephemeral early asteroids, but they are hard to identify without evidence that they were accreted as hydrous lithologies and contemporaneously with chondrules.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"464-483"},"PeriodicalIF":2.2,"publicationDate":"2025-02-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14310","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143632998","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":"Mid-infrared detection and characterization of refractory inclusions in CM and CO chondrites: A non-destructive approach for returned space samples","authors":"Jean Charlier,&nbsp;Alice Aléon-Toppani,&nbsp;Rosario Brunetto,&nbsp;Jérôme Aléon,&nbsp;Ferenc Borondics","doi":"10.1111/maps.14314","DOIUrl":"https://doi.org/10.1111/maps.14314","url":null,"abstract":"<p>Refractory inclusions (RIs) in chondrites are widely used as tracers of early solar system formation conditions. In the context of sample-return missions, a non-destructive and non-invasive analytical tool that can rapidly detect and characterize RIs in space samples during their early phase of study is highly needed. Here, we performed mid-infrared (MIR) fine-scale hyperspectral imaging over large fields of view to detect RIs in CM and CO chondrites. A database of MIR spectra of typical RIs minerals was built (1) to support future remote sensing observations in astronomical environments and (2) to develop a detection method based on machine-learning algorithms and spectral distance between sample and reference minerals. With this method, up to 96.5% of the RI content is detected in a meteorite section. Further comparison between scanning electron microscopy and spot analysis acquired in reflectance in the full MIR range shows that RIs can be classified following their mineralogy based on infrared (IR) properties. Finally, we show that the relative OH content of several RIs in CM chondrites determined from IR spectroscopy can be used to infer the extent of modification caused by aqueous alteration on the asteroidal parent body.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"544-569"},"PeriodicalIF":2.2,"publicationDate":"2025-02-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14314","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143632999","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":"The solar system Fe/Mg ratio","authors":"D. S. Burnett,&nbsp;A. J. G. Jurewicz,&nbsp;D. S. Woolum,&nbsp;Y. Guan,&nbsp;V. S. Heber,&nbsp;R. Hervig,&nbsp;M. Humayun,&nbsp;K. D. McKeegan,&nbsp;L. R. Nittler,&nbsp;C. T. Olinger,&nbsp;D. B. Reisenfeld,&nbsp;J. Wang","doi":"10.1111/maps.14313","DOIUrl":"https://doi.org/10.1111/maps.14313","url":null,"abstract":"<p>Solar wind Fe and Mg fluences (atoms/cm²) were measured from Genesis collectors. Fe and Mg have similar first ionization potentials and solar wind Fe/Mg should equal the solar ratio. Solar wind Fe/Mg is a more valid measure of solar composition than CI chondrites and can be measured more accurately than spectroscopic photospheric abundances. Mg and Fe fluences analyzed in four laboratories give satisfactory agreement. Si and diamond-like carbon collector fluences agree for both elements. The Mg and Fe fluences are 1.731 ± 0.073 × 10¹² and 1.366 ± 0.058 × 10¹² atoms/cm². All plausible sources of errors down to the 1% level are documented. Our value for the solar system Fe/Mg, 0.789 ± 0.048 agrees within 1 sigma errors with CI chondrites, spectroscopic photospheric abundances, and with the solar wind data from the ACE spacecraft. CI samples from asteroid Ryugu give Fe/Mg in agreement with Genesis and meteoritic CI samples despite very small sample sizes. The higher accuracy of the Genesis solar Fe/Mg permits a comparison with chondritic Fe/Mg at the 10% level. Intermeteorite Fe/Mg averages differ among the main C chondrite groups but are within, or very close to, the ±1 sigma Genesis solar Fe/Mg.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"529-543"},"PeriodicalIF":2.2,"publicationDate":"2025-01-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14313","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143633090","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":"Location of NWA 6148 and NWA 10153 in the nakhlite body and their aqueous alteration","authors":"Kakeru Kukihara,&nbsp;Masaaki Miyahara,&nbsp;Akira Yamaguchi,&nbsp;Yoshio Takahashi,&nbsp;Yasuo Takeichi,&nbsp;Naotaka Tomioka,&nbsp;Eiji Ohtani","doi":"10.1111/maps.14316","DOIUrl":"https://doi.org/10.1111/maps.14316","url":null,"abstract":"<p>The petrologic and mineralogical characteristics and alteration processes of the nakhlites NWA 6148 and NWA 10153 were studied. Both consist of augite, olivine, and mesostasis. Based on the characteristics of each volume fraction of the components and the chemical composition of olivine and pyroxene, NWA 6148 correspond to lava units crystallized at 1346–1391 Ma in the nakhlite body. The position of NWA 10153 in the nakhlite body is unclear. Iron oxides/hydroxides, barite, and calcite fill the fractures of NWA 6148, which are terrestrial weathering products. In NWA 10153, olivine grains are replaced by goethite, magnetite, saponite, amorphous silica, jarosite, and siderite. Although it is uncertain whether all of the alteration minerals were formed on the surface of Mars or on the surface of Earth, NWA 10153 records two different alteration environments: reducing, neutral to alkaline, and oxidizing and acidic. As in NWA 6148 and NWA 10153, the assemblage of alteration mineral species in other nakhlites is also heterogeneous even within the same lava unit. The nakhlite body was altered by the oxidizing acidic fluid after a <span></span><math>\u0000 <mrow>\u0000 <msubsup>\u0000 <mi>CO</mi>\u0000 <mn>3</mn>\u0000 <mrow>\u0000 <mn>2</mn>\u0000 <mo>−</mo>\u0000 </mrow>\u0000 </msubsup>\u0000 </mrow></math>-bearing reducing neutral to alkaline fluid. The drastic change of alteration environments may have been caused by an impact event.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"596-615"},"PeriodicalIF":2.2,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143633131","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":"VIS-to-MIR reflectance and Raman spectroscopy of the CM2 NWA 12184 carbonaceous chondrite","authors":"A. Galiano,&nbsp;F. Dirri,&nbsp;M. Ferrari,&nbsp;C. Carli,&nbsp;E. Bruschini,&nbsp;G. Filacchione,&nbsp;G. Piccioni,&nbsp;E. Palomba,&nbsp;S. Stefani,&nbsp;A. Raponi,&nbsp;M. Ciarniello,&nbsp;M. E. Palumbo,&nbsp;C. Scirè Scappuzzo,&nbsp;G. Baratta,&nbsp;R. G. Urso,&nbsp;L. Inno","doi":"10.1111/maps.14315","DOIUrl":"https://doi.org/10.1111/maps.14315","url":null,"abstract":"<p>The spectral analysis of CM meteorites can help to constrain the mineralogical composition of their parent body, the C-type asteroids. The CM2 NWA 12184 was spectrally examined employing seven complementary techniques at different spatial resolutions, including VIS-to-MIR reflectance and Raman spectroscopy. Furthermore, the effects of space weathering on asteroids can be investigated by performing laboratory simulations on meteorites samples; thus, the meteorite was processed with He⁺ ions at 200 keV (maximum fluence of 1.0 × 10¹⁷ ions cm⁻²) to simulate the solar wind irradiation on C-type asteroids. We discriminated the mineralogical composition of the NWA 12184 at the millimeter scale and at the micrometer scale, investigating both matrix and chondrules. The ion experiment produced spectral darkening, reddening, shifting of the hydration band, and weakening of the absorption band ascribed to olivine in the VIS-NIR range, as well as the reduction in the olivine's peak in MIR range, clue of the sample's amorphization. The study identified the native mineralogy of the meteorite, the products of terrestrial weathering, and the aqueous and thermal alteration experienced by the parent body of the sample.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"570-595"},"PeriodicalIF":2.2,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14315","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143633027","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":"Insights on the volcanic and impact histories of the lunar nearside from the petrology, geochemistry, and geochronology of the Calcalong Creek lunar regolith breccia meteorite","authors":"B. H. Oliveira,&nbsp;J. F. Snape,&nbsp;R. Tartèse,&nbsp;J. F. Pernet-Fisher,&nbsp;D. van Acken,&nbsp;M. J. Whitehouse,&nbsp;K. H. Joy","doi":"10.1111/maps.14305","DOIUrl":"https://doi.org/10.1111/maps.14305","url":null,"abstract":"<p>The Calcalong Creek lunar meteorite is a regolith breccia with a lithologically diverse array of clasts set in a glassy, highly vesicular matrix. Here, we present a comprehensive new analysis of the meteorite. Comparisons to remote sensing data, lunar sample lithologies, and lunar sample ages indicate that it was likely sourced from regolith surrounding the Moon's nearside Procellarum KREEP Terrane, as opposed to the farside South Pole-Aitken basin as has been previously suggested. Partial and complete reset dates of ~3.9 Ga suggest a disturbance at this time, which aligns with that of the Imbrium basin-forming event, and to a lesser degree we see evidence of a ~4.2 Ga impact, which may be related to the formation of the Serenitatis basin. Analysis of Calcalong Creek clasts, thus, provide insights not only on the timing of major impact basin formation but also on the volcanic history of the Moon. The meteorite also samples some ancient ~4.3 Ga evolved magmatism, manifested in the presence of granophyre clasts, which may have originated from a high-μ, KREEP-like source, as well as younger, ~3.7 Ga low-Ti basaltic magmatism.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"392-421"},"PeriodicalIF":2.2,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14305","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143633132","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":"The Meteoritical Society: Business from 2023 to 2024","authors":"Nancy L. Chabot,&nbsp;Jutta Zipfel,&nbsp;Tasha L. Dunn","doi":"10.1111/maps.14317","DOIUrl":"https://doi.org/10.1111/maps.14317","url":null,"abstract":"&lt;p&gt;The Meteoritical Society had an active and productive 2 years from 2023 to 2024. The society is very healthy, with membership the highest it has been in the last decade and with strong financial resources. Highlights included holding the annual meeting in 2023 in Los Angeles, United States, and in 2024 in Brussels, Belgium. Other notable activities included recognizing member achievements with society awards, supporting the society's publications, and enabling the work of the society's committees. All activities of the Meteoritical Society are possible due to the service of members. Here, we summarize the business of the Meteoritical Society from 2023 to 2024 and acknowledge many members and their contributions.&lt;/p&gt;&lt;p&gt;Council met roughly every 2 months to handle the business of the society, with five virtual 2-h meetings and one in-person meeting each year, with the in-person meeting held the Sunday prior to the annual meeting for roughly 5 h (Figure 1). Council was very active, with 43 votes in 2023 and 52 votes in 2024, as recorded in the minutes. Along with the posted minutes from each council meeting, a monthly newsletter was distributed to members via email by the President and the Secretary and posted and archived on the Meteoritical Society website.&lt;/p&gt;&lt;p&gt;At the end of 2023, the Meteoritical Society numbered 1083 members, and at the end of 2024, the society numbered 1198 members. In both years, members represented slightly over 50 different countries, with the breakdown of membership by continent being roughly: 46% North America; 35% Europe; 13% Asia; and about 2% for each of Africa, Australia, and South America. Total membership is the highest it has been within the last decade.&lt;/p&gt;&lt;p&gt;Table 1 provides the membership rates, which were the same for both 2023 and 2024, and the break down by membership category for each year. Early career members are defined as anyone within 10 years of completing their PhD or last degree. Low-income country memberships are for members residing in the countries on the Development Assistance Committee list of the Organisation for Economic Co-operation and Development who are eligible for Official Development Assistance.&lt;/p&gt;&lt;p&gt;From 2023 to 2024, the Society's finances continued to be on sound footing, with both the Operating Fund and Investment Fund in very healthy condition over the 2-year period. The Operating Fund supports the yearly activities of the society, which amounted to roughly ~$300,000 in revenue and expenses each year. The Investment Fund is currently distributed across six endowed funds, three of which support awards (the Nier Prize, the Gordon A. McKay Award, and the Elmar K. Jessberger Award). Two funds support member travel to annual meetings: The Travel for International Members (TIM) Fund supports travel for members from low-income countries, while the O. Richard Norton Fund supports travel for early career scientists. The largest fund is the General Endowment Fund, which supports a varie","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"680-696"},"PeriodicalIF":2.2,"publicationDate":"2025-01-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14317","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143633093","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":"Iron and copper sulfides in asteroid (162173) Ryugu: Formation conditions and a comparison to the CI and CY chondrites","authors":"C. S. Harrison,&nbsp;A. J. King,&nbsp;R. H. Jones,&nbsp;S. S. Russell,&nbsp;T. Nakamura,&nbsp;H. Yurimoto,&nbsp;T. Noguchi,&nbsp;R. Okazaki,&nbsp;H. Yabuta,&nbsp;H. Naraoka,&nbsp;K. Sakamoto,&nbsp;S. Tachibana,&nbsp;T. Yada,&nbsp;M. Nishimura,&nbsp;A. Nakato,&nbsp;A. Miyazaki,&nbsp;K. Yogata,&nbsp;M. Abe,&nbsp;T. Okada,&nbsp;T. Usui,&nbsp;M. Yoshikawa,&nbsp;T. Saiki,&nbsp;S. Tanaka,&nbsp;F. Terui,&nbsp;S. Nakazawa,&nbsp;S. Watanabe,&nbsp;Y. Tsuda","doi":"10.1111/maps.14312","DOIUrl":"https://doi.org/10.1111/maps.14312","url":null,"abstract":"<p>JAXA's Hayabusa2 sample return mission visited the volatile-rich carbonaceous (C-type) asteroid (162173) Ryugu with the aim of ground-truthing remote observations, returning a pristine sample from a C-type asteroid, and strengthening links between asteroids and the meteorite collection. Here, we have conducted a systematic study of coarse (&gt;10 μm) sulfide grains in Ryugu particles C0025-01 and C0103-02, the CI chondrites Orgueil and Ivuna, and the CY chondrites Y-86029 (Stage III, heated to 500–750°C) and Y-86720 (Stage IV, &gt;750°C), using scanning electron microscopy (SEM) and electron probe microanalysis (EPMA). Sulfides are sensitive tracers of secondary alteration conditions, and we find that Ryugu and the CI chondrites share a distinct sulfide assemblage that includes the iron sulfides pyrrhotite and pentlandite, and the copper sulfide cubanite, that equilibrated during periods of low temperature (~25°C) aqueous alteration. Sulfides in the CY chondrites are compositionally distinct from Ryugu and the CI chondrites as a result of post-hydration heating. However, the occurrence of Cu-rich sulfides in Ryugu, the CIs, and the CYs suggests a genetic relationship between these samples.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"506-528"},"PeriodicalIF":2.2,"publicationDate":"2025-01-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14312","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143632755","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}