Meteoritics & Planetary Science最新文献

{"title":"New high-pressure Fe-Ti oxide minerals in the Shergotty Martian meteorite: Feiite, Fe2+2(Fe2+Ti4+)O5, liuite, FeTiO3, and tschaunerite, (Fe2+)(Fe2+Ti4+)O4","authors":"Chi Ma,&nbsp;Oliver Tschauner,&nbsp;John R. Beckett,&nbsp;Vitali B. Prakapenka","doi":"10.1111/maps.14302","DOIUrl":"https://doi.org/10.1111/maps.14302","url":null,"abstract":"<p>High-pressure oxides like perovskite-type FeTiO₃, CaTi₂O₄-type Fe₂TiO₄, and ferrous-ferric oxides that form polysomes between wüstite and CaFe₂O₄-type Fe₃O₄ are potential carriers of Fe, Ti, and other transition metals in the mantle and may play an important role in the redox budget of the deep Earth. Here, we report the occurrence of three of these phases as the new minerals: feiite (Sr₂Tl₂O₅-type Fe²⁺₂(Fe²⁺Ti⁴⁺)O₅), liuite (FeTiO₃ with a GdFeO₃-type perovskite structure), and tschaunerite (CaTi₂O₄-type (Fe²⁺)(Fe²⁺Ti⁴⁺)O₄), along with wangdaodeite (LiNbO₃-type FeTiO₃) in a transformed ulvöspinel clast entrained in a shock melt pocket in the Shergotty Martian meteorite. We show that reaction between the shocked ulvöspinel precursor and melt occurred at pressures between 20 and 25 GPa. The high-pressure Fe-, Ti-minerals lost Fe and O to the surrounding shock melt in exchange for Si, Mg, and Ca. Concentrations of Si and Mg in all of these clast phases and of Na in liuite are significant. They substantiate chemical interaction of the clast with melt during the shock event and highlight potential elemental distributions in complex Fe- and Ti-rich lithologies at pressures of the deep transition zone to shallow lower mantle.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 3","pages":"375-391"},"PeriodicalIF":2.2,"publicationDate":"2024-12-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143633125","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":"Methylene-to-methyl ratio variability in Ryugu samples: Clues to a heterogeneous aqueous alteration","authors":"Zélia Dionnet,&nbsp;Zahia Djouadi,&nbsp;Lukas Delaye,&nbsp;Lucas Caron,&nbsp;Rosario Brunetto,&nbsp;Alice Aléon-Toppani,&nbsp;Cateline Lantz,&nbsp;Stefano Rubino,&nbsp;Donia Baklouti,&nbsp;Tomoki Nakamura,&nbsp;Ferenc Borondics,&nbsp;Christophe Sandt,&nbsp;Megumi Matsumoto,&nbsp;Kana Amano,&nbsp;Tomoyo Morita,&nbsp;Hisayoshi Yurimoto,&nbsp;Takaaki Noguchi,&nbsp;Ryuji Okazaki,&nbsp;Hikaru Yabuta,&nbsp;Hiroshi Naraoka,&nbsp;Kanako Sakamoto,&nbsp;Shogo Tachibana,&nbsp;Toru Yada,&nbsp;Masahiro Nishimura,&nbsp;Aiko Nakato,&nbsp;Akiko Miyazaki,&nbsp;Kasumi Yogata,&nbsp;Masanao Abe,&nbsp;Tatsuaki Okada,&nbsp;Tomohiro Usui,&nbsp;Makoto Yoshikawa,&nbsp;Takanao Saiki,&nbsp;Satoshi Tanaka,&nbsp;Fuyuto Terui,&nbsp;Satoru Nakazawa,&nbsp;Seiichiro Watanabe,&nbsp;Yuichi Tsuda,&nbsp;the Hayabusa2-initial-analysis Stone team","doi":"10.1111/maps.14304","DOIUrl":"https://doi.org/10.1111/maps.14304","url":null,"abstract":"<p>Understanding the processes of aqueous alteration within primitive bodies is crucial for unraveling the complex history of early planetesimals. To better identify the signs of this process and its consequences, we have studied the heterogeneity at a micrometric scale of the structure of the aliphatic organic compounds and its relationship to its mineralogical environment. Here, we report an analysis performed on two micrometric grains of Ryugu (C0002-FC027 and C0002-FC028). The samples were crushed in a diamond compression cell and analyzed using high-spatial resolution Fourier Transform InfraRed (FT-IR) hyperspectral imaging measurements conducted in transmission mode. We showed here the spatial distributions of the main components and the structural heterogeneity of the aliphatic organic matter highlighting a micrometer-scale variability in the methylene-to-methyl ratio. Moreover, we connected this heterogeneity to the one of the phyllosilicate band positions. Our findings indicate that the organic matter within Ryugu's micrometric grains underwent varying degrees of aqueous alteration in distinct microenvironments resulting in an elongation of the length of their aliphatic chains, and/or a reduction in their branching and/or cross-linking.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"273-285"},"PeriodicalIF":2.2,"publicationDate":"2024-12-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143424253","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":"Cafeosite, Ca4Fe2+3Fe3+2□O6S4, a new meteoritic oxysulfide, a redox indicator of metamorphic alteration of carbonaceous asteroids","authors":"Marina A. Ivanova,&nbsp;Sergey N. Britvin,&nbsp;Roza I. Gulyaeva,&nbsp;Sofia A. Petrova,&nbsp;Nina G. Zinovieva,&nbsp;Vladimir V. Kozlov,&nbsp;Stanislav N. Tyushnyakov,&nbsp;Anatoly V. Kasatkin","doi":"10.1111/maps.14296","DOIUrl":"https://doi.org/10.1111/maps.14296","url":null,"abstract":"&lt;p&gt;A natural iron-bearing oxysulfide, named сafeosite after its chemical composition, is a unique example of a mineral that simultaneously contains iron in three oxidation states: Fe&lt;sup&gt;3+&lt;/sup&gt;, Fe&lt;sup&gt;2+&lt;/sup&gt;, and intermediate between Fe&lt;sup&gt;2+&lt;/sup&gt; and Fe&lt;sup&gt;0&lt;/sup&gt; involved in metallic-type Fe&lt;span&gt;&lt;/span&gt;Fe bonding. Cafeosite was discovered in metamorphosed carbonaceous chondrite Dhofar 225, which is classified as CM-anomalous but likely related to the CY (Yamato-type) group. The mineral occurs as tiny anhedral grains that coalesce into irregular aggregates up to 20 μm, commonly encrusted by micrometer-thick troilite or pyrrhotite rims. The grains are randomly disseminated within a chondrite matrix composed of thermally altered phyllosilicates. Associated accessory minerals are troilite, pyrrhotite, Fe-rich, Al-bearing olivine, unknown Al-bearing Fe sulfide, Al-rich chromite, kamacite, awaruite, pentlandite, escolaite, and perovskite. In reflected light, cafeosite is gray, with no internal reflections. Anisotropy is moderate, bireflectance in gray hues. Infrared microspectroscopy did not reveal any bands attributable to (OH)&lt;sup&gt;−&lt;/sup&gt;, H&lt;sub&gt;2&lt;/sub&gt;O or CO&lt;sub&gt;3&lt;/sub&gt;&lt;sup&gt;2−&lt;/sup&gt; vibrations. Owing to the small grain size, the crystal structure of the mineral has been studied using synthetic analog, which was found to be isostructural with natural cafeosite based on electron backscatter diffraction (EBSD) data. Cafeosite is orthorhombic, space group &lt;i&gt;Cmce&lt;/i&gt; (#64), &lt;i&gt;a&lt;/i&gt; 17.4856(9), &lt;i&gt;b&lt;/i&gt; 11.1516(5), &lt;i&gt;c&lt;/i&gt; 11.1543(5) Å, &lt;i&gt;V&lt;/i&gt; 2175.0(2) Å&lt;sup&gt;3&lt;/sup&gt;, &lt;i&gt;Z&lt;/i&gt; = 8, &lt;i&gt;D&lt;/i&gt;&lt;sub&gt;x&lt;/sub&gt; = 4.11 g cm&lt;sup&gt;−3&lt;/sup&gt;. The crystal structure has been solved and refined to &lt;i&gt;R&lt;/i&gt;&lt;sub&gt;1&lt;/sub&gt; = 0.039 for 1105 unique reflections. Chemical composition of both natural and synthetic cafeosite corresponds to the formula Ca&lt;sub&gt;4&lt;/sub&gt;Fe&lt;sup&gt;2+&lt;/sup&gt;&lt;sub&gt;3&lt;/sub&gt;Fe&lt;sup&gt;3+&lt;/sup&gt;&lt;sub&gt;2&lt;/sub&gt;(□&lt;sub&gt;1−x&lt;/sub&gt;Fe&lt;sub&gt;x&lt;/sub&gt;)O&lt;sub&gt;6&lt;/sub&gt;S&lt;sub&gt;4&lt;/sub&gt; where (□&lt;sub&gt;1−&lt;i&gt;x&lt;/i&gt;&lt;/sub&gt;Fe&lt;sub&gt;&lt;i&gt;x&lt;/i&gt;&lt;/sub&gt;) denotes structural vacancy partially occupied by semimetallic-type Fe (&lt;i&gt;x&lt;/i&gt; = 0.2–0.3). The ideal endmember formula of the mineral is Ca&lt;sub&gt;4&lt;/sub&gt;Fe&lt;sup&gt;2+&lt;/sup&gt;&lt;sub&gt;3&lt;/sub&gt;Fe&lt;sup&gt;3+&lt;/sup&gt;&lt;sub&gt;2&lt;/sub&gt;□O&lt;sub&gt;6&lt;/sub&gt;S&lt;sub&gt;4&lt;/sub&gt;. Cafeosite was likely formed from previously altered precursor material of Dhofar 225, which, like common CM chondrites, consisted of phyllosilicates, Ca-bearing carbonates, tochilinite-like sulfides–hydroxides and pyrrhotite. During thermal metamorphism at temperatures between 750 and 900°C, sulfides–hydroxides were partly sintered with calcined carbonates and iron oxides, resulting in cafeosite formation. Due to varying and redox-dependent contents of Fe&lt;sup&gt;3+&lt;/sup&gt; and Fe&lt;sup&gt;2+&lt;/sup&gt;, as well as the presence of metallic-type Fe in the structure, cafeosite could be regarded as a single-phase redox indicator alternative to the known triple-phase buffers, for example, iron–magnetite–pyrrhotite (IM-Po), iron–wüsti","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"175-189"},"PeriodicalIF":2.2,"publicationDate":"2024-12-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143424254","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":"2021 Service Award for Christian Koeberl","authors":"Janice L. Bishop,&nbsp;Peter A. J. Englert","doi":"10.1111/maps.14294","DOIUrl":"https://doi.org/10.1111/maps.14294","url":null,"abstract":"","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"E1-E3"},"PeriodicalIF":2.2,"publicationDate":"2024-12-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143424198","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":"Petrofabrics in the CM chondrite Kolang: Evidence for non-spherical chondrules in the protoplanetary disk","authors":"Laura E. Jenkins,&nbsp;Martin R. Lee,&nbsp;Luke Daly,&nbsp;Ashley J. King,&nbsp;Cameron J. Floyd,&nbsp;Peter Chung,&nbsp;Sammy Griffin","doi":"10.1111/maps.14297","DOIUrl":"https://doi.org/10.1111/maps.14297","url":null,"abstract":"<p>The alignment of non-spherical “flattened” chondrules into a petrofabric is a common feature of hydrated carbonaceous chondrite meteorites. This texture can form as a result of impacts at peak shock pressures exceeding 10 GPa. However, many carbonaceous chondrites with petrofabrics are unshocked. While several processes have been proposed to explain this incongruency, including erasure of shock effects by alteration (both aqueous and thermal), none have yet been confirmed. Kolang is a brecciated Mighei-like carbonaceous chondrite wherein analysis of chondrule shape and orientation shows that it has a pronounced petrofabric defined by elongate chondrules that is shared between clasts with differing aqueous and thermal alteration histories. Its petrofabric, therefore, must have developed after the altered clasts had been juxtaposed; any sign of shock associated with impact-driven deformation cannot have been erased. We have investigated the shock experienced by Kolang with a combination of traditional optical methods and electron backscatter diffraction. We find that the peak shock pressure experienced by Kolang was likely ~4–5 GPa, too low to generate an impact-induced petrofabric. Kolang has not experienced sufficient shock, whether by a single or multiple impacts, to deform its chondrules from spheres into elongate chondrules. The most likely explanation, therefore, is that Kolang accreted elongate chondrules that were aligned under relatively low pressure.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"190-205"},"PeriodicalIF":2.2,"publicationDate":"2024-12-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14297","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143424223","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":"Multistage aqueous alteration in CeC 022 and other nakhlites","authors":"L. Krämer Ruggiu,&nbsp;B. Devouard,&nbsp;J. Gattacceca,&nbsp;L. Bonal,&nbsp;L. Piani,&nbsp;H. Leroux,&nbsp;O. Grauby","doi":"10.1111/maps.14295","DOIUrl":"https://doi.org/10.1111/maps.14295","url":null,"abstract":"<p>We studied Caleta el Cobre 022, a nakhlite showing a high abundance of aqueous alteration products, commonly called “iddingsite” and compared it to eight other nakhlites, in order to constrain the composition and the history of the aqueous alteration of nakhlites. Olivine grains in nakhlites display planes of secondary fluid inclusions, composed of pyroxene, magnetite, and a void potentially filled by a fluid. They were formed by a first fluid alteration event, previous to the iddingsite alteration event, probably from a late magmatic fluid circulation. We observed magnetite–pyroxene symplectites in olivine grains in most nakhlites, related to the same fluid-assisted tardi-magmatic event as the crystallization of the secondary inclusion planes. Those secondary inclusions and symplectites can be observed at the center of iddingsite veins, inside the most altered nakhlites, and are thus interpreted as being weakness planes, easing the circulation of the fluid forming the iddingsite inside the olivine grains. In every nakhlite, the alteration veins show at least two types of iddingsite: a coarse iddingsite with crystals around 50 nm, up to 200 nm, and a fine iddingsite with a nanocrystalline to amorphous texture with crystalline domains &lt;10 nm. Both iddingsite types are composed mainly of Si, Mg, and Fe, with anticorrelated Si and Fe contents. The coarse iddingsite is composed of a mixture of phyllosilicates, with Fe-oxyhydroxides and minor siderite, and the fine iddingsite has a composition close to saponite. Organic matter located in coarse iddingsite is detected by Raman spectroscopy in the iddingsite of many nakhlites and was confirmed by the TEM study of NWA 10153. In addition, the TEM study of NWA 10153 displays complex chemical zoning in the fine iddingsite of Mg, Ca, Mn, S, P, and Al, suggesting at least two stages of circulations. Both the compositions and textures of the two types of iddingsite are suggestive of a progressive evolution of the alteration fluid, enriched in elements from basaltic mineral dissolution, with crystallization mainly by filling of existing fractures, and selective dissolution of host olivine. We also observe pyrrhotite–magnetite veinlets at the center of iddingsite veins and cross-cutting iddingsite veins and silicates, which are interpreted as the result of another later fluid circulation.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"151-174"},"PeriodicalIF":2.2,"publicationDate":"2024-12-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143424134","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":"“Ground truth” occurrence of Pink Spinel Anorthosite (PSA) as clasts in lunar meteorite Northwest Africa (NWA) 15500: Chemical evidence for a genetic relationship with lunar highlands Mg-suite and formation by magma–wallrock interactions","authors":"Daniel Sheikh,&nbsp;Alex M. Ruzicka,&nbsp;Melinda L. Hutson","doi":"10.1111/maps.14298","DOIUrl":"https://doi.org/10.1111/maps.14298","url":null,"abstract":"<p>Pink spinel anorthosite (PSA), a distinctive plagioclase and spinel-rich lithology (spinel &gt;20%) observed on the lunar surface by the Moon Mineralogy Mapper (M³) imaging spectrometer, has sparked considerable interest in understanding magmatic processes on the Moon that cannot be explained by the well-established lunar magma ocean paradigm. Competing ideas on the PSA-forming mechanisms have invoked either (1) impact melting of troctolitic source rocks on the lunar surface or (2) magma–wallrock interactions between anorthositic crust and Mg-suite parental melts, but have been difficult to evaluate given the lack of ground truth samples. Here, we investigate the textures and mineral compositions of seven PSA clasts in lunar meteorite Northwest Africa (NWA) 15500, and the bulk trace element compositions of a PSA clast separate and NWA 15500 host lithologies A and B. Our findings suggest derivation of PSA from an incompatible-element-poor source and are consistent with PSA representing an Mg-suite lithology genetically related to pink spinel troctolites that reflects increased degrees of crustal assimilation during magma–wallrock interactions, and a sourcing of PSA far from the Procellarum KREEP Terrane. Excavation of PSA material was followed by multiple, subsequent localized impact events, resulting in the formation of Lithologies A and B.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 2","pages":"206-224"},"PeriodicalIF":2.2,"publicationDate":"2024-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143423869","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":"The MetBase database has been merged into Astromat","authors":"Dominik C. Hezel,&nbsp;Kerstin A. Lehnert,&nbsp;Premkumar Elangovan,&nbsp;Peng Ji,&nbsp;Jennifer Mays,&nbsp;Jörn Koblitz","doi":"10.1111/maps.14293","DOIUrl":"https://doi.org/10.1111/maps.14293","url":null,"abstract":"<p>MetBase has been the world's largest database for meteorite compositions, but has now passed this torch on to the Astromaterials Data System (Astromat), into which MetBase has recently been merged. This merger had been planned for some time and took almost 1 year to complete. Not only differences in the structure of the databases, in the content and organization of data and metadata, and in the terminology used but also incorporation of new data needed to be resolved to combine the data holdings of MetBase with the Astromat synthesis database. Astromat is NASA's primary archive for laboratory analyses of astromaterial samples and funded by NASA to provide services for the preservation and open access of data from astromaterials, including meteorites, in alignment with the FAIR principles. After merging MetBase into Astromat's synthesis database, this now provides the cosmochemical community the largest compilation of cosmochemical analytical data by far: over 2 million analytical data points. Astromat is also part of a bigger ecosystem of geo- and cosmochemcial databases, as its foundation is aligned with other large geochemical databases such as EarthChem and GEOROC. The visualization tools and the teaching tool from MetBase will be further developed and now exist as independent tools. We provide a brief history of the two databases and their journeys, an outlook toward the future, as well as lessons learned from this merger. We recommend that other cosmochemical databases try whenever possible to adopt the Astromat database schema as early as possible, or get in contact for alternative options. We believe MetBase now being a part of Astromat is a match made in heaven and hope Astromat will become a reliable and trusted service within the community.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 1","pages":"143-148"},"PeriodicalIF":2.2,"publicationDate":"2024-12-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14293","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143116099","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":"Cover","authors":"","doi":"10.1111/maps.14024","DOIUrl":"https://doi.org/10.1111/maps.14024","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":"59 12","pages":"i"},"PeriodicalIF":2.2,"publicationDate":"2024-12-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14024","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142851478","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":"Shanghai Astronomy Museum and its meteorite collections","authors":"Du Zhimao,&nbsp;Li Shaolin,&nbsp;Shan Xingmei,&nbsp;Lin Qing","doi":"10.1111/maps.14291","DOIUrl":"https://doi.org/10.1111/maps.14291","url":null,"abstract":"<p>The Shanghai Astronomy Museum (SAM) has opened its meteorite collections to the planetary science community. Inaugurated in July 2021, SAM is recognized as the world's largest astronomical museum and currently houses a collection of 97 meteorites weighing a total of 469 kg. These meteorites come from over 40 nations and encompass a diverse array of 37 different groups. Among them, 70 meteorites are displayed in the museum. The museum also features a series of interactive exhibition areas showcasing the internal structure of meteorites, engaging games introducing meteorite identification, and simulating the formation process of asteroid impact craters. This comprehensive range of offerings enables public access to extensive scientific knowledge about meteorites, making the museum a pivotal platform for disseminating meteoritics to the public.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 1","pages":"133-142"},"PeriodicalIF":2.2,"publicationDate":"2024-12-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143112240","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}