Meteoritics & Planetary Science最新文献

{"title":"Cover","authors":"","doi":"10.1111/maps.14201","DOIUrl":"https://doi.org/10.1111/maps.14201","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 4","pages":"i"},"PeriodicalIF":2.2,"publicationDate":"2025-04-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14201","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143809624","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":"Metal–forsterite condensate nodules and H-L-LL compositions","authors":"Denton S. Ebel,&nbsp;Marina E. Gemma,&nbsp;Michael K. Weisberg,&nbsp;Jon M. Friedrich","doi":"10.1111/maps.14328","DOIUrl":"https://doi.org/10.1111/maps.14328","url":null,"abstract":"<p>Compared to the carbonaceous chondrites (CCs), ordinary chondrites (OCs) are depleted in Mg and refractory lithophile elements. The OCs are classified by a trend from high metal (H) to low total iron (L) to low total iron and low metal (LL) compositions with increasing heavy O isotopes and refractory siderophile enrichment. We surveyed many CC for primitive materials that might be analogs of components that formed in, and then escaped, originally solar composition reservoirs from which OCs formed. Amoeboid olivine aggregates (AOA) are nodular accretions with discrete refractory Ca-, Al-, Ti-rich mineral assemblages and often with separate Fe-metal alloy nodules, all surrounded by ¹⁶O-rich, near-pure olivine Mg₂SiO₄ rinds. Most AOAs contain the daughter products of extinct ²⁶Al revealing their very early ages. We find relatively large metal grains with olivine rims forming isolated or clumped nodules or “metal–olivine inclusions” in AOAs in many carbonaceous chondrites, particularly the highly primitive CO-like chondrite Acfer 094 (C2 ungr). Similar nodules have been reported in samples returned from the highly altered, CI-like asteroid Bennu by the OSIRIS-REx mission. In discrete regions and times in the protoplanetary disk, differing drift velocities of these 10s of micron scale components could have caused the correlated loss of both refractory siderophiles (in metal), refractory lithophiles, and Mg and ¹⁶O (in olivine). Varying degrees of loss of nodules similar to these “MOI,” from the chondrule-forming reservoirs from which H, L, and LL chondrites accreted could, simultaneously, explain the multiple aspects of their chemical compositions.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 4","pages":"757-777"},"PeriodicalIF":2.2,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143809700","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":"Near- and mid-infrared spectral diversity in the Aguas Zarcas carbonaceous chondrite and implications for inferring aqueous processes on primitive asteroids using remote sensing","authors":"Cody Schultz,&nbsp;Ralph E. Milliken,&nbsp;Joseph Boesenberg,&nbsp;Imene Kerraouch","doi":"10.1111/maps.14339","DOIUrl":"https://doi.org/10.1111/maps.14339","url":null,"abstract":"<p>CM carbonaceous chondrites are complex brecciated meteorites that exhibit significant chemical, mineralogic, and petrographic diversity both between and within individual samples. As most reflectance spectroscopy studies of carbonaceous chondrites are performed on bulk powders, important questions remain about the true spectral diversity of these complex breccias and the degree to which lab-based meteorite spectra can be reliably related to remotely acquired spectra of primitive asteroids. The Aguas Zarcas meteorite is a unique CM chondrite in that it has been found to exhibit at least five chemically and isotopically distinct lithologies that are all associated with a single fall event. Here, we describe a coordinated petrographic and spectroscopic study to further investigate the thermochemical and collisional history of the Aguas Zarcas parent body and to better understand how to interpret remotely acquired spectra of primitive asteroids. Four intact sections of the Aguas Zarcas meteorite, which together represent at least three to four distinct lithologies, were analyzed using microscope FT-IR (μFT-IR) spectroscopy and electron probe microanalysis (EPMA) elemental mapping. Our study found significant variations in spectral features, particularly in the mid-infrared (MIR) wavelength region, that can be linked to petrographic diversity between lithologies. The relative abundance of matrix phyllosilicates and pyroxene appears to have the strongest influence on the shape, position, and strength of MIR spectral features. Linear spectral unmixing models as a method for compositional interpretation showed varying accuracy when compared to EPMA-based estimates, with integrated μFT-IR spectral maps showing better results compared to unmixing of bulk (larger spot size) FT-IR spectra. A notable discovery in two sections of the Aguas Zarcas meteorite was the presence of carbonate veins along the boundary of chemically and petrographically separate lithologies, which provide important constraints on the nature and timing of pre- and post-brecciation aqueous alteration.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 4","pages":"876-915"},"PeriodicalIF":2.2,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143809699","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":"Type B–type C CAI in a CR chondrite: Evidence for multiple melting events, gas–melt interaction, and oxygen-isotope exchange","authors":"Kirsten Larsen,&nbsp;Alexander N. Krot,&nbsp;Daniel Wielandt,&nbsp;Kazuhide Nagashima,&nbsp;Guy Libourel,&nbsp;Martin Bizzarro","doi":"10.1111/maps.14325","DOIUrl":"https://doi.org/10.1111/maps.14325","url":null,"abstract":"<p>A coarse-grained igneous calcium-aluminum-rich inclusion (CAI) <i>N-53</i>, 4.3 × 5.9 mm in size, from the CR (Renazzo-type) carbonaceous chondrite Northwest Africa (NWA) 6043 is composed of two mineralogically, chemically, and isotopically distinct units—type B (<i>B</i>) and type C (<i>C</i>). Type <i>B</i> unit occurs in the CAI core and consists of melilite (Åk_28–56), AlTi-diopside, anorthite, spinel, and minor Fe,Ni-metal. Type <i>C</i> unit forms islands in <i>B</i> (<i>C</i>_c) and mantle (<i>C</i>_m) around it and consists of Na-bearing åkermanitic melilite (Åk_58–72, 0.18–0.86 wt% Na₂O), anorthite, AlTi-diopside (up to 1.2 wt% Cr₂O₃), spinel (up to 2.1 wt% Cr₂O₃), perovskite, and minor wollastonite. The outermost portion of <i>N-53</i> contains relict grains of olivine (Fa₄) and low-Ca pyroxene (Fs₄Wo₅); Wark–Lovering rim is absent. Magnesian spinel in <i>B</i> and <i>C</i> is ¹⁶O-rich (Δ¹⁷O ~ −23‰); Cr-bearing spinel in <i>C</i>_m is ¹⁶O-depleted (Δ¹⁷O ~ −11‰). AlTi-diopside, anorthite, and melilite in <i>B</i> and <i>C</i>_c are ¹⁶O-depleted to various degrees (Δ¹⁷O ~ −22‰ to −19‰, −21‰ to −17‰, −13‰ to −8‰, respectively). AlTi-diopside, anorthite, and melilite in <i>C</i>_m show a range of compositions correlated with a distance from the CAI edge (Δ¹⁷O ~ −18‰ to −8‰, −16‰ to −8‰, ~ −8‰ to −2‰). Melilite in <i>B</i> has the heaviest Mg-isotope composition (Δ²⁵Mg ~ 10‰); average Δ²⁵Mg of melilite, AlTi-diopside, and spinel in <i>C</i> are ~9, ~8‰, and ~6‰, respectively; anorthite in both units has Δ²⁵Mg of ~4‰. On the Al-Mg evolutionary diagram, melilite data in <i>B</i> oscillate around the canonical isochron. Melilite, AlTi-diopside, and spinel in <i>C</i> have resolvable δ²⁶Mg* and deviate to the left of this isochron; anorthite in both units has barely resolvable δ²⁶Mg*. Although these data are consistent with late-stage reprocessing of <i>N-</i>53, they provide no clear chronological information. We conclude that <i>N-53</i> experienced multiple melting events. Initial melting of solid precursors took place in an ¹⁶O-rich gaseous reservoir and resulted in formation of the uniformly ¹⁶O-rich (Δ¹⁷O ~ −24‰) type B CAI. Subsequent single- or multi-stage partial melting of this CAI occurred in an ¹⁶O-depleted gaseous reservoir(s) and resulted in addition of SiO and Na to the CAI melt, O- and Mg-isotope exchange, and crystallization of <i>C</i> unit.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 4","pages":"717-743"},"PeriodicalIF":2.2,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143809837","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":"Review of asteroid, meteor, and meteorite-type links","authors":"Peter Jenniskens,&nbsp;Hadrien A. R. Devillepoix","doi":"10.1111/maps.14321","DOIUrl":"https://doi.org/10.1111/maps.14321","url":null,"abstract":"<p>With the goal to determine the origin of our meteorites in the asteroid belt, video and photographic observations of meteors have now tracked 75 meteorite falls. Six years ago, there were just hints that different meteorite types arrived on different orbits, but now, the number of orbits (<i>N</i>) is high enough for distinct patterns to emerge. In general, 0.1–1-m sized meteoroids do not arrive on similar orbits as the larger ~1-km sized near-Earth asteroids (NEA) of corresponding taxonomic class. Unlike larger NEA, a group of H chondrite meteoroids arrived on low-inclined orbits from a source just beyond the 5:2 mean-motion resonance with Jupiter (<i>N</i> = 12), three of which have the 7 Ma cosmic ray exposure (CRE) age from a significant collision event among H chondrites. There is also a source of H chondrites low in the inner main belt with a ~35 Ma CRE age (<i>N</i> = 8). In contrast, larger H-like taxonomic S-class NEA arrive from high-inclined orbits out of the 3:1 resonance. Some H chondrites do so also, four of which have a 6 Ma CRE age and two have an 18 Ma CRE age. L chondrites arrive from a single source low in the inner main belt, mostly via the ν₆ secular resonance (<i>N</i> = 21), not the 3:1 resonance as most L-like NEA do. LL chondrites arrive too from the inner main belt (<i>N</i> = 5), as do larger LL-like NEA. CM chondrites are delivered from a low <i>i</i> &lt; 3<b>°</b> inclined source beyond the 3:1 resonance (<i>N</i> = 4). Source asteroid families for these meteorite types are proposed, many of which have the same CRE age as the asteroid family's dynamical age. Also, two HED achondrites are now traced to specific impact craters on asteroid Vesta.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 4","pages":"928-973"},"PeriodicalIF":2.2,"publicationDate":"2025-03-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14321","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143809835","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.14199","DOIUrl":"https://doi.org/10.1111/maps.14199","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 3","pages":"i"},"PeriodicalIF":2.2,"publicationDate":"2025-03-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14199","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143632956","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":"Revealing the relationship between 2-D and 3-D chondrule size–frequency distribution in a meteorite","authors":"Dominik C. Hezel,&nbsp;Knut Metzler,&nbsp;Mara Hochstein","doi":"10.1111/maps.14336","DOIUrl":"https://doi.org/10.1111/maps.14336","url":null,"abstract":"<p>Chondrule size–frequency distributions provide important information to understand the origin of chondrules. Size–frequency distributions are often obtained as apparent 2-D size–frequency distributions in thin sections, as determining a 3-D size–frequency distribution is notoriously difficult. The relationship between a 2-D size–frequency distribution and its corresponding 3-D size–frequency distribution has been previously modeled; however, the results contradict measured results. Models so far predict a higher mean of the 2-D size–frequency distribution than the corresponding mean of the 3-D size–frequency distribution, while the measurements of real chondrule populations show the opposite. Here, we use a new model approach that agrees with these measurements and at the same time offers a solution, why models so far predicted the opposite. Our new model provides a tool with which the 3-D chondrule size–frequency distribution can be determined from the fit of a measured 2-D chondrule size–frequency distribution.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 4","pages":"869-875"},"PeriodicalIF":2.2,"publicationDate":"2025-03-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14336","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143809536","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":"Erratum to “Effects of hot desert weathering on highly siderophile elements in ordinary chondrites”","authors":"","doi":"10.1111/maps.14334","DOIUrl":"https://doi.org/10.1111/maps.14334","url":null,"abstract":"<p>Almas, K. S., Ash, R. D., and Walker, R. J. 2024. Effects of Hot Desert Weathering on Highly Siderophile Elements in Ordinary Chondrites. <i>Meteoritics &amp; Planetary Science</i> 59: 3072–3086. https://doi.org/10.1111/maps.14267.</p><p>Agnieszka Baier was inadvertently named as the handling editor of this article. Dr. A. J. Timothy Jull was the handling editor. We apologize for this error.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 4","pages":"974"},"PeriodicalIF":2.2,"publicationDate":"2025-03-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14334","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143809497","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":"Microfaults: Abundant shear deformation and frictional melting in chondrites","authors":"Craig R. Walton,&nbsp;Mahesh Anand,&nbsp;Maria Schönbächler","doi":"10.1111/maps.14333","DOIUrl":"https://doi.org/10.1111/maps.14333","url":null,"abstract":"<p>The majority of ordinary chondrite (OC) meteorites record some amount of textural evidence for impact-induced deformation. Melt veins in some shocked samples have been compared to terrestrial impact-related pseudotachylites, which form by frictional melting of host rock. However, lacking in situ context, the role of friction in driving impact-related melting in meteorites remains unclear. Here, we present evidence for an important role for shear deformation and friction in complementing shock melting of OC material. We find microfaults directly associated with textural evidence for quenched frictional shock melt in samples of a broad range of bulk shock stages and across all three classes studied (LL, L, or H). Microfaults occur in 20% of our studied samples. We identify examples of both individual microfaults and, in rare cases, microfault networks, complete with subsidiary shear structures. Our observations indicate that friction plays an important role in melt generation in weakly to moderately shocked samples and may also be relevant for strongly shocked meteorites. Microfault structures may be of underestimated significance in chondrites in general—both with regard to their general abundance and their possible utility for elucidating the geological settings sampled by meteoritic impactites.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 4","pages":"858-868"},"PeriodicalIF":2.2,"publicationDate":"2025-03-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14333","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143809574","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":"Space weathering and compositional stratigraphy of Apollo 17 double drive tube 73001/2","authors":"Lingzhi Sun,&nbsp;Paul G. Lucey,&nbsp;Abigail Flom,&nbsp;James A. McFadden,&nbsp;Ryan A. Zeigler,&nbsp;Juliane Gross,&nbsp;Michelle S. Thompson,&nbsp;Francis M. McCubbin,&nbsp;Charles K. Shearer,&nbsp;The ANGSA Science Team","doi":"10.1111/maps.14332","DOIUrl":"https://doi.org/10.1111/maps.14332","url":null,"abstract":"<p>The double drive tube 73001/2 is a regolith core and was collected on the Light Mantle at Station 3 during the Apollo 17 mission. This core preserves an in situ record of space weathering and compositional stratigraphy, providing insights to the thickness of the Light Mantle and the local regolith reworking time scale. We measured the dissection passes 2–3 of core 73002 and passes 1–3 of core 73001 using a high-spatial resolution multispectral imaging system, and analyzed the space weathering products on individual soil grains from pass 2 of 73002 using transmission electron microscopy analysis. Our results indicate that the double drive tube 73001/2 contains a zone of submature to mature soil overlying a zone of immature soil. The top more mature zone is about 6–7 cm thick, corresponding to the local regolith reworking depth. On the basis of this depth, the estimated regolith reworking time scale for core 73001/2 is approximately 9–13 million years. Due to mixing with basaltic materials from the central valley, the top mature zone exhibits an FeO content 1–3 wt% higher than the underlying immature soils. Spectral images indicate that the double drive tube failed to penetrate the bottom of the Light Mantle but may have reached the edge of the landslide-valley material mixing zone. The local landslide deposit is thicker than the maximum sampling depth of the double drive tube, which is about 70 cm.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 4","pages":"849-857"},"PeriodicalIF":2.2,"publicationDate":"2025-03-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143809575","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}