Laura Noel García, Frederic Danoix, Martina Ávalos, Pouyan Shen, María Eugenia Varela
{"title":"Spheroidized plessite in Vaca Muerta: Formation mechanism and its implications for mesosiderites genesis and cooling history","authors":"Laura Noel García, Frederic Danoix, Martina Ávalos, Pouyan Shen, María Eugenia Varela","doi":"10.1111/maps.14352","DOIUrl":"https://doi.org/10.1111/maps.14352","url":null,"abstract":"<p>The presence of spheroidized plessite (SP) in mesosiderites was recently reported in the literature. This finding coupled with the poor understanding of this plessite variant, motivated us to investigate its formation process and evaluate its implications in assessing the previous proposals concerning mesosiderites' genesis and cooling history. SP consists of spherulitic taenite particles irregularly distributed, usually surrounded by carbides, and embedded in a kamacite matrix. It has been reported in iron meteorites containing graphite, carbides, and pearlitic plessite (PP), especially in the IAB main group and the sLL and sLH subgroups. From the combination of X-ray tomography, electron backscatter diffraction, energy-dispersive spectrometry, and atom probe tomography in three samples of Vaca Muerta mesosiderite (A1, low to moderate metamorphism) from the ICATE (Argentina) collection of meteorites, we were able to identify a common crystallographic orientation between spheroids and retained taenite, the absence of PP and the carbon depletion in the metallic portion contiguous to the spheroids, and the high volumetric connectivity of the metallic portion. Based on these findings: (i) SP likely grew at the expense of pearlite lamellae, with their absence resulting from complete consumption after an extraordinarily slow cooling rate, probably succeeding a deep burial in a breccia of rock fragments. (ii) Carbon introduction would have followed plessite formation in mesosiderites at a temperature low enough to prevent carbon solid-state diffusion. (iii) Metal would have been poured in silicates, which favors the collision model between a differentiated asteroid and a molten core for mesosiderite genesis.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 5","pages":"1236-1248"},"PeriodicalIF":2.2,"publicationDate":"2025-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930142","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}
Y. Zheng, X. Yang, M. Valdes, A. M. Davis, P. R. Heck
{"title":"Volume measurement of microparticles using SEM photogrammetry and 3-D reconstruction","authors":"Y. Zheng, X. Yang, M. Valdes, A. M. Davis, P. R. Heck","doi":"10.1111/maps.14351","DOIUrl":"https://doi.org/10.1111/maps.14351","url":null,"abstract":"<p>In this paper, we introduce a method for volume measurement of microparticles that includes scanning electron microscope photogrammetry with 3-D model construction. Our results show that our method limits the volume uncertainty to ±10%, which is a significant improvement compared to previous methods (which likely overestimated volume by 100%–200%). We also discuss how the size, morphology, and porosity of the sample can affect the uncertainty of volume measurement. We find that our method can have a significant impact on cosmic ray exposure age determinations based on noble gas concentration, with implications for our understanding of cosmic ray irradiation of refractory minerals in the early solar system and presolar grains in the interstellar medium.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 5","pages":"1227-1235"},"PeriodicalIF":2.2,"publicationDate":"2025-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14351","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930141","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":"Highly siderophile element nano-nuggets in Wabar impact glass","authors":"Axel Wittmann, Marc Biren","doi":"10.1111/maps.14350","DOIUrl":"https://doi.org/10.1111/maps.14350","url":null,"abstract":"<p>Circa 300 years ago, a ~15-m iron asteroid impacted sand dunes in the Empty Quarter of Saudi Arabia, creating the Wabar craters and fragments of the IIIAB Wabar iron meteorite. A significant portion of the asteroid dissolved into the sand, forming a wide range of impactites including glassy Wabar pearls, dumbbells, and dark scoria-like material. In this study, we report the discovery of ~60–1400 nm nuggets of refractory highly siderophile elements (HSEs) dominated by Pt, Os, Ru, Ir, Re, and Rh in Wabar impact glass. These HSEs were distributed in the IIIAB iron at low parts per million and became concentrated up to ×44,000 in the nano-nuggets. The petrologic context of the nano-nuggets is consistent with the rapid dissolution of the iron meteorite into the dune sand target triggered by the impact shockwave, followed by the separation of immiscible HSEs from the silicate impact melt at 1900°C to over 2700°C. This research provides new insights into the formation processes of HSE nano-nuggets in impact glass and predicts the potential for similar findings at other impact sites.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 6","pages":"1289-1301"},"PeriodicalIF":2.2,"publicationDate":"2025-04-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144292498","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}
Larbi Zennouri, Hasnaa Chennaoui Aoudjehane, Luigi Folco, Taha Shisseh, Abderrazak El Albani, Arnaud Mazurier, Mohamed Hassan Leili
{"title":"Tamdakht: A Moroccan ordinary chondrite fall with an uncommon fusion crust","authors":"Larbi Zennouri, Hasnaa Chennaoui Aoudjehane, Luigi Folco, Taha Shisseh, Abderrazak El Albani, Arnaud Mazurier, Mohamed Hassan Leili","doi":"10.1111/maps.14349","DOIUrl":"https://doi.org/10.1111/maps.14349","url":null,"abstract":"<p>Tamdakht meteorite is the most massive observed fall in Morocco with a total recovered mass of ~500 kg. Most of the specimens investigated in this study are covered by a well-developed primary fusion crust with thickness that reaches up to 12 mm. Macroscopic investigations reveal the development of complex fusion crust features indicative of unusual entry conditions. In some specimens, pieces of the primary fusion crust are missing, and the newly exposed areas developed a thinner fusion crust, which suggests that the former were removed during the late stages of the meteoroid's flight. Meteorite fragments are enclosed in the primary fusion crust, implying a potential intershower debris transfer prior to the dark flight and that the broken pieces were retained by the viscous fusion crust. X-ray tomographic and backscattered electron imaging shows that the primary fusion is irregular in thickness and consists of three layers. The outer layer is mainly composed of magnetite that formed as a result of the reaction of atmospheric oxygen with Fe in the melt produced by heating. The middle layer consists of zoned olivine phenocrysts, large vesicles, and metal and sulfide grains. The innermost layer displays a lower degree of melting and contains tiny vesicles, as well as metal and iron sulfides in the form of blebs and veins invading the substrate. The textural, mineralogy, and the compositional variation of Tamdakht's fusion crust imply a change in the degassing degree, temperature, and reaction with atmospheric oxygen from the surface inward.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 5","pages":"1216-1226"},"PeriodicalIF":2.2,"publicationDate":"2025-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930201","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}
Alexandre V. Andronikov, Irina E. Andronikova, Ondrej Pour, Petr Bohdalek
{"title":"A Potůčky fragment of the Steinbach IVA-an meteorite: Implications from the trace-element composition of the constituent phases","authors":"Alexandre V. Andronikov, Irina E. Andronikova, Ondrej Pour, Petr Bohdalek","doi":"10.1111/maps.14347","DOIUrl":"https://doi.org/10.1111/maps.14347","url":null,"abstract":"<p>We have analyzed in situ mineral phases in a Potůčky fragment of the stony-iron IVA-an meteorite Steinbach for trace-element compositions. The studied fragment contains silicate grains (pyroxene and tridymite) interspersed with grains of metal (kamacite, plessite, and taenite) displaying Widmanstätten pattern and troilite. Multiple inclusions of chromite, troilite, and bi-mineral troilite + taenite assemblages were observed within some pyroxene grains. The data on variations in trace-element compositions in different meteorite phases are consistent with a number of models, suggesting the involvement of several processes in the generation of the lithologies presently observed in the Potůčky meteorite. These processes might have involved fractional crystallization of silicate liquid, collision, impact, shock melting, and cooling. As a result of such processes, specific trace-element composition of different mineral phases was formed. Trace-element compositions of metals and sulfides from the Potůčky meteorite are very similar to those for minerals from the LL ordinary chondrite, suggesting LL-like asteroid as a parent body for the Potůčky (IVA-an) precursor material.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 5","pages":"1166-1193"},"PeriodicalIF":2.2,"publicationDate":"2025-04-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930314","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}
Markus Patzek, Yogita Kadlag, Miriam Rüfenacht, Evelyn Füri, Andreas Pack, Addi Bischoff, Harry Becker, Robbin Visser, Timm John, Maria Schönbächler
{"title":"Multi-isotope (N, O, Ti, and Cr) study of C1 and CM-like clasts—Probing unsampled C1 material","authors":"Markus Patzek, Yogita Kadlag, Miriam Rüfenacht, Evelyn Füri, Andreas Pack, Addi Bischoff, Harry Becker, Robbin Visser, Timm John, Maria Schönbächler","doi":"10.1111/maps.14343","DOIUrl":"https://doi.org/10.1111/maps.14343","url":null,"abstract":"<p>A multi-element isotope (N, O, Ti, and Cr) study was conducted on C1 and CM-like clasts hosted in achondrites and chondrite breccias to understand the genesis of these chondritic clasts. The mineralogy, O, and N isotopes confirm that CM-like clasts in howardites and polymict eucrites closely resemble CM chondrite-like material. The O and Cr isotope composition of C1 clasts in CR chondrites overlaps with those of CR chondrites, implying either formation in a similar nebular environment or resemblance to local CR material that underwent more extensive in situ alteration. Notably, these clasts are less enriched in <sup>15</sup>N than bulk CR chondrites. In contrast, C1 clasts in ureilites are enriched in <sup>15</sup>N relative to the Earth's atmosphere by ~100‰ setting them apart from any other known solar system material. They display elevated <sup>17</sup>O and <sup>18</sup>O values and lie along the CCAM line. In addition, a C1 clast from an ureilite represents the most <sup>54</sup>Cr-enriched and <sup>50</sup>Ti-depleted endmember among the carbonaceous chondrites. Altogether, these isotopic characteristics suggest that C1 clasts in ureilites represent material not sampled by any known meteorite group. Overall, this study highlights the presence of primitive, isotopically distinct materials in the early outer solar system, some of which were transported to the inner solar system to the accretion region of the host parent bodies.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 5","pages":"1073-1094"},"PeriodicalIF":2.2,"publicationDate":"2025-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14343","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930311","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}
Alice Macente, Luke Daly, Sammy Griffin, Maria Gritsevich, Jarmo Moilanen, Josh Franz Einsle, Patrick Trimby, Chris Mulcahy, Jonathan Moffat, Alexander M. Ruzicka
{"title":"The petrology of the Ozerki meteorite constrained by electron backscatter diffraction and X-ray computed tomography","authors":"Alice Macente, Luke Daly, Sammy Griffin, Maria Gritsevich, Jarmo Moilanen, Josh Franz Einsle, Patrick Trimby, Chris Mulcahy, Jonathan Moffat, Alexander M. Ruzicka","doi":"10.1111/maps.14344","DOIUrl":"https://doi.org/10.1111/maps.14344","url":null,"abstract":"<p>Combining electron backscatter diffraction (EBSD) with X-ray computed tomography (XCT) offers a comprehensive approach to investigate shock deformation and rock texture in meteorites, yet such integration remains uncommon. In this study, we demonstrate the synergistic potential of XCT and EBSD in revealing deformation metrics, thereby enhancing our understanding of petrofabric strength and shock-induced deformation. Our analysis focuses on the Ozerki (L6, S4/5, W0) meteorite fall, which was instrumentally observed on June 21, 2018, and subsequently recovered by the Ural's branch of the Russian Fireball Network (UrFU) recovery expedition a few days later. The trajectory analysis conducted by the Finnish Fireball Network facilitated the prompt retrieval of the meteorite. We show that Ozerki is deformed, with a moderate strength foliation fabric defined by metal and sulfide grain shapes. Microstructural analysis using EBSD shows that the parent body was likely still thermally active during this impact event. Our data suggest that these microstructures were likely produced during an impact while the Ozerki's parent body was still warm.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 5","pages":"1095-1118"},"PeriodicalIF":2.2,"publicationDate":"2025-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://onlinelibrary.wiley.com/doi/epdf/10.1111/maps.14344","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930312","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":"Evidence of solar wind irradiation on mineral grains embedded in matrix of the Northwest Africa 801 CR chondrite","authors":"Sohei Wada, Ken-ichi Bajo, Tomoya Obase, Hisayoshi Yurimoto","doi":"10.1111/maps.14346","DOIUrl":"https://doi.org/10.1111/maps.14346","url":null,"abstract":"<p>Solar wind (SW) is preserved in meteorites as abundant solar noble gases. We performed in situ <sup>4</sup>He isotope imaging of mineral grains in the CR2 chondrite matrix of Northwest Africa 801 using time-of-flight secondary neutral mass spectrometry with strong-field post ionization. <sup>4</sup>He<sup>+</sup> signals were detected along the surfaces of individual grains of Fe-Ni metal, ferrihydrite, olivine, pyroxene, and troilite. The high <sup>4</sup>He concentrations along the surfaces indicate implantation of SW into the mineral grains. We determined the SW-<sup>4</sup>He fluence of eight mineral grains from the line profiles across the grain boundaries. SW-<sup>4</sup>He fluence ranged from 2.7 × 10<sup>16</sup> to 58 × 10<sup>16</sup> atoms cm<sup>−2</sup>. These fluences were then used to calculate the SW irradiation durations. Assuming irradiation occurred at 4 astronomical units, the durations ranged from 3.8 to 82 kyr. These durations correspond to the residence time of individual mineral grains on the surface of the parent body. The variation in residence time for the mineral grains suggests variable durations for local mixing and burial processes on the parent body. The SW exposure ages provide insights into the gardening rate driven by small-scale impact mixing processes on the parent body.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 5","pages":"1151-1165"},"PeriodicalIF":2.2,"publicationDate":"2025-03-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930480","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}
Peter Jenniskens, Gerardo J. Soto, Gabriel Goncalves Silva, Oscar Lücke, Pilar Madrigal, Tatiana Ballestero, Carolina Salas Matamoros, Paulo Ruiz Cubillo, Daniela Cardozo Mourao, Othon Cabo Winter, Rafael Sfair, Clemens E. Tillier, Jim Albers, Laurence A. J. Garvie, Karen Ziegler, Qing-Zhu Yin, Matthew E. Sanborn, Henner Busemann, My E. I. Riebe, Kees C. Welten, Marc W. Caffee, Matthias Laubenstein, Darrel K. Robertson, David Nesvorný
{"title":"Orbit, meteoroid size, and cosmic ray exposure history of the Aguas Zarcas CM2 breccia","authors":"Peter Jenniskens, Gerardo J. Soto, Gabriel Goncalves Silva, Oscar Lücke, Pilar Madrigal, Tatiana Ballestero, Carolina Salas Matamoros, Paulo Ruiz Cubillo, Daniela Cardozo Mourao, Othon Cabo Winter, Rafael Sfair, Clemens E. Tillier, Jim Albers, Laurence A. J. Garvie, Karen Ziegler, Qing-Zhu Yin, Matthew E. Sanborn, Henner Busemann, My E. I. Riebe, Kees C. Welten, Marc W. Caffee, Matthias Laubenstein, Darrel K. Robertson, David Nesvorný","doi":"10.1111/maps.14337","DOIUrl":"https://doi.org/10.1111/maps.14337","url":null,"abstract":"<p>The Aguas Zarcas (Costa Rica) CM2 carbonaceous chondrite fell during nighttime in April 2019. Security and dashboard camera videos of the meteor were analyzed to provide a trajectory, light curve, and orbit of the meteoroid. The trajectory was near vertical, 81° steep, arriving from an ~109° (WNW) direction with an apparent entry speed of 14.6 ± 0.6 km s<sup>−1</sup>. The meteoroid penetrated to ~25 km altitude (5 MPa dynamic pressure), where the surviving mass shattered, producing a flare that was detected by the Geostationary Lightning Mappers on GOES-16 and GOES-17. The cosmogenic radionuclides were analyzed in three recovered meteorites by either gamma-ray spectroscopy or accelerator mass spectrometry (AMS), while noble gas concentrations and isotopic compositions were measured in the same fragment that was analyzed by AMS. From this, the pre-atmospheric size of the meteoroid and its cosmic ray exposure age were determined. The studied samples came from a few cm up to 30 cm deep in an object with an original diameter of ~60 cm that was ejected from its parent body 2.0 ± 0.2 Ma ago. The ejected material had an argon retention age of 2.9 Ga. The object was delivered most likely by the 3:1 or 5:2 mean motion resonances and, without subsequent fragmentation, approached the Earth from a low <i>i</i> < 2.8° inclined orbit with a perihelion distance <i>q</i> = 0.98 AU close to the Earth's orbit. The steep entry trajectory and high strength resulted in deep penetration in the atmosphere and a relatively large fraction of surviving mass.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 5","pages":"997-1022"},"PeriodicalIF":2.2,"publicationDate":"2025-03-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930371","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}
Franz Brandstätter, Niels J. de Winter, Alessandro Migliori, Roman Padillia-Alvarez, Dan Topa, Seerp Visser, Steven Goderis, Philippe Claeys, Christian Koeberl
{"title":"On the possible contribution of meteoritic metal to Ni-rich Indonesian kris daggers: Comparing original daggers and newly forged analog objects","authors":"Franz Brandstätter, Niels J. de Winter, Alessandro Migliori, Roman Padillia-Alvarez, Dan Topa, Seerp Visser, Steven Goderis, Philippe Claeys, Christian Koeberl","doi":"10.1111/maps.14340","DOIUrl":"https://doi.org/10.1111/maps.14340","url":null,"abstract":"<p>The “Weltmuseum Wien” owns a large collection of kris daggers from Indonesia. These objects are famous for their metal blades consisting of numerous layers made by a complicated forging process involving repeated folding and welding of the individual layers. There is a widespread belief that some krises were manufactured by adding meteoritic nickel–iron from the Prambanan meteorite that fell in Central Java and is known since the late 18th century. In our study, we investigated a selection of five Ni-rich krises from this collection with the aim to identify in their blades nickel–iron from Prambanan or another iron meteorite source. To obtain a better insight into the forging process, we investigated analog objects that were produced by a forging procedure similar to the one applied in the production of original krises and by using iron meteorite material from the meteorites Campo del Cielo and Gibeon as admixture. These investigations were performed by nondestructive analytical techniques, including handheld X-ray fluorescence (HH-XRF) analysis, scanning electron microscopy (SEM), and electron microprobe (EMP) analysis. The original daggers were investigated by HH-XRF and micro-X-ray fluorescence (μ-XRF) analysis, as well as by portable laser ablation (pLA) subsampling followed by trace element analysis using inductively coupled plasma mass spectrometry (ICP-MS). By comparing the data obtained for both materials, we demonstrate that the main difficulties in identifying the presence of a meteoritic component in the kris daggers are due to the exclusive use of (quasi-)nondestructive methods in combination with locally varying surface heterogeneities, resulting from contamination, corrosion, and etching features. We also show that the presence of significant amounts of Ni and Co (in the wt% range) in a premodern kris dagger does not imply that it was manufactured with an admixture of meteoritic metal. We found that among the five krises investigated, only a single dagger (no. 900382) was manufactured with the possible admixture of nickel–iron from the Prambanan iron meteorite, as it contains high concentrations of siderophile elements and has a Ni/Co ratio comparable to that of the meteorite.</p>","PeriodicalId":18555,"journal":{"name":"Meteoritics & Planetary Science","volume":"60 5","pages":"1023-1047"},"PeriodicalIF":2.2,"publicationDate":"2025-03-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143930407","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}