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87th Annual Meeting of the Meteoritical Society 2025: Contents 2025年第87届气象学会年会:内容
IF 2.4 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS Pub Date : 2025-09-09 DOI: 10.1111/maps.70032
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引用次数: 0
87th Annual Meeting of the Meteoritical Society 2025: Cover 第87届气象学会年会2025:封面
IF 2.4 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS Pub Date : 2025-09-09 DOI: 10.1111/maps.70034

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引用次数: 0
Trace element analyses of plagioclase from troctolite 76535 and implications for the petrogenesis of the lunar highlands Mg-suite 月球高原滑石76535中斜长石的微量元素分析及其对镁套岩成因的启示
IF 2.4 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS Pub Date : 2025-09-09 DOI: 10.1111/maps.70047
Isaiah Spring, Ananya Mallik, Jason Kirk, Pranabendu Moitra, Richard Hervig, Lars Borg

We used trace element analyses of plagioclase from Mg-suite troctolite 76535 to estimate the Rare Earth Element (REE) concentrations of its parental liquid and assess the feasibility of an urKREEP contribution to the Mg-suite parental liquid. We measured 33 trace elements in 76535 plagioclase separates. Our measurements revealed enrichments in incompatible elements consistent with previous analyses. Using the measured REE concentrations, we estimated the REE concentrations of the unfractionated Mg-suite parental liquid using a RhyoliteMELTS-based forward model. Compared to chondritic concentrations, the Mg-suite parental liquid is ~100 times more enriched in light REEs and ~10 times more enriched in heavy REEs. We sought to explore the feasibility of reproducing these enrichments in the parental liquid through assimilation of urKREEP by a partial melt of rising LMO cumulates during cumulate mantle overturn. We show that these enrichments can be reproduced by a 30%–50% addition of fully molten urKREEP to the LMO cumulate melt, if the LMO cumulate melt and urKREEP are in thermal equilibrium with each other. However, the Mg# of these mixtures (57–68) is too low to produce the most Mg-rich olivine (Fo 91) observed in Mg-suite troctolites. Alternatively, assuming that the LMO cumulate melt and urKREEP are in thermal disequilibrium, we reproduced both the REE abundances and Mg# of the Mg-suite parental liquid with only a 10% addition of the urKREEP partial melt. These results support the feasibility of urKREEP assimilation as a mechanism for generating the incompatible element enrichments in Mg-suite magmas while preserving their major element chemistry.

通过对76535 mg套件橄榄岩斜长石的微量元素分析,估算了其母液中稀土元素的浓度,并评估了urKREEP对mg套件母液贡献的可行性。在76535份斜长石分离物中测定了33种微量元素。我们的测量结果显示不相容元素的富集与先前的分析一致。利用测量到的稀土浓度,我们使用基于rhyolitemelts的正推模型估算了未分馏mg套件母液的稀土浓度。与球粒体浓度相比,镁组亲本液的轻稀土富集量是球粒体浓度的100倍,重稀土富集量是球粒体浓度的10倍。我们试图探索在累积地幔翻转过程中,通过上升的LMO堆积的部分熔融同化urKREEP,在母质液体中再现这些富集的可行性。我们发现,如果LMO累积熔体和urKREEP彼此处于热平衡状态,那么在LMO累积熔体中加入30%-50%完全熔融的urKREEP可以重现这些富集。然而,这些混合物的mg#(57-68)太低,无法产生在镁套橄榄岩中观察到的最富镁的橄榄石(f91)。或者,假设LMO累积熔体和urKREEP处于热不平衡状态,我们只添加10%的urKREEP部分熔体,就可以重现Mg套件母液的REE丰度和Mg#。这些结果支持了urKREEP同化作为一种机制的可行性,即在保持镁套件岩浆主要元素化学性质的同时产生不相容元素富集。
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引用次数: 0
In situ Sr-Nd-Pb isotopes of lunar basaltic meteorite NWA 14526: Implications for the generation of young mare basalts 月球玄武岩陨石NWA 14526的原位Sr-Nd-Pb同位素:对年轻海母玄武岩生成的启示
IF 2.4 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS Pub Date : 2025-09-08 DOI: 10.1111/maps.70048
Le Zhang, Zexian Cui, Zhiming Chen, Qing Yang, Jingyou Chen, Ya-Nan Yang, Pengli He, Haiyang Xian, Chengyuan Wang, Jintuan Wang, Yan-Qiang Zhang, Yi-Gang Xu

This study presents a comprehensive analysis of the mineralogical, geochemical properties, and in situ Sr-Nd-Pb isotopic systematics of a newly discovered unbrecciated lunar basaltic meteorite NWA 14526 (NWA refers to northwest Africa). Bulk composition derived through both mineral modes and impact melt vein classifies NWA 14526 as a low-Ti, low-Al, and low-K mare basalt. In situ Pb isotopic analyses define a Pb–Pb isochron yielding an age of 3009 ± 43 Ma, representing the meteorite's crystallization age. In situ Rb-Sr isotopic analyses of plagioclase and maskelynite provide an initial 87Sr/86Sr ratio of 0.69969 ± 0.00024 (2σ), while phosphate and mesostasis in situ Sm-Nd analyses yield an initial εNd value of +10.7 ± 2.1 (2σ). Although NWA 14526 shares comparable mineralogical, bulk-rock composition, and Sr isotopic characteristics with contemporaneous lunar basaltic meteorites (NWA 4734, LAP 02205, NWA 14137, and NWA 10597), its significantly elevated εNd values preclude genetic pairing with these specimens. Isotopic modeling indicates minimal KREEP component contribution (<0.5%) in its mantle source. Our compilation of lunar Sr-Nd isotopic data reveals two distinct evolutionary trends corresponding to depleted lunar mantle and urKREEP reservoirs, respectively. Notably, no temporal correlation between basalt source KREEP enrichment and eruption age is observed, suggesting that the KREEP component did not necessarily play a decisive role in driving late-stage lunar magmatism and volcanism.

对新发现的未角化月球玄武岩陨石NWA 14526 (NWA指非洲西北部)的矿物学、地球化学性质和原位Sr-Nd-Pb同位素系统进行了综合分析。通过矿物模式和冲击熔体脉得出的整体成分将NWA 14526归类为低钛、低铝和低钾海母玄武岩。原位Pb同位素分析确定了Pb - Pb等时线,得出的年龄为3009±43 Ma,代表了陨石的结晶年龄。斜长石和掩斑岩的原位Rb-Sr同位素初始比值为0.69969±0.00024 (2σ),而磷酸盐和中稳态Sm-Nd原位分析的初始εNd值为+10.7±2.1 (2σ)。尽管NWA 14526与同时期月球玄武岩陨石(NWA 4734、LAP 02205、NWA 14137和NWA 10597)具有相似的矿物学、块状岩石组成和Sr同位素特征,但其显著升高的εNd值排除了与这些样本的遗传配对。同位素模拟表明,其地幔源中KREEP组分的贡献最小(<0.5%)。我们收集的月球Sr-Nd同位素数据揭示了两种截然不同的演化趋势,分别对应于枯竭的月球地幔和urKREEP储层。值得注意的是,玄武岩源KREEP富集与喷发年龄之间没有时间相关性,表明KREEP成分不一定在推动晚期月球岩浆活动和火山活动中起决定性作用。
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引用次数: 0
Secondary corundum in CAIs from CK3 carbonaceous chondrites dates metasomatic alteration of CK chondrites 来自CK3碳质球粒陨石的CAIs中的次生刚玉确定了CK球粒陨石交代变化的年代
IF 2.4 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS Pub Date : 2025-09-08 DOI: 10.1111/maps.70044
A. N. Krot, K. Nagashima, S. Ebert, M. I. Petaev, C. Ma, J. Han, T. L. Dunn

We report on the mineralogy, petrography, and oxygen and aluminum-magnesium isotopic systematics of the corundum-bearing Ca,Al-rich inclusions (CAIs) from the CK3 (Karoonda-type) carbonaceous chondrites NWA (Northwest Africa) 4964-#1 and -Homer, NWA 5343-#1, and LAR (Larkman Nunatak) 12002-#1. These CAIs experienced extensive metasomatic alteration: melilite and possibly anorthite and AlTi-diopside are nearly completely replaced by secondary corundum, grossular, CaNa-plagioclase, FeAl-diopside, and FeO-rich spinel; perovskite is largely replaced by ilmenite. Two types of corundum grains occur in the NWA 4964 CAIs: (1) compact, FeO-poor grains zoned in cathodoluminescent (CL) images and (2) FeO-bearing (up to 1.5 wt% FeO), porous grains showing no detectable CL; the porous corundum grains overgrow the compact ones. Corundum grains in CAIs from LAR 12002 and NWA 5343 belong to the first and second types, respectively. Hibonite, primary spinel, and rare perovskite inclusions in spinel retained the original, 16O-rich compositions (Δ17O ~ −24 ± 2‰), whereas melilite, most perovskite grains, and secondary corundum and spinel are 16O-depleted (Δ17O ~ −5 ± 2‰). Hibonite and melilite have excesses of radiogenic 26Mg (26Mg*) corresponding to approximately the canonical initial 26Al/27Al ratio [(26Al/27Al)0] of ~5 × 10−5 suggesting that corundum-bearing CAIs studied belong to a population of the canonical inclusions, dominant in most chondrite groups. Corundum grains in LAR 12002-#1, NWA 4964-#1, NWA 4964-Homer, and NWA 5343-#1 show resolvable 26Mg* correlated with 27Al/24Mg ratio which corresponds to much lower than the canonical (26Al/27Al)0: (3.10 ± 0.48) × 10−6, (3.03 ± 0.23) × 10−6, (2.72 ± 0.19) × 10−6, and (3.5 ± 1.2) × 10−7, respectively. Porous Fe-bearing corundum grains in NWA 4964 CAIs Homer and #1 have low 26Mg* not correlated with 27Al/24Mg ratio. We conclude that compact corundum grains in the CK3 CAIs studied are secondary parent body products that resulted from metasomatic alteration of the host inclusions by hydrothermal fluid ~3−5 Ma after their crystallization. Porous corundum grains may have formed by dehydration of diaspore [AlO(OH)] during subsequent thermal metamorphism.

本文报道了CK3 (karoonda型)碳质球粒陨石NWA(西北非洲)4964-#1和- homer, NWA 5343-#1和LAR (Larkman Nunatak) 12002-#1中含刚玉的Ca, al富包裹体(CAIs)的矿物学、岩石学、氧和铝镁同位素系统。这些CAIs经历了广泛的交代蚀变:千英石(可能还有钙长石和铝透辉石)几乎完全被次生刚玉、粗晶、cana斜长石、铁透辉石和富feo尖晶石所取代;钙钛矿大部分被钛铁矿取代。NWA 4964 CAIs中出现了两种类型的刚玉颗粒:(1)致密,阴极发光(CL)图像中显示FeO贫颗粒;(2)含FeO(高达1.5 wt% FeO),多孔颗粒,未检测到CL;多孔刚玉晶粒比致密刚玉晶粒长得多。LAR 12002和NWA 5343的CAIs中刚玉晶粒分别属于第一类和第二类。尖晶石中的Hibonite、原生尖晶石和稀有钙钛矿包裹体保留了原始的富含16o的成分(Δ17O ~−24±2‰),而melilite、大多数钙钛矿颗粒、次生刚玉和尖晶石则缺乏16o (Δ17O ~−5±2‰)。Hibonite和melilite具有过量的放射性成因26Mg (26Mg*),大约对应于典型的初始26Al/27Al比值[(26Al/27Al)0]为~5 × 10−5,这表明所研究的含刚玉的CAIs属于典型包裹体群体,在大多数球粒陨石群中占主导地位。在LAR 12002-#1、NWA 4964-#1、NWA 4964- homer和NWA 5343-#1中,刚玉晶粒的26Mg*与27Al/24Mg比值的相关性远低于规范的(26Al/27Al)0:(3.10±0.48)× 10−6、(3.03±0.23)× 10−6、(2.72±0.19)× 10−6和(3.5±1.2)× 10−7。NWA 4964 CAIs Homer和#1的多孔含铁刚玉颗粒26Mg*较低,与27Al/24Mg比值无关。我们认为,CK3 CAIs致密刚玉颗粒是在结晶后3 ~ 5 Ma的热液作用下,寄主包裹体发生交代蚀变的次生母体产物。多孔刚玉颗粒可能是由一水硬铝石[AlO(OH)]在随后的热变质过程中脱水形成的。
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引用次数: 0
Löpönvaara: A new phosphorus-rich iron meteorite from Finland Löpönvaara:来自芬兰的一颗新的富磷铁陨石
IF 2.4 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS Pub Date : 2025-09-08 DOI: 10.1111/maps.70049
Laura Kotomaa, Markku Väisänen, Jussi S. Heinonen, Ermei Mäkilä, Hugh O'Brien, Arto Peltola

Löpönvaara is a rare new phosphorus-rich iron meteorite find from Löpönvaara, Finland. The ~164 g meteorite was discovered in 2017 from the same area as the ungrouped Lieksa pallasite. Löpönvaara was classified as an ungrouped iron meteorite due to its unusually high concentration of P (>4 wt%), coupled with a moderate concentration of Ni (~11 wt%), and Ga–Ge abundances in the “III” range. The meteorite consists of ~75 vol% kamacite and ~22 vol% schreibersite, with accessory troilite (<0.1 vol%), and minor terrestrial weathering products. The kamacite in Löpönvaara occurs as three different types: (1) rare, large 2–5 mm partially resorbed clasts; (2) round, ≤0.5 mm partially resorbed clasts; and (3) small, several tens of μm to sub-μm exsolution blebs and globules in the matrix. Schreibersite occurs solely as microscopic matrix material in between the type (1) and (2) kamacite clasts. The lack of taenite and the overall compositional and textural features of Löpönvaara suggest that it retained its composition possibly from a P-rich portion of immiscible melt at late stages of fractional crystallization, but its textural features suggest that the meteorite suffered impact-related metamorphism. The meteorite has no close textural or compositional affinities, which makes it unique and an important target for future studies.

Löpönvaara是芬兰Löpönvaara发现的一颗罕见的新富磷铁陨石。这颗重约164克的陨石是在2017年与未分类的Lieksa pallasite在同一地区发现的。Löpönvaara由于其异常高浓度的P (>4 wt%),加上中等浓度的Ni (~11 wt%),以及在“III”范围内的Ga-Ge丰度,被归类为未分类的铁陨石。该陨石由~75 vol%的绢云母岩和~22 vol%的晶长石组成,伴生有<;0.1 vol%的绢云母岩和少量的陆地风化产物。Löpönvaara的绢云母岩主要有三种类型:(1)罕见的2 ~ 5 mm大的部分再吸收碎屑;(2)圆形,≤0.5 mm部分再吸收碎屑;(3)基体中存在数十μm至亚μm的小气泡和小球。在(1)型和(2)型卡玛石碎屑之间,schreiberite仅作为微观基质物质存在。Löpönvaara缺少带长石,其整体组成和结构特征表明其成分可能来自于分离结晶后期非混溶熔体的富p部分,但其结构特征表明该陨石遭受了撞击相关的变质作用。该陨石没有紧密的结构或成分亲和力,这使得它成为未来研究的重要目标。
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引用次数: 0
The nature and formation of silica minerals in eucrite meteorites: Insight into the protoplanetary magma crystallization 长晶陨石中二氧化硅矿物的性质与形成:对原行星岩浆结晶的洞察
IF 2.4 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS Pub Date : 2025-09-06 DOI: 10.1111/maps.70045
Rei Kanemaru, Akira Yamaguchi, Naoya Imae, Ryoga Maeda, Makoto Kimura, Kenji Horie, Takashi Mikouchi, Masaaki Miyahara, Masahiro Yasutake, Atsushi Takenouchi, Haruka Ono, Aiko Nakato, Junko Isa, Tomohiro Usui, Hirotsugu Nishido

Silica polymorphs in meteorites provide critical constraints on crystallization processes associated with thermal activity in the early solar system. A detailed investigation of silica polymorphs in eucrites (the largest group of achondrites) using cathodoluminescence imaging and laser-Raman spectroscopy revealed significant variations in the relative abundance of silica polymorphs. Based on these variations, the eucrites were divided into four “Si-groups” according to their dominant silica phase: Si-0 (cristobalite-dominant eucrites), Si-I (quartz-dominant eucrites), Si-II (quartz and tridymite-dominant eucrites), and Si-III (tridymite-dominant eucrites). In studied eucrites, tridymite and cristobalite form lathy euhedral shapes, while quartz is anhedral, coexistent with opaques and phosphates, suggesting that silica polymorphs were crystallized from different stages and formation processes. We propose a new model that explains the formation pathways of silica minerals in eucrites and accounts for the distinct formation histories represented by each Si-group: tridymite crystallizes from alkali-rich immiscible melts (starting at ≥ ~1060°C), cristobalite crystallizes from quenched melts (~1060°C), and quartz crystallizes from extremely differentiated melts and/or by solid-state transformation from tridymite and cristobalite through interactions with sulfur-rich vapor below ~1025°C. This model explains the occurrences of silica polymorphs in eucrites without requiring secondary heating or shock processes.

陨石中的二氧化硅多晶态提供了与早期太阳系热活动相关的结晶过程的关键限制。利用阴极发光成像和激光拉曼光谱对长晶硅多晶(最大的无球粒陨石群)进行了详细的研究,揭示了硅多晶相对丰度的显著变化。在此基础上,根据其优势硅相将其划分为4个“si族”:Si-0(方英石-优势长长岩)、Si-I(石英-优势长长岩)、Si-II(石英-三晶石-优势长长岩)和Si-III(三晶石-优势长长岩)。石英为正面体,与不透明体和磷酸盐共存,表明石英多晶体的结晶阶段和形成过程不同。我们提出了一个新的模型来解释硅矿物在辉长岩中的形成途径,并解释了每一个硅基团所代表的不同的形成历史:从富碱的不混溶熔体(开始于≥~1060℃)中形成三角石结晶,从淬火熔体(~1060℃)中形成方英石结晶,从极端分化的熔体和/或由三角石和方英石在~1025℃以下与富硫蒸汽相互作用而形成的固态转变中形成石英结晶。该模型解释了在不需要二次加热或冲击过程的情况下二氧化硅多晶在长晶中的出现。
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引用次数: 0
A statistical investigation into relationships between the IIE irons and the ordinary, F and “HH” chondrites IIE铁与普通、F和HH球粒陨石之间关系的统计研究
IF 2.4 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS Pub Date : 2025-09-05 DOI: 10.1111/maps.70040
Rachel S. Kirby, Penelope L. King, Andrew G. Tomkins

It has been proposed that IIE iron meteorites formed through impact processes on a parent body that was composed of either the H chondrites or a much-debated fourth ordinary chondrite group, the HH chondrites. To resolve this debate, we have compiled a large dataset for the ordinary chondrites, low-fayalite ungrouped chondrites, and IIE irons, and undertaken a statistical analysis to determine if: (1) the current classification of ordinary chondrite groups is statistically appropriate; and (2) the IIE irons are related to H chondrites or if they represent a distinct group that formed on a “HH” chondrite parent body. We demonstrate that the current classification system based on petrography and olivine and orthopyroxene chemistry is appropriate for the H, L, and LL chondrites. We define a fourth “F chondrite” group consisting of eight, previously ungrouped, very low-Fa Type 3 and 4 chondrites. Statistical analysis of Δ17O data alone cannot distinguish between the H chondrites and IIE irons, nor between the L and LL chondrites. Furthermore, statistical analyses are unable to distinguish H chondrites from IIE irons in all measures (mineral chemistry, chondrule size, bulk Δ17O, Ge and Mo isotopic compositions, and bulk siderophile element abundances in metal); there is no evidence for a “HH” chondrite group. These results are consistent with formation of IIE iron meteorites through impact melting and near-surface metal segregation on the H chondrite parent body. This genetic link between H chondrites and IIE irons allows us to understand the geochemical and petrological changes that occurred during planetary formation and evolution.

有人提出,IIE铁陨石是由H球粒陨石或备受争议的第四种普通球粒陨石HH球粒陨石组成的母体撞击形成的。为了解决这一争论,我们编制了普通球粒陨石、低球粒陨石未分组球粒陨石和IIE铁的大型数据集,并进行了统计分析,以确定:(1)目前普通球粒陨石组的分类在统计上是否合适;(2) IIE铁与H球粒陨石有关,或者它们是否代表了在“HH”球粒陨石母体上形成的不同群。研究表明,目前基于岩石学、橄榄石和正辉石化学的分类体系适合于H、L和LL球粒陨石。我们定义了第四个“F球粒陨石”组,由8个以前未分组的非常低fa的3型和4型球粒陨石组成。单靠Δ17O数据的统计分析无法区分H型球粒陨石和IIE铁,也无法区分L型和LL型球粒陨石。此外,统计分析无法在所有测量(矿物化学、球粒大小、体积Δ17O、Ge和Mo同位素组成以及金属中亲铁元素的体积丰度)中区分H球粒陨石和IIE铁;没有证据表明存在“HH”球粒陨石群。这些结果与在H球粒陨石母体上通过撞击熔融和近表面金属偏析形成IIE铁陨石的理论一致。H球粒陨石和IIE铁之间的遗传联系使我们能够了解行星形成和演化过程中发生的地球化学和岩石学变化。
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引用次数: 0
Isotopic analysis of tochilinite (carbonate and magnetite) in Winchcombe: Temperature constraints on early-stage aqueous alteration in the CM parent body 温奇库姆地区tochilinite(碳酸盐和磁铁矿)同位素分析:CM母体早期水蚀变的温度约束
IF 2.4 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS Pub Date : 2025-09-03 DOI: 10.1111/maps.70043
M. D. Suttle, R. Findlay, I. A. Franchi, C. Biagioni, X. Zhao, F. A. J. Abernethy, L. Riches, L. Folco

We report the first oxygen isotope measurements of tochilinite (δ17O: 11.0 ± 2.1‰, δ18O: 23.5 ± 4.0‰ and Δ17O: −1.1 ± 1.2‰) in a CM chondrite (Winchcombe, lithology C [CM2.2/2.3]). We analyzed type-I tochilinite-cronstedtite intergrowths (TCIs)—formed by pseudomorphic replacement of kamacite. Alongside T1 and T2 calcite and magnetite, these secondary phases define a linear trendline in δ17O-δ18O isotope space with a slope of 0.50, slightly shallower than the mass-dependent slope (0.52). This demonstrates that, in addition to dominant mass-dependent fractionation (controlled by mineral-specific and temperature-dependent equilibrium processes), mass-independent mixing between 16O-rich anhydrous silicates, and 16O-poor water influenced the evolving Δ17O composition of alteration fluids. Petrographic evidence shows tochilinite and T1 calcite formed early and are closely associated in the alteration sequence. Assuming isotopic equilibrium between these phases, we estimate formation temperatures of approximately 135°C and a δ18Owater value of 28‰. These findings align with previous hydrothermal synthesis experiments and underscore the value of multi-phase isotopic measurements for reconstructing the fluid history of chondritic parent bodies.

本文报道了CM球粒陨石(Winchcombe,岩性C [CM2.2/2.3])中tochilinite的首次氧同位素测量结果(δ17O: 11.0±2.1‰,δ18O: 23.5±4.0‰和Δ17O:−1.1±1.2‰)。我们分析了由假晶替代卡玛石而形成的i型透辉石-透辉石共生体(tci)。这些次级相与T1和T2方解石和磁铁矿一起在δ17O-δ18O同位素空间中定义了一条线性趋势线,斜率为0.50,略低于质量相关斜率(0.52)。这表明,除了主要的质量依赖分馏(由矿物特异性和温度依赖的平衡过程控制)外,富含16o的无水硅酸盐和缺乏16o的水之间的质量独立混合影响了蚀变流体Δ17O组成的演化。岩石学证据表明,tochilinite和T1方解石形成较早,在蚀变序列中关系密切。假设这些相之间的同位素平衡,我们估计地层温度约为135℃,δ18Owater值为28‰。这些发现与以前的热液合成实验相一致,强调了多相同位素测量对重建球粒质母体流体历史的价值。
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引用次数: 0
Composition and origin of the Chang'E-5 regolith breccias 嫦娥五号风化角砾岩的组成及成因
IF 2.4 4区 地球科学 Q2 GEOCHEMISTRY & GEOPHYSICS Pub Date : 2025-09-02 DOI: 10.1111/maps.70042
Zhi-Ming Chen, Le Zhang, Cheng-Yuan Wang, Ya-Nan Yang, Peng-Li He, Hai-Yang Xian, Xiao-Ping Xia, Jian-Xi Zhu, Yi-Gang Xu

Numerous studies of basalt clasts in regolith samples returned by the Chang'E-5 (CE-5) mission have provided constraints on the timing and nature of the youngest magmatism on the Moon. However, there have been far fewer studies of breccias, one of the main constituents of regolith. Here, we present a comprehensive investigation of the mineralogy, petrology, and U-Pb geochronology of two CE-5 regolith breccia samples, which are composed of lithic clasts, agglutinates, glass particles, and mineral fragments. In contrast to the high level of maturity of CE-5 regolith, the regolith breccias are immature, as judged by their low agglutinate (~11 vol%) and moderate to low matrix contents (~49 vol%). The CE-5 regolith breccias comprise mainly mare (~90 vol%) and non-mare (~10 vol%) materials. A low-Ti mare component of late Imbrian to early Eratosthenian age is identified, in addition to the predominant late Eratosthenian basalts in mare components. Non-mare components include Mg-suite norite, highland impact melt clasts, glass particles, and minor fragmented minerals. The glass particles in the CE-5 regolith breccias are compositionally variable and can be divided into five types, that is, basaltic (mare), KREEP-rich, feldspathic (highland), Si-poor, and Si-K-rich glasses. Among these glasses, most (65%) are compositionally exotic to the site. The diverse provenance of these “exotic” materials in the CE-5 breccias is consistent with the multiple ages of Zr-bearing phases at 3.97–3.92 Ga, ~3.2 Ga, 2.93–2.40 Ga, and ~2.0 Ga, in which early Eratosthenian ages are reported for the first time from returned lunar samples. The contrast in the level of maturity and in glass composition between CE-5 regolith and regolith breccias can be reconciled if CE-5 regolith breccias represent an ancient soil and were excavated from a buried stratigraphic sequence by later impacts. The duration of exposure of this old soil was short (<250 Myr), and its maturation was interrupted by late Eratosthenian basaltic magmatism.

对嫦娥五号(CE-5)任务返回的风化样品中的玄武岩碎屑进行的大量研究,为月球上最年轻岩浆活动的时间和性质提供了限制。然而,对角砾岩的研究却少得多,角砾岩是风化层的主要成分之一。本文对两个CE-5风化角砾岩样品进行了矿物学、岩石学和U-Pb年代学的综合研究,这些样品由岩屑、凝集物、玻璃颗粒和矿物碎片组成。与CE-5高成熟度的风化层相比,该风化层角砾岩较不成熟,胶结度低(~11 vol%),基质含量中低(~49 vol%)。CE-5风化角砾岩主要由母岩(~90 vol%)和非母岩(~10 vol%)组成。在海岩成分中,除了以晚埃拉托色尼玄武岩为主外,还发现了晚因布赖恩世至早埃拉托色尼时期的低钛海岩成分。非mare成分包括Mg-suite norite,高地冲击熔融碎屑,玻璃颗粒和少量破碎矿物。CE-5风化角砾岩中的玻璃颗粒成分多变,可分为玄武岩(mare)、富kreep、长石(highland)、贫si和富si - k玻璃5种类型。在这些玻璃杯中,大多数(65%)在构图上具有异国情调。CE-5角砾岩中这些“外来”物质的不同来源,与3.97 ~ 3.92 Ga、~3.2 Ga、2.93 ~ 2.40 Ga和~2.0 Ga含锆相的多个年龄相一致,其中首次从月球返回样品中报道了早埃拉托斯特尼时代。如果CE-5风化角砾岩是一种古土壤,并且是后期撞击从埋藏的层序中挖掘出来的,那么CE-5风化角砾岩与CE-5风化角砾岩在成熟度和玻璃成分上的差异是可以调和的。该古土壤暴露时间较短(250 Myr),其成熟过程被晚埃拉托色世玄武岩岩浆作用打断。
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Meteoritics & Planetary Science
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