Iron isotopes of Chang'e-5 soil and mineral components: Implications for post-eruption processes on lunar surface

IF 2.5 2区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Icarus Pub Date : 2024-10-29 DOI:10.1016/j.icarus.2024.116362
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Abstract

Due to rapid magma cooling and extensive space weathering, significant disequilibrium crystallization and secondary modification widely occur in lunar mare basalt after its eruption on the lunar surface. In this study, we conducted bulk and in-situ Fe isotope analyses to investigate the post-eruption processes on Chang'e-5 (CE-5) samples. The CE-5 soil shows a minor elevation of δ56Fe value (∼0.05 ‰) relative to the CE-5 basalt clasts. Correlations between Ni and Cu contents with δ56Fe values suggest that the minor increase in the δ56Fe from the CE-5 basalt to soil primarily occurred during evaporation caused by meteorite impacts. Such isotopic variation between CE-5 basalt and soils is notably lower than what is observed for Apollo samples and reflects the low maturity of CE-5 soils. This is consistent with the low Is/FeO value constrained by magnetic approaches. Therefore, measuring the δ56Fe values of lunar soil is suitable to evaluate the degrees of maturity for lunar soils due to space weathering. In-situ analyses of δ56Fe reveal significant variations in different grains of olivine (δ56Fe: −0.57 to −0.17 ‰) and ilmenite (−0.06 to +0.42 ‰) and also in their interior (mainly for olivine). These δ56Fe variations in minerals can be ascribed to the disequilibrium crystallization of lava flow and fast cooling, which is consistent with conclusions based on petrologic observations such as its extensive differentiation and silicate liquid immiscibility. Therefore, the post-eruption processes on the lunar surface could lead to significant variations in isotopic compositions at different scales of basalts, which in turn record the history of late-stage magma evolution and space weathering on the lunar surface.
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嫦娥五号土壤和矿物成分的铁同位素:对月球表面爆发后过程的影响
由于岩浆的快速冷却和广泛的空间风化作用,月壤玄武岩在月面喷发后普遍发生了严重的不平衡结晶和二次改造。在本研究中,我们对嫦娥五号(CE-5)样品进行了散装和原位铁同位素分析,以研究其喷发后的过程。与嫦娥五号玄武岩碎屑相比,嫦娥五号土壤中的δ56Fe值略有升高(∼0.05 ‰)。镍和铜含量与δ56Fe值之间的相关性表明,从CE-5玄武岩到土壤的δ56Fe的微小增加主要发生在陨石撞击引起的蒸发过程中。CE-5 玄武岩和土壤之间的这种同位素变化明显低于阿波罗样本,反映了 CE-5 土壤的低成熟度。这与磁性方法得出的低Is/FeO值是一致的。因此,测量月球土壤的 δ56Fe 值适用于评估空间风化造成的月球土壤成熟度。δ56Fe的原位分析显示,橄榄石(δ56Fe:-0.57至-0.17‰)和钛铁矿(-0.06至+0.42‰)的不同晶粒及其内部(主要是橄榄石)存在显著差异。矿物中的δ56Fe变化可归因于熔岩流的不平衡结晶和快速冷却,这与根据岩石学观察得出的结论是一致的,如熔岩流的广泛分异和硅酸盐液的不溶性。因此,月球表面爆发后的过程可能导致不同尺度玄武岩同位素组成的显著变化,进而记录了月球表面后期岩浆演化和空间风化的历史。
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来源期刊
Icarus
Icarus 地学天文-天文与天体物理
CiteScore
6.30
自引率
18.80%
发文量
356
审稿时长
2-4 weeks
期刊介绍: Icarus is devoted to the publication of original contributions in the field of Solar System studies. Manuscripts reporting the results of new research - observational, experimental, or theoretical - concerning the astronomy, geology, meteorology, physics, chemistry, biology, and other scientific aspects of our Solar System or extrasolar systems are welcome. The journal generally does not publish papers devoted exclusively to the Sun, the Earth, celestial mechanics, meteoritics, or astrophysics. Icarus does not publish papers that provide "improved" versions of Bode''s law, or other numerical relations, without a sound physical basis. Icarus does not publish meeting announcements or general notices. Reviews, historical papers, and manuscripts describing spacecraft instrumentation may be considered, but only with prior approval of the editor. An entire issue of the journal is occasionally devoted to a single subject, usually arising from a conference on the same topic. The language of publication is English. American or British usage is accepted, but not a mixture of these.
期刊最新文献
Large impact features on Ganymede and Callisto as revealed by geological mapping and morphometry Baroclinic waves observed on Mars from InSight data Iron isotopes of Chang'e-5 soil and mineral components: Implications for post-eruption processes on lunar surface Three-dimensional modeling of Ganymede’s Chapman–Ferraro magnetic field and its role in subsurface ocean induction Seasonal and interannual variability of the water vapor vertical distribution in the Martian lower atmosphere
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