To assess the viability of sulfide liquid saturation during crystallization of the lunar magma ocean (LMO), we present a new data set describing both the sulfur (S) concentration at sulfide liquid saturation (SCSS) and sulfide liquid‐silicate melt partition coefficients of many trace elements for various differentiated lunar magmas at lunar‐relevant conditions. Using these parameterizations, we model the SCSS and the distribution of the most chalcophile elements with progressive LMO crystallization in the absence and presence of sulfide liquids. Modeling results for different modes of LMO crystallization show that for proposed lunar mantle S abundances FeS sulfide liquid saturation is expected to occur between 96% and 98% of LMO crystallization. This is decreased to >91% for Fe‐S liquids with 30% Ni or Cu. Saturation of S‐poor sulfide liquids can occur at >75% of LMO crystallization. The timing of sulfide liquid saturation depends most strongly on the assumed S content of the lunar mantle following formation of the lunar core and on the sulfide liquid composition. Modeled abundances of chalcophile elements indicate that sulfide‐liquid saturation during late‐stage LMO crystallization would yield much lower abundances of Ni and Cu than observed in KREEP basalts and estimated for the urKREEP reservoir, as well as lower Ni/Co than observed in the latter. Sulfide liquids therefore did not affect moderately siderophile and chalcophile element fractionation within the LMO, supporting the hypothesis that the nonvolatile, siderophile element abundances of the lunar mantle reflect a phase of core formation and/or the addition of a meteoritic late veneer.

中文翻译：

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登月岩浆海洋结晶过程中硫和硫属元素的命运

为了评估月球岩浆海洋（LMO）结晶过程中硫化物液体饱和度的可行性，我们提供了一个新的数据集，描述了硫化物液体饱和度（SCSS）时的硫（S）浓度和许多硫化物液体-硅酸盐熔体分配系数月球相关条件下各种不同月球岩浆的微量元素。使用这些参数化，我们可以在不存在和存在硫化物液体的情况下，通过渐进的LMO结晶对SCSS和大多数亲硫族元素的分布进行建模。LMO结晶不同模式的模型结果表明，对于拟议的月幔S丰度，预计FeS硫化物液体饱和会发生在LMO结晶的96％至98％之间。对于含30％Ni或Cu的Fe‐S液体，其降低到> 91％。贫LMO结晶的> 75％时会发生S贫硫化物液体的饱和。硫化物液体饱和的时机最强烈地取决于在形成月球核心之后所假定的月球地幔中的S含量以及硫化物液体成分。模拟的嗜硫元素丰度表明，晚期LMO结晶过程中的硫化物-液体饱和会比KREEP玄武岩和urKREEP储层中估计的Ni和Cu丰度低得多，并且比后者要低。 。因此，硫化物液体不会对LMO中的嗜铁粒和嗜硫粒成分产生适度的影响，支持以下假设：月球幔的非挥发性嗜铁粒元素丰度反映了岩心形成的阶段和/或陨石后期单板的添加。