Abstract Shergottite meteorites are ultramafic to mafic igneous rocks derived from partial melting of distinct regions of the martian mantle. As such, they trace magmatic processes, including fractional crystallization and mixing processes in Mars. New chalcophile (Cu, Se, Zn, Pb), siderophile (Ni, Co, W), and highly siderophile element (HSE: Au, Re, Pd, Rh, Pt, Ru, Ir, Os) abundance data are reported for sulfide assemblages in a suite of thirteen incompatible trace-element depleted, intermediate and enriched shergottites, along with new whole-rock HSE abundance and 187Os/188Os data for seven shergottites. Sulfide grains in depleted and intermediate shergottites typically have the highest absolute abundances of HSE, with broadly flat CI-chondrite normalized patterns. Enriched shergottite sulfide grains typically have highly variable Au, elevated Pd and Rh and are relatively depleted in Zn, Ir and Os. The new HSE whole-rock data for enriched (Northwest Africa [NWA] 7397, NWA 7755, NWA 11043), and intermediate shergottites (NWA 10961, NWA 11065, NWA 12241, and NWA 12536) are generally consistent with existing 187Os/188Os and HSE abundance data for these geochemical groupings. Enriched shergottites with >1 ppb bulk rock Os have measured 187Os/188Os ranging between 0.1296 and 0.1471, with variable Pd and Pt contents. Intermediate shergottites with >1 ppb bulk rock Os have chondrite-relative proportions of the HSE at ∼0.01 to 0.001 × CI chondrites and 187Os/188Os from 0.1284 and 0.1295. Sulfides are the major host of the HSE, and they control the behavior of the HSE during petrogenetic processes in shergottite magmas, enabling the determination of HSE compatibility for martian magmatism in the order: Os > Ir ≥ Ru ≥≥ Rh ≥ Pd ≥ Re ≥ Pt ≥ Au. Fractionation models of removal of an olivine-dominated cumulate recreate HSE patterns for the whole-rock shergottites. Enriched shergottites are best reproduced by 25 to 30% of fractionation from a degassed parent melt (250 ± 50 ppm of S), whereas depleted and intermediate shergottites can be explained by slightly lower fractionation (10 to 15%) from higher S content parent melts (350 ± 100 ppm of S). Sulfur contents in the melt that are ∼50% higher than these estimates yield earlier S-saturation during fractional crystallization, leading to an abrupt decrease of the more compatible HSE (Ru, Ir, Os), which is not observed. These results indicate that the martian mantle and partial melts derived from it, are probably not anomalously enriched in S, and instead are similar to slightly higher than those of the terrestrial mantle and its partial melts.

中文翻译：

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Shergottite硫化物中的高亲铁元素和火星地幔的硫含量

摘要 Shergottite 陨石是源自火星地幔不同区域部分熔化的超镁铁质至镁铁质火成岩。因此，他们追踪岩浆过程，包括火星的分步结晶和混合过程。报告了硫化物的新亲硫元素（Cu、Se、Zn、Pb）、亲铁元素（Ni、Co、W）和高度亲铁元素（HSE：Au、Re、Pd、Rh、Pt、Ru、Ir、Os）丰度数据一组 13 个不相容的微量元素耗尽、中间和富集的陨石的组合，以及新的全岩 HSE 丰度和 7 个陨石的 187Os/188Os 数据。贫化和中间带状陨石中的硫化物颗粒通常具有最高的 HSE 绝对丰度，具有广泛平坦的 CI 球粒陨石归一化模式。富集的辉石硫化物颗粒通常具有高度可变的金，Pd 和 Rh 升高，Zn、Ir 和 Os 相对缺乏。富集（西北非 [NWA] 7397、NWA 7755、NWA 11043）和中间带状花岗岩（NWA 10961、NWA 11065、NWA 12241 和 NWA 12536）的新 HSE 全岩数据与现有/187O 和这些地球化学分组的 HSE 丰度数据。具有 > 1 ppb 大块岩石 Os 的富集带状长石已测得 187Os/188Os 范围在 0.1296 和 0.1471 之间，具有可变的 Pd 和 Pt 含量。具有 > 1 ppb 大块岩石 Os 的中间带状陨石具有球粒陨石相对比例的 HSE 约为 0.01 到 0.001 × CI 球粒陨石和 187Os/188Os 的 0.1284 和 0.1295。硫化物是 HSE 的主要宿主，它们在 Shergottite 岩浆的成岩过程中控制 HSE 的行为，能够按顺序确定火星岩浆活动的 HSE 兼容性：Os > Ir ≥ Ru ≥ ≥ Rh ≥ Pd ≥ Re ≥ Pt ≥ Au。去除以橄榄石为主的堆积物的分馏模型重建了全岩 Shergottites 的 HSE 模式。从脱气母体熔体（250 ± 50 ppm 的 S）分馏 25% 到 30% 可以最好地重现富集的陨石，而贫化和中间的陨石可以通过从较高 S 含量的母熔体中略低的分馏（10 到 15%）来解释（350 ± 100 ppm 的硫）。熔体中的硫含量比这些估计值高约 50%，在分步结晶过程中会产生较早的 S 饱和度，导致更相容的 HSE（Ru、Ir、Os）突然减少，这是未观察到的。这些结果表明火星地幔和部分熔体来源于它，