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首页> 外文期刊>Earth and Planetary Science Letters: A Letter Journal Devoted to the Development in Time of the Earth and Planetary System >The evolution of a heterogeneous Martian mantle: Clues from K, P, Ti, Cr, and Ni variations in Gusev basalts and shergottite meteorites
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The evolution of a heterogeneous Martian mantle: Clues from K, P, Ti, Cr, and Ni variations in Gusev basalts and shergottite meteorites

机译：异质火星地幔的演化：古塞夫玄武岩和黑云母陨石中K，P，Ti，Cr和Ni变化的线索

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摘要

Martian basalts represent samples of the interior of the planet, and their composition reflects their source at the time of extraction as well as later igneous processes that affected them. To better understand the composition and evolution of Mars, we compare whole rock compositions of basaltic shergottitic meteorites and basaltic lavas examined by the Spirit Mars Exploration Rover in Gusev Crater. Concentrations range from K-poor (as low as 0.02wt.% K_2O) in the shergottites to K-rich (up to 1.2wt.% K_2O) in basalts from the Columbia Hills (CH) of Gusev Crater; the Adirondack basalts from the Gusev Plains have more intermediate concentrations of K_2O (0.16wt.% to below detection limit). The compositional dataset for the Gusev basalts is more limited than for the shergottites, but it includes the minor elements K, P, Ti, Cr, and Ni, whose behavior during mantle melting varies from very incompatible (prefers melt) to very compatible (remains in the residuum). The range in partitioning behavior of these elements provides leverage on interpreting igneous processes. Models are presented that demonstrate how concentrations of these elements in Gusev basaltic magmas would change by simple igneous processes (fractional crystallization, crustal contamination, and mantle partial melting). The Gusev basalts may be related by two-stage batch melting of a primitive (K-rich) mantle source to first, generate the K-rich, Columbia Hills basalts and second, the lower K Adirondack basalts, leaving behind a K-poor residuum. The mantle source for the Gusev basalts is separate from the more depleted (K-poorer) source region of the shergottites. This indicates that primitive, K-rich mantle persisted until the Early Hesperian during formation of the Columbia Hills basalts. We suggest that separate mantle reservoirs developed by inhomogeneous partial melting (at melt fractions greater than 0.05) to form the Martian crust in the first 1Ga of the planet's history.
机译：火星玄武岩代表了行星内部的样本，其成分反映了提取时的来源以及后来影响它们的火成岩过程。为了更好地了解火星的组成和演化，我们比较了Gusev Crater的Spirit Mars Exploration Rover检测的玄武质滑石陨石和玄武熔岩的整个岩石组成。浓度范围从钙铁矿中的贫K（低至0.02wt。％K_2O）到来自Gusev Crater哥伦比亚山（CH）的玄武岩中的富K（至1.2wt。％K_2O）。 Gusev平原的阿迪朗达克玄武岩的K_2O的中间浓度更高（0.16wt。％，低于检出限）。 Gusev玄武岩的成分数据集比斜方岩更为有限，但它包含微量元素K，P，Ti，Cr和Ni，它们在地幔融化过程中的行为从极不相容（首选熔体）到极相容（剩余）在残留物中）。这些元素的分区行为范围为解释火成过程提供了影响。提出的模型证明了古塞夫玄武岩浆中这些元素的浓度将通过简单的火成过程（分形结晶，地壳污染和地幔部分熔融）而改变。古塞夫玄武岩可能与原始（富含钾）地幔源的两阶段批熔有关，首先是生成富含钾的哥伦比亚希尔斯玄武岩，其次是下部阿迪朗达克钾玄武岩，而留下贫钾的残渣。 Gusev玄武岩的地幔源与斜方矿的贫化（钾贫）源区分开。这表明原始的富含钾的地幔一直持续到哥伦比亚山玄武岩形成期间的早黑斯佩里亚时期。我们建议通过不均匀的局部熔融（熔融分数大于0.05）形成的单独的地幔储层在地球历史上的第一个1Ga中形成火星地壳。

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