Origin of the depletion of siderophile volatile elements in Earth, Mars and the aubrite parent body

关于类地行星的组成和演化的新数据表明，目前地球上青睐的非均质吸积模式，即先吸积还原的挥发分贫质，然后再吸积氧化的挥发分富物质，可能并不普遍适用。火星，可能还有水星，具有与地球相似或更高的中等挥发性元素的丰度，并可能在地球完成吸积之前就已经聚积。让事情更复杂的是，地球上高挥发性元素的丰度可能比火星上的高。核心形成后未分化物质的后期积累(后期单板)对类地行星挥发性元素收支的作用尚不清楚。高度亲铁元素的丰度表明，地球、月球、火星和一些分化的陨石母体都受到了晚期陨石的影响。在这里，将获得新的亲铁挥发性元素(S、Se、Te、Cd、Tl、Cu、Ag、In、Pb)的浓度数据，以研究岩芯形成和晚期单板的组成对硅酸盐地球、火星和奥镁石母体内挥发性元素丰度的影响(汞的模型？)。这些数据将与其他挥发性元素的数据和实验研究一起使用，以获得对类地行星中挥发性元素分布的新见解。

New data on the composition and evolution of the terrestrial planets suggest that the heterogeneous accretion model currently favored for Earth, accretion of reduced, volatile poor material followed by oxidized, volatile rich material, may not be generally applicable. Mars, and possibly also Mercury, have similar or higher abundances of moderately volatile elements than Earth, and may have accreted before accretion of Earth was completed. To complicate matters, abundances of highly volatile elements in Earth may be higher than in Mars. The role of late accretion of undifferentiated material after core formation (late veneer) for the volatile element budget of the terrestrial planets remains unclear. Abundances of highly siderophile elements indicate that Earth, Moon, Mars and parent bodies of some differentiated meteorites all have been affected by a late veneer. Here, new concentration data of siderophile volatile elements (S, Se, Te, Cd, Tl, Cu, Ag, In, Pb) will be obtained to study the influence of core formation and the composition of the late veneer on abundances of volatile elements in the silicate earth, Mars, and in the aubrite parent body (a model for Mercury?). The data will be used with data for other volatile elements and experimental studies to obtain new insights into the distribution of volatile elements in the terrestrial planets.