| タイトル | Metal-Silicate Partitioning of Bi, In, and Cd as a Function of Temperature and Melt Composition |
| 本文（外部サイト） | http://hdl.handle.net/2060/20130004244 |
| 著者（英） | Marin, Nicole; Danielson, L.; Pando, K.; Righter, K.; Lee, C. |
| 著者所属（英） | NASA Johnson Space Center |
| 発行日 | 2013-01-01 |
| 言語 | eng |
| 内容記述 | The origin of volatile elements in the Earth, Moon and Mars is not known; however, several theories have been proposed based on volatile elements such as In, As, Se, Te and Zn which are in lower concentration in the Earth, Moon, and Mars than in chondrites. Explanations for these low concentrations are based on two contrasting theories for the origin of Earth: equilibrium core formation versus late accretion. One idea is that the volatiles were added during growth of the planets and Moon, and some mobilized into the metallic core while others stayed in the mantle (e.g., [1]). The competing idea is that they were added to the mantles after core formation had completed (e.g., [2]). Testing these ideas involves quantitative modeling which can only be performed after data is obtained on the systematic metal-silicate partitioning behavior of volatile elements with temperature, pressure and melt composition. Until now, such data for Bi, In, and Cd has been lacking. After conducting a series of high pressure, high temperature experiments, the metal-silicate partition coefficients of Bi, In, and Cd as a function of temperature and melt composition can be used to evaluate potential conditions under which terrestrial planets differentiated into core and mantle, and how they acquired volatiles. |
| NASA分類 | Lunar and Planetary Science and Exploration |
| レポートNO | JSC-CN-27951 |
| 権利 | Copyright, Distribution as joint owner in the copyright |
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