| タイトル | Definitive Mineralogical Analysis of Martian Rocks and Soil Using the CheMin XRD/XRF Instrument and the USDC Sampler |
| 著者（英） | Chipera, S. J.; Sarrazin, P.; Sherrit, S.; Bar-Cohen, Y.; Bish, D. L.; Bryson, C.; Blake, D. F.; Collins, S.; Vaniman, D. T.; Boyer, B. |
| 著者所属（英） | NASA Ames Research Center |
| 発行日 | 2003-01-01
2003 |
| 言語 | eng |
| 内容記述 | The search for evidence of extant or extinct life on Mars will initially be a search for evidence of present or past conditions supportive of life (e.g., evidence of water), not for life itself. Definitive evidence of past or present water activity lies in the discovery of: * Hydrated minerals: The "rock type" hosting the hydrated minerals could be igneous, metamorphic, or sedimentary, with only a minor hydrated mineral phase. Therefore, the identification of minor phases is important. * Clastic sediments: Clastic sediments are commonly identified by the fact that they contain minerals of disparate origin that could only have come together as a mechanical mixture. Therefore, the identification of all minerals present in a mixture to ascertain mineralogical source regions is important. * Hydrothermal precipitates and chemical sediments: Some chemical precipitates are uniquely identified only by their structure. For example, Opal A, Opal CT, tridymite, crystobalite, high and low Quartz all have the same composition (SiO2) but different crystal structures indicative of different environments - from hydrothermal hydrothermal formation to low temperature precipitation. Other silica types such as stishovite can provide evidence of shock metamorphism. Therefore, identification of crystal structures and structural polymorphs is important. The elucidation of the nature of the Mars soil will require the identification of mineral components that can unravel its history and the history of the Mars atmosphere. |
| NASA分類 | Lunar and Planetary Science and Exploration |
| 権利 | Copyright, Distribution under U.S. Government purpose rights |
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