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Are Small Differences in Phosphorous Content Responsible for Large Differences in the Composition of Terrestrial and Martian Magmatic Rocks
| Content Provider | Semantic Scholar |
|---|---|
| Author | Toplis, Michael J. Baratoux, David Gasnault, Olivier Pinet, P. C. Belin, Esther Roche, Claude |
| Copyright Year | 2008 |
| Abstract | analyses at the hand-sample scale performed by land-ers or rovers at the Martian surface (e.g. Viking, Path-finder, MER), orbital measurements at the planetaryscale (e.g. the Gamma Ray Spectrometer onboard MarsOdyssey, or the OMEGA instrument onboard MarsExpress) and the Shergottite-Nakhlite-Chassignite(SNC) group of meteorites generally accepted to be ofMartian origin. The quantity and quality of the dataavailable has increased dramatically over the past fewyears, providing unprecedented insight into the detailsof the chemistry and mineralogy of Martian rocks.When all data are considered, it is immediately appar-ent that rocks from Mars show many important differ-ences compared to their Terrestrial counterparts. Forexample, one of the most striking features of volcanicrocks from Mars is that they are significantly richer iniron and poorer in silica than lavas produced by partialmelting of the Earth's mantle. The iron-rich nature ofMartian volcanics has been attributed to a higher FeOcontent of the Martian mantle compared to that of theEarth [1], while the low silica content has no widelyaccepted explanation. It is also of note that the SNCmeteorites generally show superchondritic Ca/Al, anobservation which contrasts with most terrestrial ba-salts, and which places constraints on the compositionof the mantle source which produced the SNC's [2]. |
| File Format | PDF HTM / HTML |
| Alternate Webpage(s) | https://www.lpi.usra.edu/meetings/lpsc2008/pdf/1282.pdf |
| Language | English |
| Access Restriction | Open |
| Content Type | Text |
| Resource Type | Article |
