Other
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p21a1579p&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P21A-1579
Other
[1027] Geochemistry / Composition Of The Planets, [3630] Mineralogy And Petrology / Experimental Mineralogy And Petrology, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
We present the solidus and near-solidus phase relations experiments performed on a water-saturated Martian model mantle composition using a multi-anvil apparatus over the P range 5-7GPa and 700-1000°C. Furthering the understanding of the effect of water on the differentiation of the early Mars requires the investigation of the melting properties of an undegassed Martian mantle. In particular, water has a significant effect on the solidus temperature, and little is known about the near-solidus behavior in systems chemically equivalent to the Martian mantle at pressures above 4GPa. At 5 and 7 GPa the vapor-saturated solidus lies between 800 and 900°C. A significant amount (about 10wt%) of silicic hydrous melt is present in the 5GPa and 900°C experiment along with several hydrous silicate phases. In addition to olivine, orthopyroxene, clinopyroxene, garnet, spinel and apatite, at least one and possibly two different hydrous phases have been synthesized. One of these hydrous minerals has been tentatively identified as part of the humite group (norbergite and chondrodite) and contains 8 - 9 wt. % H2O. Another tentative hydrous phase most closely resembles hydrous phase E. The presence of these hydrous phases at elevated pressures indicates that previously unknown minerals could be stable to sequester H2O deep in planetary interiors and that hydrous silicates may have been buried deeply in the Martian interior early on its accretionary history. The results also confirm that there are other sources for water storage besides ”nominally anhydrous minerals”. If it is likely that water played a critical role during the formation and differentiation of terrestrial planets, it is not clear from our current understanding of the early history of the evolution of Mars whether water was incorporated during accretion from the solar nebula dust or during a late veneer-type phase. Our study allows further exploration of the first hypothesis that water can be stored during accretion processes. The understanding of water redistribution when the planet progressively heats, melts and degasses and the importance of water degassing as part of the primordial atmospheric history may be the key to understanding the incorporation of water in the interiors of the terrestrial planets.
Grove Timothy L.
Pommier Anne
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