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On the weathering of Martian igneous rocksBesides the young crystallization age, one of the first arguments for the martian origin of shergottite, nakhlite, and chassignite (SNC) meteorites came from the chemical similarity of the meteorite Shergotty and the martian soil as measured by Viking XRF analyses. In the meantime, the discovery of trapped rare gas and nitrogen components with element and isotope ratios closely matching the highly characteristic ratios of the Mars atmosphere in the shock glasses of shergottite EETA79001 was further striking evidence that the SNC's are martian surface rocks. The martian soil composition as derived from the Viking mission, with its extremely high S and Cl concentrations, was interpreted as weathering products of mafic igneous rocks. The low SiO2 content and the low abundance of K and other trace elements in the martian soils point to a mafic crust with a considerably smaller degree of fractionation compared to the terrestrial crust. However, the chemical evolution of the martian regolith and soil in respect to surface reaction with the planetary atmosphere or hydrosphere is poorly understood. A critical point in this respect is that the geochemical evidence as derived from the SNC meteorites suggests that Mars is a very dry planet that should have lost almost all its initially large water inventory during its accretion.
Document ID
19930022752
Acquisition Source
Legacy CDMS
Document Type
Other
Authors
Dreibus, G.
(Max-Planck-Inst. fuer Chemie Mainz, Germany)
Waenke, H.
(Max-Planck-Inst. fuer Chemie Mainz, Germany)
Date Acquired
September 6, 2013
Publication Date
September 12, 1992
Publication Information
Publication: Lunar and Planetary Inst., MSATT Workshop on Chemical Weathering on Mars
Subject Category
Lunar And Planetary Exploration
Accession Number
93N31941
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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