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Geochemistry of Martian Meteorites and the Petrologic Evolution of MarsMafic igneous rocks serve as probes of the interiors of their parent bodies - the compositions of the magmas contain an imprint of the source region composition and mineralogy, the melting and crystallization processes, and mixing and assimilation. Although complicated by their multifarious history, it is possible to constrain the petrologic evolution of an igneous province through compositional study of the rocks. Incompatible trace elements provide one means of doing this. I will use incompatible element ratios of martian meteorites to constrain the early petrologic evolution of Mars. Incompatible elements are strongly partitioned into the melt phase during igneous processes. The degree of incompatibility will differ depending on the mineral phases in equilibrium with the melt. Most martian meteorites contain some cumulus grains, but nevertheless, incompatible element ratios of bulk meteorites will be close to those of their parent magmas. ALH 84001 is an exception, and it will not be discussed. The martian meteorites will be considered in two groups; a 1.3 Ga group composed of the clinopyroxenites and dunite, and a younger group composed of all others.
Document ID
20020090125
Acquisition Source
Johnson Space Center
Document Type
Conference Paper
Authors
Mittlefehldt, D. W.
(NASA Johnson Space Center Houston, TX United States)
Date Acquired
August 20, 2013
Publication Date
January 1, 2002
Publication Information
Publication: Unmixing the SNCs: Chemical, Isotopic, and Petrologic Components of the Martian Meteorites
Subject Category
Lunar And Planetary Science And Exploration
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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