The chlorine isotopic composition of Martian meteorites 1: Chlorine isotope composition of Martian mantle and crustal reservoirs and their interactions

The Martian meteorites record a wide diversity of environments, processes, and ages. Much work has been done to decipher potential mantle sources for Martian magmas and their interactions with crustal and surface environments. Chlorine isotopes provide a unique opportunity to assess interactions bet...

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Bibliographic Details
Published in:Meteoritics & planetary science 2016-11, Vol.51 (11), p.2092-2110
Main Authors: Williams, J. T., Shearer, C. K., Sharp, Z. D., Burger, P. V., McCubbin, F. M., Santos, A. R., Agee, C. B., McKeegan, K. D.
Format: Article
Language:English
Subjects:
Age
Breccia
Chlorine
Chlorine isotopes
Crusts
Crystallization
Enrichment
Fractional crystallization
Isotope composition
Isotopes
Magma
Mantle
Mars environment
Martian meteorites
Meteorites
Meteors & meteorites
Nakhlites
Olivine
Planetary mantles
Regolith
Reservoirs
Shergottites
SNC meteorites
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Summary:The Martian meteorites record a wide diversity of environments, processes, and ages. Much work has been done to decipher potential mantle sources for Martian magmas and their interactions with crustal and surface environments. Chlorine isotopes provide a unique opportunity to assess interactions between Martian mantle‐derived magmas and the crust. We have measured the Cl‐isotopic composition of 17 samples that span the range of known ages, Martian environments, and mantle reservoirs. The 37Cl of the Martian mantle, as represented by the olivine‐phyric shergottites, NWA 2737 (chassignite), and Shergotty (basaltic shergottite), has a low value of approximately −3.8‰. This value is lower than that of all other planetary bodies measured thus far. The Martian crust, as represented by regolith breccia NWA 7034, is variably enriched in the heavy isotope of Cl. This enrichment is reflective of preferential loss of 35Cl to space. Most basaltic shergottites (less Shergotty), nakhlites, Chassigny, and Allan Hills 84001 lie on a continuum between the Martian mantle and crust. This intermediate range is explained by mechanical mixing through impact, fluid interaction, and assimilation‐fractional crystallization.
ISSN:1086-9379
1945-5100
DOI:10.1111/maps.12647