K and Cl concentrations on the Martian surface determined by the Mars Odyssey Gamma Ray Spectrometer: Implications for bulk halogen abundances in Mars

Details K and Cl concentrations on the Martian surface determined by the Mars Odyssey Gamma Ray Spectrometer: Implications for bulk halogen abundances in Mars K and Cl concentrations on the Martian surface determined by the Mars Odyssey Gamma Ray Spectrometer: Implications for bulk halogen abundances in Mars

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010georl..3712204t&link_type=abstract

Geophysical Research Letters, Volume 37, Issue 12, CiteID L12204

Physics

2

Planetary Sciences: Solid Surface Planets: Composition (1060, 3672), Geochemistry: Planetary Geochemistry (5405, 5410, 5704, 5709, 6005, 6008), Mineralogy And Petrology: Planetary Mineralogy And Petrology (5410), Planetary Sciences: Solid Surface Planets: Origin And Evolution, Planetary Sciences: Solar System Objects: Mars

Scientific paper

Orbital gamma ray spectrometry shows that the Martian surface has a mean Cl/K ratio of 1.3 ± 0.2, indistinguishable from the ratio in CI chondrites (1.28). Although Cl and K fractionate by magma degassing and aqueous processing, during igneous partial melting both elements are highly incompatible. Thus, if the surface Cl/K reflects the bulk crustal value, then the mantle, hence primitive silicate Mars, also has a roughly CI ratio. Martian meteorite data indicate that Cl/Br is also approximately chondritic, suggesting that elements that condensed in the nebula between ˜1000 K (K and Cl) to ˜500 K (Br) are uniformly depleted in Mars at about 0.6 × CI chondrite concentrations. Mars clearly does not contain 0.6 × CI levels of H2O, which would be ˜6 wt%, indicating that Mars was constructed by planetesimals rich in volatile elements, but not in water.

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