Forsterite/melt partitioning of argon and iodine: Implications for atmosphere formation by outgassing of an early Martian magma ocean

Details Forsterite/melt partitioning of argon and iodine: Implications for atmosphere formation by outgassing of an early Martian magma ocean Forsterite/melt partitioning of argon and iodine: Implications for atmosphere formation by outgassing of an early Martian magma ocean

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992pcmo.work...40m&link_type=abstract

In Lunar and Planetary Inst., Workshop on the Physics and Chemistry of Magma Oceans from 1 Bar to 4 Mbar p 40-41 (SEE N92-28587

Physics

Argon, Forsterite, Iodine Isotopes, Magma, Mars (Planet), Mars Atmosphere, Outgassing, Planetary Mantles, Planetary Structure, Radiogenic Materials, Half Life, Meteorites, Oceans, Signatures, Solar System, Solubility, Water, Xenon 129

Scientific paper

Argon and Xe in the Martian atmosphere are radiogenic relative to the Martian mantle if the SNC meteorites are from Mars. Decay of the short lived isotope I-129 to Xe-129 (t sub 1/2 = 16 m.y.) is the most plausible source of the radiogenic Xe. This short half life constrains any process responsible for the elevated Xe-129/Xe-132 ratio of the Martian atmosphere to occur very early in solar system history. Musselwhite et al. proposed that the differential solubility of I and Xe in liquid water played a key role in producing the radiogenic signature in the Martian atmosphere. Here we explore an alternative hypothesis involving purely igneous processes, and motivated in part by new experimental results on the partitioning of I and Xe between minerals and melt.

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