Valence state partitioning of vanadium between olivine-liquid; estimates of the oxygen fugacity of Y980459 and application to other olivine-phyric Martian basalts
Valence state partitioning of vanadium between olivine-liquid; estimates of the oxygen fugacity of Y980459 and application to other olivine-phyric Martian basalts (in Planetary materials; from the Earth to the Moon and beyond; Jim Papike special issue, Charles Shearer (prefacer), David Vaniman (prefacer) and Ted Labotka (prefacer))
American Mineralogist (October 2006) 91 (10): 1657-1663
- achondrites
- basalts
- fugacity
- igneous rocks
- Mars
- Martian meteorites
- melts
- metals
- meteorites
- nesosilicates
- olivine
- olivine group
- orthosilicates
- oxygen
- partitioning
- planets
- rare earths
- shergottite
- silicate melts
- silicates
- SNC Meteorites
- stony meteorites
- terrestrial planets
- trace elements
- valency
- vanadium
- volcanic rocks
- Yamato Meteorites
- Y 980459
The valence state of vanadium (V (super 2+) , V (super 3+) , V (super 4+) , and V (super 5+) ) is highly sensitive to variations in redox conditions of basaltic magmas. Differences in valence state will influence its partitioning behavior between minerals and basaltic liquid. Using partitioning behavior of V between olivine and basaltic liquid precisely calibrated for Martian basalts, we determined the oxidation state of a primitive (olivine-rich, high Mg no.) Martian basalt (Y980459) near its liquidus. The behavior of V in the olivine from other Martian olivine-phyric basalts (SaU005, DaG476, and NWA1110) was documented. The combination of oxidation state and incompatible-element characteristics determined from early olivine indicates that correlations among geochemical characteristics such as f (sub O2) , LREE/HREE, initial (super 87) Sr/ (super 86) Sr, and initial epsilon (sub Nd) observed in many Martian basalts is also a fundamental characteristic of these primitive magmas. These observations are interpreted as indicating that the mantle sources for these magmas have a limited variation in f (sub O2) from IW to IW+1 and are incompatible-element depleted. Moreover, these mantle-derived magmas assimilated a more oxidizing (>IW+3), incompatible-element enriched, lower-crustal component as they ponded at the base of the Martian crust.