Vaporization and thermodynamics of forsterite-rich olivine and some implications for silicate atmospheres of hot rocky exoplanets

We describe an experimental and theoretical study of olivine [Mg2SiO4 (Fo)-Fe2SiO4 (Fa)] vaporization. The vaporization behavior and thermodynamic properties of a fosterite-rich olivine (Fo(95)Fa(5)) have been explored by high-temperature Knudsen effusion mass spectrometry (KEMS) from 1750 to 2250K. The gases observed (in order of decreasing partial pressure) are Fe, SiO, Mg, O-2 and O. We measured the solidus temperature (similar to 2050K), partial pressures of individual gases, the total vapor pressure, and thermodynamic activities and partial molar enthalpies of MgO, 'FeO', and SiO2 for the Fo(95)Fa(5) olivine. The results are compared to other measurements and models of the olivine system. Our experimental data show olivine vaporizes incongruently. We discuss this system both as a psuedo-binary of Fo-Fa and a psuedo-ternary of MgO-'FeO'-SiO2. Iron/magnesium molar ratios in the sample before (similar to 0.05) and after (similar to 0.04) vaporization are consistent with the small positive deviations from ideality of fayalite (gamma similar to 1.17) in olivine of the composition studied (e.g., Nafziger and Muan, 1967). Our data for olivine+melt confirm prior theoretical models predicting fractional vaporization of Fe relative to Mg from molten silicates (Fegley and Cameron, 1987; Schaefer and Fegley, 2009; Ito et al., 2015). If loss of silicate atmospheres occurs from hot rocky exoplanets with magma oceans the residual planet may be enriched in magnesium relative to iron. (C) 2017 Elsevier Inc. All rights reserved.