The effect of Fe on olivine H (sub 2) O storage capacity; consequences for H (sub 2) O in the Martian mantle

To investigate the influence of chemical composition on the behavior of H (sub 2) O in Fe-rich nominally anhydrous minerals, and to determine the difference between H (sub 2) O behavior in the martian and terrestrial mantles, we conducted high-pressure H (sub 2) O storage capacity experiments employing a wide range of olivine compositions. Experiments were conducted with bulk compositions in the system FeO-MgO-SiO (sub 2) -H (sub 2) O with Mg no. [Mg no.=100Xmolar Mg/(Mg+Fe)] ranging between 50 and 100 at 3 GPa in a piston-cylinder and at 6 GPa in a multi-anvil apparatus. Experiments at 3 GPa were conducted at 1200 degrees C, with f (sub O2) buffered by the coexistence of Fe and FeO, and at 1300-1500 degrees C in unbuffered assemblies. Experiments at 6 GPa were conducted at 1200 degrees C without buffers. Experiments at 1200 degrees C produced olivine+orthopyroxene+hydrous liquid (liq), and higher T experiments produced olivine+liq. Additionally, we synthesized a suite of 7 olivine standards (Mg no.=90) for low blank secondary ion mass spectrometry (SIMS) analysis of H in multi-anvil experiments at 3-10 GPa and 1250 degrees C, resulting in large (200-400 mu m) homogeneous crystals with 0.037 to 0.30 wt% H (sub 2) O. Polarized Fourier transform infrared (FTIR) measurements on randomly oriented grains from the synthesis experiments were used to determine principal axis spectra through least-squares regression, and H contents were calculated from the total absorbance in the OH stretching region. Using these olivines as calibrants for SIMS analyses, the H contents of olivines and pyroxenes from the variable Mg no. experiments were measured by counting (super 16) OH ions. Ignoring any matrix effects owing to variation in Mg no., H contents of olivine and pyroxene increase linearly with decreasing Mg no. At 6 GPa and 1200 degrees C, olivine H contents increase from 0.05 to 0.13 wt% H (sub 2) O (8360 to 23 900 H/10 (super 6) Si) as olivine Mg no. decreases from 100 to 68, and at 3 GPa and 1200 degrees C olivine H contents increase from 0.017 to 0.054 wt% (278 to 10 000 H/10 (super 6) Si) as Mg no. decreases from 100 to 55. The partition coefficient for H between pyroxene and olivine, D (sub H) (super opx/ol) , decreases from 1.05 at 3 GPa and 1200 degrees C to 0.61 at 6 GPa and 1200 degrees C. The storage capacity of Fe-rich olivines with compositions expected in the martian mantle is approximately 1.5 times greater than those in the terrestrial mantle, suggesting that the geochemical behavior of H (sub 2) O in the mantles of the two planets are quite similar. If 50% of the K (sub 2) O on Mars remains in its mantle (Taylor et al. 2006), then a similar or greater proportion of the H (sub 2) O is also in the mantle. Given accretionary models of the total martian H (sub 2) O budget (Lunine et al. 2003), this suggests concentrations of 100-500 ppm H (sub 2) O in the martian mantle and 0.1-1.9 wt% H (sub 2) O in primary martian basalts.