The Lithophile Element Budget of Earth's Core

Abstract The relative composition of Earth's core and mantle were set during core formation. By determining how elements partition between metal and silicate at high pressures and temperatures, measurements of the mantle composition and geophysical observations of the core can be used to understand the mechanisms by which Earth formed. Here we present the results of metal‐silicate partitioning experiments for a range of nominally lithophile elements (Al, Ca, K, Mg, O, Si, Th, and U) and S to 85 GPa and up to 5400 K. With our results and a compilation of literature data, we developed a parameterization for partitioning that accounts for compositional dependencies in both the metal and silicate phases. Using this parameterization in a range of planetary growth models, we find that, in general, lithophile element partitioning into the metallic phase is enhanced at high temperatures. The relative abundances of FeO, SiO2, and MgO in the mantle vary significantly between planetary growth models, and the mantle abundances of these elements can be used to provide important constraints on Earth's accretion. To match Earth's core mass and mantle composition, Earth's building blocks must have been enriched in Fe and depleted in Si compared with CI chondrites. Finally, too little Mg, Si, and O are partitioned into the core for precipitation of oxides to be a major source of energy for the geodynamo. In contrast, several ppb of U can be partitioned into the core at high temperatures, and this energy source must be accounted for in thermal evolution models

A study of dynamics of magma extrusion and investigation of volcanic vapor Final report, 25 Mar. 1966 - 30 Jun. 1967

Modified heat flow model for magma extrusion and volcanic vapo

Experimental Investigation into the Thermal and Magmatic Evolution of Mercury

During the time that the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft was in orbit around the innermost planet, new and exciting results regarding the planets structure, chemical makeup, and diverse surface were revealed, confirming that Mercury is a geochemical endmember among the terrestrial planets. Data from this mission, more specifically data from the X-Ray Spectrometer and Gamma-Ray Spectrometer onboard MESSENGER, has been used to provide insight into the thermal and magmatic evolution of Mercury. This dissertation consists of five chapters that, as a whole, have substantially increased our knowledge about Mercury through a high pressure and high temperature experimental investigation. First, we identified nine distinct geochemical regions that have characteristic major element compositions. We computed silicate and sulfide mineralogy of these regions and petrologically classified them according to IUGS specifications. The diversity of the rocks and minerals on Mercury was then compared to other planetary bodies revealing the wide range in diversity of the mercurian surface. Second, we conducted sink-float experiments on a melt composition similar to the composition of the largest volcanic field on the planet to provide insight into crust formation on Mercury. These results suggested a primary floatation crust composed of graphite is possible given a magma ocean event on Mercury. Third, we experimentally determined the phase assemblages associated with the largest volcanic field on the planet. From this data we were able to provide insight into eruption scenarios that produced the northern volcanic plains on Mercury. Fourth, we determined the sulfide concentration at sulfide saturation in mercurian-like melts by conducting sulfide solubility experiments on a synthetic rock composition matching the northern volcanic plains. These results indicated that the high amounts of sulfur on the surface of Mercury measured by MESSENGER are a direct consequence of the low oxygen fugacity of the planet, which allowed transport of S towards the surface in reducing melts which have a higher carrying capacity for S than oxidized melts. Finally, we investigated the carbon concentration at graphite saturation in Fe-rich metals with various amounts of Si to determine the amount of C that would be soluble in the mercurian core as a function of core composition and temperature. The results of this dissertation provide important information regarding the evolution of Mercury from its primary magma ocean event to the current state of the planet

Concept for a research project in early crustal genesis

Planetary volatiles, physical and chemical planetary evolution, surface processes, planetary formation, metallogenesis, crustal features and their development, tectonics, and paleobiology are discussed

High Pressure- Temperature Electrical Resistivity Experiments on Fe-Si Alloys Bearing on Conductive Heat Flow at the Top of the Outer Core

The electrical resistivity of Fe17wt%Si alloy was measured within the solid and the liquid phases up to 5 GPa in 200 ton and 1000 ton cubic anvil presses. Special attention was paid in the investigation to the challenges in resistance measurements in connection with the contaminations originating from the electrode materials and also the dominant role of the electrode resistances in the final results. The current results on Fe17Si alloys yielded insights to the manifestations of the magnetic, order-disorder and melting transitions on the electrical resistivity at high P, T. A drop in electrical resistivity in Fe17Si was observed at the melting boundary at high pressures up to 5 GPa as reported by Baum et al. (1967) at 1 atm. The liquid resistivity results from the present study provide insight on the effect of Si on the electrical resistivity of Fe-Si alloy specifically that the difference in resistivity between Fe and Fe17Si decreased with increasing pressure. The model of saturation resistivity (Mooij, 1973) describes saturation of electron-scattering where the electron mean free path approaches the interatomic distance (Ioffe-Regel criteria); the temperature coefficient of resistivity (TCR) has been shown to change sign due to compositionally-induced changes to the mean free path and interatomic distance. The results of the present study show that pressure can also provide a mechanism for resistivity saturation and change of TCR sign most likely due to reduction in interatomic distance. The present electrical resistivity results of Fe17Si were interpreted in terms of the resistivity saturation model in order to estimate the electrical resistivity of the Earth’s outer core. This yielded a range of 9.0×10-7Ωm to 9.4×10-7Ωm which is in agreement with the very recently reported studies on the electrical resistivity of the Earth’s core. Using Wiedemann-Franz law, electrical thermal conductivities were calculated to be 103 Wm−1K−1 to 109Wm−1K−1

Compression experiments to 126 GPa and 2500 K and thermal equation of state of Fe3S: Implications for sulphur in the Earth’s core

Pressure-volume-temperature (P-V-T) experiments on tetragonal Fe3S were conducted to 126 GPa and 2500 K in laser-heated diamond anvil cells (DAC) with in-situ X-ray diffraction (XRD). Seventy nine high-T data as well as four 300-K data were collected, based on which new thermal equations of state (EoS) for Fe3S were established. The room-T data together with existing data were fitted to the third order Birch-Murnaghan EoS, which yielded, GPa and with fixed at 377.0 Å3. A constant term in the thermal pressure equation, Pth = , fitted the high-T data well to the highest temperature, which implies that the contributions from the anharmonic and electronic terms should be minor in the thermal pressure term. The high-T data were also fitted to the Mie-Grüneisen-Debye model; with and q fixed at 417 K and 1 respectively. Calculations from the EoS show that crystalline Fe3S at 4000-5500 K is denser than the Earth's outer core and less dense than the inner core. Assuming a density reduction due to melting, liquid Fe3S would meet the outer core density profile, which however suggests that no less than 16 wt%S is needed to reconcile the observed outer core density deficit. The S-rich B2 phase, which was suggested to be a potential liquidus phase of an Fe3S-outer core above 250 GPa, namely the main constituent of its solid inner core, would likely be less dense than the Earth's inner core. As such, while the outer core density requires as much sulphur as 16 wt%, the resulting liquidus phase cannot meet the density of the inner core. Any sulphur-rich composition should therefore be rejected for the Earth's core

Conference on Planetary Volatiles

Initial and present volatile inventories and distributions in the Earth, other planets, meteorites, and comets; observational evidence on the time history of volatile transfer among reservoirs; and volatiles in planetary bodies, their mechanisms of transport, and their relation to thermal, chemical, geological and biological evolution are addressed

Planetary geosciences, 1989-1990

NASA's Planetary Geosciences Programs (the Planetary Geology and Geophysics and the Planetary Material and Geochemistry Programs) provide support and an organizational framework for scientific research on solid bodies of the solar system. These research and analysis programs support scientific research aimed at increasing our understanding of the physical, chemical, and dynamic nature of the solid bodies of the solar system: the Moon, the terrestrial planets, the satellites of the outer planets, the rings, the asteroids, and the comets. This research is conducted using a variety of methods: laboratory experiments, theoretical approaches, data analysis, and Earth analog techniques. Through research supported by these programs, we are expanding our understanding of the origin and evolution of the solar system. This document is intended to provide an overview of the more significant scientific findings and discoveries made this year by scientists supported by the Planetary Geosciences Program. To a large degree, these results and discoveries are the measure of success of the programs