Program > Browse abstracts by speaker > Edmund Eric

Planets and moons which form beyond the condensation line of H2O accrete in the presence of significant quantities of water and ice, which results in celestial bodies with outer layers largely composed of ice and mixed compounds of H2O with other elements or molecules. Our understanding of the bulk composition and structure of these bodies is therefore controlled by the chemistry of ice and H2O-rich molecular compounds, for which there is little data at simultaneous high pressures and temperatures. In the present study we perform in situ investigations of the reactivity of He and H2O at high pressures and temperatures using resistively-heated diamond anvil cells and X-ray diffraction at P02.2 (Petra III), providing new constraints on their solubility at planetary interior conditions.