ELMO · Experimental Laboratory Magma Ocean

Volatile chemical elements such as C, O, H, S, and N, are critical components in the formation and evolution of planets, control physical properties of planet interiors and associated processes such as plate tectonics, largely make up the composition of atmospheres, and determine planet habitability. Telescopic observations of exoplanets provide information about the atmospheres of planets, and the abundances of these volatile elements. However, we lack experimental constraints to reliably interpret atmosphere observations and link them to planet compositions. I propose a novel experimental approach that will provide a quantitative link of atmosphere chemistry and molecular speciation, to magma ocean composition.All terrestrial planets have experienced a magma ocean stage early in their evolution. With my group I will study the role of volatile elements in this planetary stage, and how composition, and oxidation state of magma oceans control the molecular inventory of their atmospheres. This information is crucial to derive primordial atmosphere compositions of solar system planets and constrain their volatile inventories. The new data will be put in the context of ongoing and future European space missions, such as BepiColombo to Mercury, in which I am directly involved. On the other hand, with the proposed experimental approach I will build a link from observed volatile species in exoplanet atmospheres to the compositions of the interiors of hot magma ocean worlds. The novel data will be directly integrated with observations from spectroscopic measurements of exoplanet atmospheres by JWST and the planned ESA Ariel mission to constrain planet compositions. By comparing the derived magma ocean atmosphere of Earth with the atmospheres of observed hot exoplanets, I will be able to assess how common systems like the early Earth are, beyond the solar system.