000006837 001__ 6837
000006837 005__ 20240217113550.0
000006837 0247_ $$2DOI$$a10.1051/0004-6361/201833942
000006837 037__ $$aSCART-2024-0093
000006837 100__ $$aHakim, Kaustubh
000006837 245__ $$aCapturing the oxidation of silicon carbide in rocky exoplanetary interiors
000006837 260__ $$c2018
000006837 520__ $$aContext. Theoretical models predict the condensation of silicon carbide around host stars with C/O ratios higher than 0.65 (cf. C/OSun = 0.54), in addition to its observations in meteorites, interstellar medium and protoplanetary disks. Consequently, the interiors of rocky exoplanets born from carbon-enriched refractory material are often assumed to contain large amounts of silicon carbide. Aims. Here we aim to investigate the stability of silicon carbide in the interior of carbon-enriched rocky exoplanets and to derive the reaction leading to its transformation. Methods. We performed a high-pressure high-temperature experiment to investigate the reaction between a silicon carbide layer and a layer representative of the bulk composition of a carbon-enriched rocky exoplanet. Results. We report the reaction leading to oxidation of silicon carbide producing quartz, graphite, and molten iron silicide. Combined with previous studies, we show that in order to stabilize silicon carbide, carbon saturation is not sufficient, and a complete reduction of Fe2+ to Fe0 in a planetary mantle is required, suggesting that future spectroscopic detection of Fe2+ or Fe3+ on the surface of rocky exoplanets would imply the absence of silicon carbide in their interiors.
000006837 594__ $$aNO
000006837 700__ $$avan Westrenen, Wim
000006837 700__ $$aDominik, Carsten
000006837 773__ $$cL6$$pAstronomy & Astrophysics$$v618$$y2018
000006837 8560_ $$fkaustubh.hakim@ksb-orb.be
000006837 85642 $$ahttps://doi.org/10.1051/0004-6361/201833942
000006837 8564_ $$s1191586$$uhttp://publi2-as.oma.be/record/6837/files/Hakim2018SiliconCarbideOxidation.pdf
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000006837 905__ $$apublished in
000006837 980__ $$aREFERD