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Theoretical models predict the condensation of silicon carbide around hoststars with C/O ratios higher than 0.65 (cf. C/O$_{\mathrm{Sun}}$ = 0.54), inaddition to its observations in meteorites, interstellar medium andprotoplanetary disks. Consequently, the interiors of rocky exoplanets born fromcarbon-enriched refractory material are often assumed to contain large amountsof silicon carbide. Here we aim to investigate the stability of silicon carbidein the interior of carbon-enriched rocky exoplanets and to derive the reactionleading to its transformation. We performed a high-pressure high-temperatureexperiment to investigate the reaction between a silicon carbide layer and alayer representative of the bulk composition of a carbon-enriched rockyexoplanet. We report the reaction leading to oxidation of silicon carbideproducing quartz, graphite, and molten iron silicide. Combined with previousstudies, we show that in order to stabilize silicon carbide, carbon saturationis not sufficient, and a complete reduction of Fe$^{2+}$ to Fe$^{0}$ in aplanetary mantle is required, suggesting that future spectroscopic detection ofFe$^{2+}$ or Fe$^{3+}$ on the surface of rocky exoplanets would imply theabsence of silicon carbide in their interiors.

Capturing the oxidation of silicon carbide in rocky exoplanetary interiors