3D GCM simulations favor a thick (>=10 bar), CO2-rich (>1% mixing ratio) atmosphere for 55 Cancri e that matches JWST spectra while ruling out thin or CO/CO2-poor cases.
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Simulations indicate that order-of-magnitude changes in TiO2 and SiO2 abundances in lava melts produce distinguishable TiO, SiO, and SiO2 features in dry lava planet emission spectra, potentially observable with 12 JWST eclipses for the brightest targets.
citing papers explorer
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Reinterpreting the JWST Observations of 55 Cancri e with a Non-Grey General Circulation Model
3D GCM simulations favor a thick (>=10 bar), CO2-rich (>1% mixing ratio) atmosphere for 55 Cancri e that matches JWST spectra while ruling out thin or CO/CO2-poor cases.
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Sensitivity of Dry Lava Planet Atmospheric Emission Spectra to Changes in Lava Compositions
Simulations indicate that order-of-magnitude changes in TiO2 and SiO2 abundances in lava melts produce distinguishable TiO, SiO, and SiO2 features in dry lava planet emission spectra, potentially observable with 12 JWST eclipses for the brightest targets.