Coupled thermal-orbital models show lava planets undergo two-stage migration from ~0.1 AU requiring initial eccentricities >=0.9 and sustained forcing, with migration rate depending on mantle state.
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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.
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Coupled orbital and interior structure evolution of lava planets
Coupled thermal-orbital models show lava planets undergo two-stage migration from ~0.1 AU requiring initial eccentricities >=0.9 and sustained forcing, with migration rate depending on mantle state.
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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.