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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POSEIDON now includes lab-derived rocky surface albedos, enabling JWST emission spectra to separate thin versus thick atmospheres and potentially identify granite-like versus basaltic surfaces.
Accounting for stellar and orbital uncertainties shows that predicted eclipse depths for bare-rock models of rocky exoplanets carry substantial uncertainty comparable to measurements, establishing a fundamental precision limit for atmospheric and compositional inferences.
citing papers explorer
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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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The Rocky Planet Picture Show: Implementation of Surface Reflection and Emission in $\texttt{POSEIDON}$ with Application to and Interpretation of JWST Data
POSEIDON now includes lab-derived rocky surface albedos, enabling JWST emission spectra to separate thin versus thick atmospheres and potentially identify granite-like versus basaltic surfaces.
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Uniform Reinterpretation of Rocky Exoplanet Secondary Eclipse Observations and the Impact of Stellar and Orbital Uncertainties
Accounting for stellar and orbital uncertainties shows that predicted eclipse depths for bare-rock models of rocky exoplanets carry substantial uncertainty comparable to measurements, establishing a fundamental precision limit for atmospheric and compositional inferences.