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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A retrieval technique infers surface gas fluxes from exoplanet spectra via inversion of a photochemical-climate model, demonstrated on synthetic TRAPPIST-1 e data with an Archean-like biosphere.
Water-hydrogen demixing occurs on warm sub-Neptunes with envelope metallicities of 150-700 times solar, including TOI-270 d, implying layered interiors and underestimated bulk metallicities when using fully-miscible models.
In 1D N2-CO2-H2O model atmospheres, increasing background N2 pressure warms the climate under low CO2 via H2O dilution and under high CO2 via H2O loading, while high N2 induces cooling via Rayleigh scattering that can be overwhelmed by enhanced H2O absorption.
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.
WASP-96b shows super-solar metallicity of 2-6x stellar, roughly stellar C/O, tentative SO2 consistent with photochemistry, and an optical slope from scattering aerosols, supporting core-accretion formation beyond the water snowline.
LIFE can constrain atmospheric H2O abundances from roughly 10^{-3} to 1 bar surface pressure on Earth-like exoplanets for certain vertical profiles, providing a potential proxy for surface oceans, but cannot detect water below 10^{-6} bar or precisely characterize the highest abundances.
The paper reviews physical processes, modeling techniques, retrieval methods, and observational strategies for characterizing exoplanet atmospheres, emphasizing Swiss research progress.
citing papers explorer
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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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Toward Inferring the Surface Fluxes of Biosignature Gases on Rocky Exoplanets from Telescope Spectra
A retrieval technique infers surface gas fluxes from exoplanet spectra via inversion of a photochemical-climate model, demonstrated on synthetic TRAPPIST-1 e data with an Archean-like biosphere.
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A window for water-hydrogen demixing on warm metal-rich sub-Neptunes
Water-hydrogen demixing occurs on warm sub-Neptunes with envelope metallicities of 150-700 times solar, including TOI-270 d, implying layered interiors and underestimated bulk metallicities when using fully-miscible models.
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Revisiting the greenhouse effect of non-greenhouse gases in the atmospheres of Earth-like planets
In 1D N2-CO2-H2O model atmospheres, increasing background N2 pressure warms the climate under low CO2 via H2O dilution and under high CO2 via H2O loading, while high N2 induces cooling via Rayleigh scattering that can be overwhelmed by enhanced H2O absorption.
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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.
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Super-Solar Metallicity and Tentative Evidence for Photochemistry on WASP-96b from JWST and Ground-Based VLT Transmission Spectroscopy
WASP-96b shows super-solar metallicity of 2-6x stellar, roughly stellar C/O, tentative SO2 consistent with photochemistry, and an optical slope from scattering aerosols, supporting core-accretion formation beyond the water snowline.
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The Goldilocks problem for detecting water in terrestrial planets: Constraining water abundances in the mid-IR with LIFE
LIFE can constrain atmospheric H2O abundances from roughly 10^{-3} to 1 bar surface pressure on Earth-like exoplanets for certain vertical profiles, providing a potential proxy for surface oceans, but cannot detect water below 10^{-6} bar or precisely characterize the highest abundances.
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NCCR PlanetS: Observational and computational characterization of exoplanet atmospheres
The paper reviews physical processes, modeling techniques, retrieval methods, and observational strategies for characterizing exoplanet atmospheres, emphasizing Swiss research progress.