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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4 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
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astro-ph.EP 4years
2026 4representative citing papers
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.
A Python port of a classic volcanic plume model is applied to exoplanet conditions, identifying parameter regions where plumes reach low-pressure altitudes and become potentially detectable.
Archival MIRI imaging reaches contrasts of 10^-3 to 10^-4 at 1-3 arcseconds, enabling detection of ~170 K Jupiter-sized planets at separations >35 AU around M-dwarfs at 12.5 pc, with no new planets found but useful sensitivity maps produced.
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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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.
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Modeling Volcanic Plume Heights Across Exoplanet Atmospheres: Insights from TRAPPIST-1
A Python port of a classic volcanic plume model is applied to exoplanet conditions, identifying parameter regions where plumes reach low-pressure altitudes and become potentially detectable.
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A Search for Wide-orbit Planets Around M-dwarfs using Deep MIRI 15-micron Images
Archival MIRI imaging reaches contrasts of 10^-3 to 10^-4 at 1-3 arcseconds, enabling detection of ~170 K Jupiter-sized planets at separations >35 AU around M-dwarfs at 12.5 pc, with no new planets found but useful sensitivity maps produced.