New computed rates for excited S(1D) and SO(1Δ) plus a 1 ppm near-surface atomic sulfur source improve photochemical modeling of sulfur species in Venus and exo-Venus atmospheres.
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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.
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.
citing papers explorer
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A Comprehensive Sulfur Chemistry Network Including Excited S(1D) and SO(1{\Delta}) for the XODIAC Photochemical Model: Accounting for Missing Sulfur Processes in Venus and Exo-Venus Analogs
New computed rates for excited S(1D) and SO(1Δ) plus a 1 ppm near-surface atomic sulfur source improve photochemical modeling of sulfur species in Venus and exo-Venus atmospheres.
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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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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.