LIFE mission simulations show that baselines of 25-80 m or even discrete values can achieve planet yield and fringe tracking with less than 10% performance loss compared to wider ranges.
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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.
citing papers explorer
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A preliminary exploration of the effects of baseline length for the LIFE space mission
LIFE mission simulations show that baselines of 25-80 m or even discrete values can achieve planet yield and fringe tracking with less than 10% performance loss compared to wider ranges.
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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.