Produced by: Mohsin Shaikh
Trappist-1 b, once thought to lack an atmosphere, reveals surprising hints of CO2-rich conditions and volatile changes, challenging earlier beliefs about its nature.
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Researchers propose a dynamic crust shaped by extreme volcanism or tectonics, with surface rocks potentially younger than 1,000 years—an anomaly for a billion-year-old planet.
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A thick CO2 atmosphere with hydrocarbon haze, like Titan’s, could exist. Researchers from MPIA explore how this haze alters temperature and suggests new atmospheric possibilities.
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Using JWST’s MIRI, scientists detected thermal infrared emissions, indicating faster cooling and possible haze-driven temperature inversions, key for understanding Trappist-1 b.
Similarities to Saturn’s moon Titan emerge, where UV radiation triggers haze formation. Trappist-1 b’s star’s strong radiation may catalyze similar processes.
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Atmospheres on rocky planets are thin, producing weak signatures. Researchers emphasize the difficulty in conclusively identifying atmospheres even with JWST.
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Red dwarfs like Trappist-1 produce strong winds and radiation, potentially stripping nearby planets of atmospheres, adding complexity to the detection process.
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Observing Trappist-1 b during eclipses allows scientists to analyze its atmosphere’s thermal properties and surface heat distribution—a pivotal technique for rocky planets.
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NASA’s ‘Rocky Worlds’ program aims to confirm findings through 500 hours of JWST observations. Comprehensive phase-curve analysis will reveal atmospheric presence and heat dynamics.