Young sub-Neptunes transition from core-powered bolometric escape to photoevaporative escape at smaller radii for lower-mass and more irradiated planets, with self-consistent simulations yielding combined mass-loss rates and analytic transition scalings.
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Varying the adiabatic index from 1.2 to 1.4 in exoplanet evolution models shows that higher gamma produces puffier initial envelopes that contract faster with accelerated mass loss, so using gamma=1.4 overestimates mass-loss effects on young planets.
Mass of 13.7 Earth masses and density 0.4 g cm^{-3} measured for TOI-1883 b, a super-Neptune in the ridge regime around an early-M dwarf, with implications for disk migration and photoevaporation.
citing papers explorer
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Characterizing the bolometric-photoevaporative transition in young sub-Neptunes with radiation-hydrodynamic simulations
Young sub-Neptunes transition from core-powered bolometric escape to photoevaporative escape at smaller radii for lower-mass and more irradiated planets, with self-consistent simulations yielding combined mass-loss rates and analytic transition scalings.
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The Effect of Adiabatic Index on Radius Evolution and the Mass Loss
Varying the adiabatic index from 1.2 to 1.4 in exoplanet evolution models shows that higher gamma produces puffier initial envelopes that contract faster with accelerated mass loss, so using gamma=1.4 overestimates mass-loss effects on young planets.
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The mass of TOI-1883 b: A low density super-Neptune in the ridge regime transiting an early-M dwarf
Mass of 13.7 Earth masses and density 0.4 g cm^{-3} measured for TOI-1883 b, a super-Neptune in the ridge regime around an early-M dwarf, with implications for disk migration and photoevaporation.