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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Uranus and Neptune are reinterpreted as magma-ocean giants with hydrogen-rich interiors rather than traditional ice giants, consistent with observations via three fit parameters each.
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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Ice Giants Revisited: Uranus and Neptune as Magma Ocean Worlds
Uranus and Neptune are reinterpreted as magma-ocean giants with hydrogen-rich interiors rather than traditional ice giants, consistent with observations via three fit parameters each.