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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An intercomparison of planetary evolution codes finds Earth magma oceans solidify in about 4 million years while Venus scenarios show more varied prolonged stages up to 50 million years, with outcomes sensitive to initial volatile budgets and model-specific treatments.
Microlensing-inferred free-floating planets plus bound planets require more mass than protoplanetary disks supply, even at 100% conversion efficiency, potentially creating a crisis if the mass function is bottom-heavy.
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
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.
Models coupling hydrogen-silicate-iron miscibility with atmospheric escape reproduce the observed mass-radius occurrence density of sub-Neptunes and super-Earths.
The paper reviews ML applications for sequence modeling, pattern recognition, and generative Bayesian analysis to tackle heterogeneous data challenges in (exo)planetary science.
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