JWST NIRISS/SOSS data yield a transmission spectrum of the 23 Myr V1298 Tau c showing H2O absorption and an atmospheric metallicity of 14.8^{+56}_{-12} times solar, lower than mature planets of similar mass.
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SUPER-EARTH ATMOSPHERES: SELF-CONSISTENT GAS ACCRETION AND RETENTION
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astro-ph.EP 13years
2026 13representative citing papers
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.
Coupled thermal-chemical models indicate that sub-Neptunes formed outside the water-ice line exhibit high atmospheric CH4, H2O, and C/O ratios while those formed inside show suppressed CH4 and low C/O.
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.
An open-source GCE code with a 100x faster solver demonstrates that refractory ratios Mg/Si and Fe/Si control carbon partitioning and atmospheric properties in water-accreting sub-Neptunes.
The transmission spectrum of AU Mic b is dominated by the transit light source effect from stellar spots, yielding only weak atmospheric constraints with a preferred scale height below 185 km.
A simulated 2.5-year multi-band photometric survey is projected to detect ~100 young transiting planets, sufficient to measure their occurrence rate to 5% precision and differentiate gas-dwarf versus water-world formation scenarios.
Coupling Bern formation models with extended chemical equilibrium including S and N shows equilibration depletes atmospheric nitrogen, shifts C/O higher outside the ice line, generates Si species, and leaves sulfur abundances weakly dependent on formation location.
Sub-Neptunes around metal-rich stars have a 42.6% conditional probability of cold Jupiters versus 14.5% for super-Earths, showing a metallicity-dependent correlation absent in the latter.
Photoevaporative and collisional mass losses diversify exoplanet parameter space in ways consistent with standard core accretion, enabling an expanded eight-class classification scheme.
Hydrogen-silicate miscibility stores hydrogen in sub-Neptune interiors, resupplies escaping envelopes, delays contraction, matches young-planet observations, and enables a population test requiring 70-100 targets under 100 Myr.
Models coupling hydrogen-silicate-iron miscibility with atmospheric escape reproduce the observed mass-radius occurrence density of sub-Neptunes and super-Earths.
An upgraded planet population synthesis model incorporates post-disc dynamical evolution and atmospheric enrichment to generate synthetic exoplanet populations with improved fidelity to N-body results and observations.
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