Planetary formation tracks on the HR diagram show three branches: ascending during solid accretion with L proportional to T to the 8th for in-situ planetesimals, near-horizontal during gas accretion, and descending during post-accretion cooling.
S., Lustig-Yaeger, J., Fortney, J
9 Pith papers cite this work, alongside 315 external citations. Polarity classification is still indexing.
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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.
WASP-96b shows super-solar metallicity of 2-6x stellar, roughly stellar C/O, tentative SO2 consistent with photochemistry, and an optical slope from scattering aerosols, supporting core-accretion formation beyond the water snowline.
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
Variable hydrogen-silicate-iron miscibility coupled with atmospheric escape reproduces the occurrence density structure, radius gap, and radius-period relation of sub-Neptunes and super-Earths based on accreted hydrogen fraction.
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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The Influences of Hydrogen-Silicate-Iron Miscibility on the Demographics of Sub-Neptunes and Super-Earths
Variable hydrogen-silicate-iron miscibility coupled with atmospheric escape reproduces the occurrence density structure, radius gap, and radius-period relation of sub-Neptunes and super-Earths based on accreted hydrogen fraction.