Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
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The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.
The Bern Model has incorporated MHD disk evolution, pebble accretion, and improved interiors, yielding quantitative matches to exoplanet mass functions, radius distributions, and system architectures.
citing papers explorer
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Constructing Earth Formation History Using Deep Mantle Noble Gas Reservoirs
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
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Giant Planet Formation by Disk Instability
The disk instability model remains viable for explaining giant planets that form early, at large orbital distances, and around M-dwarf stars, supported by updated simulations and observations.
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The formation of planetary systems: physics, populations, and architectures
The Bern Model has incorporated MHD disk evolution, pebble accretion, and improved interiors, yielding quantitative matches to exoplanet mass functions, radius distributions, and system architectures.