Giant planet formation traps dust in pressure bumps and planetesimal formation converts dust to larger bodies, making evolved disk masses appear low as a natural outcome of these processes, with models matching observations best for initial disk masses of 4-7% solar mass.
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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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A giant solution to the disk mass budget problem of planet formation
Giant planet formation traps dust in pressure bumps and planetesimal formation converts dust to larger bodies, making evolved disk masses appear low as a natural outcome of these processes, with models matching observations best for initial disk masses of 4-7% solar mass.
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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.