AGN dust tori can form tens of millions of planetesimals from Earth to super-Jupiter masses via streaming instability, with continued growth to stellar masses through pebble and gas accretion.
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7 Pith papers cite this work. Polarity classification is still indexing.
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Sustained mass transfer from a circumbinary disc enables giant planet formation in gamma-Cephei-like binaries by prolonging the lifetime of the circumprimary disc against truncation and photoevaporation.
An optimal Stokes number window of 0.01-0.03 allows streaming instability to form planetesimals and pebble accretion to build all three main planet classes, with cold gas giants needing the lowest turbulence and largest discs.
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
Simulations require 2000 Earth masses of pebbles to match observed disc gaps, but this produces mostly gas giants and few super-Earths, contradicting exoplanet data.
Multi-technique observations constrain the configuration of the ξ Tau system, detecting orbital oscillations on multiple timescales and suggesting component C is itself a binary.
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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Active Galactic Nucleus Tori: Potential Birthplace to Millions of Planets
AGN dust tori can form tens of millions of planetesimals from Earth to super-Jupiter masses via streaming instability, with continued growth to stellar masses through pebble and gas accretion.
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A formation pathway for giant planets in S-type discs of {\gamma}-Cephei-like compact binaries
Sustained mass transfer from a circumbinary disc enables giant planet formation in gamma-Cephei-like binaries by prolonging the lifetime of the circumprimary disc against truncation and photoevaporation.
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Exploring the conditions for forming planetesimals by the streaming instability and planetary systems by pebble accretion
An optimal Stokes number window of 0.01-0.03 allows streaming instability to form planetesimals and pebble accretion to build all three main planet classes, with cold gas giants needing the lowest turbulence and largest discs.
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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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Are the observed gaps in protoplanetary discs caused by growing planets?
Simulations require 2000 Earth masses of pebbles to match observed disc gaps, but this produces mostly gas giants and few super-Earths, contradicting exoplanet data.
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Configuration of the $\xi$ Tau system constrained by multi-technique observations
Multi-technique observations constrain the configuration of the ξ Tau system, detecting orbital oscillations on multiple timescales and suggesting component C is itself a binary.
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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.