GPU-accelerated N-body simulations show that the common acceleration factor f distorts planetary chemical compositions and that terrestrial planets can form resonant chains without gas-driven orbital migration.
Chambers, Icarus180(2), 496 (2006)
4 Pith papers cite this work. Polarity classification is still indexing.
4
Pith papers citing it
citation-role summary
background 2
method 1
citation-polarity summary
fields
astro-ph.EP 4verdicts
UNVERDICTED 4representative citing papers
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
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.
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
-
Terrestrial planet formation in the era of GPU computing
GPU-accelerated N-body simulations show that the common acceleration factor f distorts planetary chemical compositions and that terrestrial planets can form resonant chains without gas-driven orbital migration.
-
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.
-
Rapid and Predictive Planet Population Synthesis Model (RAPPS) I. Upgraded model and resulting synthetic populations
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.
-
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.