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.
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6 Pith papers cite this work. Polarity classification is still indexing.
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Planets with realistic dense cores survive close star encounters without total disruption, allowing more to circularize into hot Jupiters or be ejected after mass loss.
The atmosphere of TOI-1130b shows high metallicity, low C/O, and elevated mean molecular weight consistent with ex-situ formation beyond the water ice line.
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.
Astronomical objects from asteroids to stars mostly follow a cohesive mass-density sequence reflecting gravitational contraction and nuclear ignition, while compact stellar remnants deviate from it.
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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Planetary formation tracks on the Hertzsprung-Russell diagram: Visualising the processes of giant planet growth
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.
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Where Do Hot Jupiters Come From? Revisiting Tidal Disruption and Ejection in High-Eccentricity Migration
Planets with realistic dense cores survive close star encounters without total disruption, allowing more to circularize into hot Jupiters or be ejected after mass loss.
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JWST unveils a high mean molecular weight atmosphere for mini-Neptune TOI-1130b: Evidence for formation beyond the water ice line
The atmosphere of TOI-1130b shows high metallicity, low C/O, and elevated mean molecular weight consistent with ex-situ formation beyond the water ice line.
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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.
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The Cohesive Object Sequence: The Mass-Density Distribution of Astronomical Objects from Asteroids to Stars
Astronomical objects from asteroids to stars mostly follow a cohesive mass-density sequence reflecting gravitational contraction and nuclear ignition, while compact stellar remnants deviate from it.
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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.