Simulations of giant impacts between 0.2-4 Earth-mass planets yield post-impact luminosities of 5e-5 to 0.1 L_sun cooling over 1-2000 days, predicting 0-14 detections in Gaia DR4 and a comparable number in LSST.
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7 Pith papers cite this work, alongside 197 external citations. Polarity classification is still indexing.
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Two-stage GMM clustering of close-in exoplanets in dynamical feature space mapped to pebble-accretion models identifies sub-populations with distinct formation histories including earlier epochs for very-massive gas giants.
Numerical model of C outgassing shows CC planetesimals deplete >50% carbon while NCs deplete <50% for typical sizes and formation times, favoring NC bodies as the main C source for terrestrial planets.
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.
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.
Simulations tie the deep-mantle primordial neon reservoir to an initial embryo mass of ~0.3 Earth masses assembled during solar-nebula dispersal.
Photoevaporative and collisional mass losses diversify exoplanet parameter space in ways consistent with standard core accretion, enabling an expanded eight-class classification scheme.
citing papers explorer
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Can giant impacts be directly detected in other star systems?
Simulations of giant impacts between 0.2-4 Earth-mass planets yield post-impact luminosities of 5e-5 to 0.1 L_sun cooling over 1-2000 days, predicting 0-14 detections in Gaia DR4 and a comparable number in LSST.
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Machine-learning clustering of close-in exoplanet populations: links to pebble accretion
Two-stage GMM clustering of close-in exoplanets in dynamical feature space mapped to pebble-accretion models identifies sub-populations with distinct formation histories including earlier epochs for very-massive gas giants.
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Modeling carbon outgassing from chondritic planetesimals
Numerical model of C outgassing shows CC planetesimals deplete >50% carbon while NCs deplete <50% for typical sizes and formation times, favoring NC bodies as the main C source for terrestrial planets.
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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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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.
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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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Formation and evolution pathways of planets. I. Comparison between theory and observations
Photoevaporative and collisional mass losses diversify exoplanet parameter space in ways consistent with standard core accretion, enabling an expanded eight-class classification scheme.