A tree algorithm reduces multi-component coagulation complexity from O(N^{2d}) to O(d N^d log N) by grouping similar interactions and matches direct-method results in tests with analytic solutions.
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7 Pith papers cite this work, alongside 883 external citations. Polarity classification is still indexing.
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Gas giants form sub-snowline in binaries via dust traps at the tidal truncation radius, with observed planet semi-major axes following a_planet = 0.569 r_t (R²=0.94).
A semi-analytic model using elastoplastic contact mechanics and weakest-link fracture statistics reproduces the sticking-bouncing boundary from DEM simulations and places the bouncing barrier within ALMA-inferred size-velocity ranges for moderately porous aggregates.
Simulations of hypervelocity rocky-on-icy impacts show porosity controls crater morphology but not the efficient vaporization of the rocky impactor material.
Updated DALI models reproduce observed C2H2 fluxes with solar C/O and find the C2H2/H2O flux ratio sensitive to elemental abundances and small-grain abundance in planet-forming disk regions.
Radiative-transfer simulations with common dust models generate a range of spectral indices but cannot reach the lowest observed emissivity indices in protostars without invoking unexpectedly large millimeter-sized grains.
Spectroscopic observations of disintegrating comet C/2019 Y4 (ATLAS) classify it as a typical Oort cloud comet with less dust, where porous dust accounts for its slightly red reflectivity gradient of ~5% per 1000 Å.
citing papers explorer
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A fast tree algorithm for multi-component coagulation equation
A tree algorithm reduces multi-component coagulation complexity from O(N^{2d}) to O(d N^d log N) by grouping similar interactions and matches direct-method results in tests with analytic solutions.
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Sub-Snowline Formation of Gas-Giant Planets in Binary Systems
Gas giants form sub-snowline in binaries via dust traps at the tidal truncation radius, with observed planet semi-major axes following a_planet = 0.569 r_t (R²=0.94).
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A semi-analytic model of the bouncing barrier for protoplanetary dust aggregates
A semi-analytic model using elastoplastic contact mechanics and weakest-link fracture statistics reproduces the sticking-bouncing boundary from DEM simulations and places the bouncing barrier within ALMA-inferred size-velocity ranges for moderately porous aggregates.
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Numerical Simulations of Hypervelocity Micrometeoroid Impacts: Rocky Impactors onto Icy Targets and the Role of Porosity
Simulations of hypervelocity rocky-on-icy impacts show porosity controls crater morphology but not the efficient vaporization of the rocky impactor material.
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Chemistry and IR emission of acetylene in planet-forming regions of T Tauri disks. Impact of elemental abundances and dust properties
Updated DALI models reproduce observed C2H2 fluxes with solar C/O and find the C2H2/H2O flux ratio sensitive to elemental abundances and small-grain abundance in planet-forming disk regions.
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Pristine composition or size evolution: Can current dust models reproduce emissivities observed in nearby protostars?
Radiative-transfer simulations with common dust models generate a range of spectral indices but cannot reach the lowest observed emissivity indices in protostars without invoking unexpectedly large millimeter-sized grains.
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Dust and Volatiles in the Disintegrating Comet C/2019 Y4 (ATLAS)
Spectroscopic observations of disintegrating comet C/2019 Y4 (ATLAS) classify it as a typical Oort cloud comet with less dust, where porous dust accounts for its slightly red reflectivity gradient of ~5% per 1000 Å.