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.
Canonical reference
Title resolution pending
Canonical reference. 71% of citing Pith papers cite this work as background.
15
Pith papers citing it
1,502
external citations · Crossref
Background
71% of classified citations
citation-role summary
background 5
method 2
citation-polarity summary
representative citing papers
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.
Young sub-Neptunes transition from core-powered bolometric escape to photoevaporative escape at smaller radii for lower-mass and more irradiated planets, with self-consistent simulations yielding combined mass-loss rates and analytic transition scalings.
Non-ideal MHD shearing-box simulations with a new damping scheme yield power-law scalings for wind-driven accretion rates based on midplane plasma beta, ambipolar Elsasser number, and active layer thickness that match results within a factor of 2-3.
Planetesimal disks with 1-4% of the planetary mass disrupt resonant Neptune chains, triggering instabilities that scatter planets to ~0.1 au orbits and enable hot Neptune formation on 10-100 Myr timescales.
Accretion increases observable water mass in disks by expanding the emitting area via higher central luminosity, while viscous heating has no effect.
Nonlinear shock formation dominates angular momentum deposition from planet-induced density waves, cooling matches it for sub-thermal planets, and viscosity only matters at unrealistically high values.
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.
Disk formation simulations reproduce carbonaceous chondrule oxygen isotopes with moderate radial infall or ice-depleted parental clouds, but ordinary chondrules inside the snow line remain difficult to explain under the modeled conditions.
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.
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.
Two migrating super-Earths in low-viscosity disks trigger narrow and broad dust substructures with high dust-to-gas ratios favorable for planetesimal formation.
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.
citing papers explorer
-
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.
-
Planetesimal-Driven Instabilities in Resonant Chains of Cold Neptunes and Their Dynamical Outcomes
Planetesimal disks with 1-4% of the planetary mass disrupt resonant Neptune chains, triggering instabilities that scatter planets to ~0.1 au orbits and enable hot Neptune formation on 10-100 Myr timescales.
-
Oxygen Isotopic Compositions of Chondrules as Probes of Solar Protoplanetary Disk Formation
Disk formation simulations reproduce carbonaceous chondrule oxygen isotopes with moderate radial infall or ice-depleted parental clouds, but ordinary chondrules inside the snow line remain difficult to explain under the modeled conditions.
-
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.
-
On the Dust Substructures Triggered by Two Super-Earths Migrating in Low-viscosity Disks
Two migrating super-Earths in low-viscosity disks trigger narrow and broad dust substructures with high dust-to-gas ratios favorable for planetesimal formation.