Older Upper Scorpius disks show reduced molecular emission and hints of higher inner-gas C/O ratios than young disks, indicating chemical evolution consistent with pebble drift.
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Progress of Theoretical Physics Supplement , year = 1981, volume = 70, pages =
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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.
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.
Cavity truncation in circumbinary discs is set by binary parameters together with instantaneous cavity eccentricity and relative apsidal orientation, yielding a prescription for pericentre radius Rp and semi-major axis acav.
Hydrodynamical simulations of giant impacts find lower post-impact CMB pressures due to thermal and rotational effects, common full mantle melting, and conditions favoring metal-silicate equilibration near the CMB.
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.
2D radiation-hydrodynamical simulations find accretion outbursts unstable to Rossby-wave instability, forming vortices that suppress planetesimal formation until post-burst quiescence.
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.
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From Young to Older Disks: JWST/MIRI Evidence for Fading Molecular Emission and Hints for Elevated C/O in Upper Scorpius
Older Upper Scorpius disks show reduced molecular emission and hints of higher inner-gas C/O ratios than young disks, indicating chemical evolution consistent with pebble drift.
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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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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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Characterizing the bolometric-photoevaporative transition in young sub-Neptunes with radiation-hydrodynamic simulations
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.
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Revisiting the picture of circumbinary disc truncation
Cavity truncation in circumbinary discs is set by binary parameters together with instantaneous cavity eccentricity and relative apsidal orientation, yielding a prescription for pericentre radius Rp and semi-major axis acav.
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Thermal and rotational effects of giant impacts during terrestrial planet accretion
Hydrodynamical simulations of giant impacts find lower post-impact CMB pressures due to thermal and rotational effects, common full mantle melting, and conditions favoring metal-silicate equilibration near the CMB.
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Beyond the $\alpha$ model: scaling the wind-driven accretion rate in protoplanetary disks using systematic non-ideal magnetohydrodynamical simulations
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.
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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.
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Planet formation at the inner edge of the dead zone II. Outbursts, rings, vortices, and suppression of planetesimal formation
2D radiation-hydrodynamical simulations find accretion outbursts unstable to Rossby-wave instability, forming vortices that suppress planetesimal formation until post-burst quiescence.
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JWST-DECO: The Impact of Accretion on Mid-Infrared Observable Water in Planet-forming Disks
Accretion increases observable water mass in disks by expanding the emitting area via higher central luminosity, while viscous heating has no effect.
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$\alpha\beta q_\mathrm{th}$-mapping of planet-induced density wave damping in protoplanetary discs
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A formation pathway for giant planets in S-type discs of {\gamma}-Cephei-like compact binaries
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.
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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.
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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
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Configuration of the $\xi$ Tau system constrained by multi-technique observations
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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.
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Rapid and Predictive Planet Population Synthesis Model (RAPPS) I. Upgraded model and resulting synthetic populations
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