A new grid of disk models with grain-surface CO chemistry plus an ML inference tool produces gas mass estimates from ALMA observations that match independent dynamical and HD values without requiring extreme elemental depletion.
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11 Pith papers cite this work, alongside 1,155 external citations. Polarity classification is still indexing.
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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.
V1094 Sco's disk shows a planet-like double gap at ~100 au and outer rings matching secular gravitational instability, implying a hybrid origin for ring-gap pairs in one disk.
A 2D Monte Carlo dust evolution simulation shows that a planet-induced pressure bump reproduces the observed compositions and formation ages of carbonaceous chondrites, implying formation in a single long-lived dust trap outside Jupiter's orbit.
In streaming-instability simulations, gas-dust relative flow becomes azimuthal wherever dust-to-gas ratio exceeds one, so birdie-aligned prolate grains naturally emit the azimuthal polarization seen in disks like HL Tau.
Jet feedback in centrally concentrated clouds reduces star formation efficiency to 12-16% and yields cluster structures more consistent with observations than models without jets.
Streaming instability in magnetized AGN dust tori can yield tens of millions of planetary-mass objects per AGN, some formed directly above the hydrogen-burning limit.
Modeling of ALMA observations reveals diverse vertical heights for millimeter dust in six protoplanetary disks, from very thin in T Cha and PDS 111 to extended in DoAr 25, with models failing to match small dust distributions.
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.
Halos in Elias 2-24, IM Lup, and DM Tau hold 20-30% of total dust mass with cm-sized grains, helping resolve the disk mass-budget problem even though drift and growth timescales are shorter than disk ages.
Two migrating super-Earths in low-viscosity disks trigger narrow and broad dust substructures with high dust-to-gas ratios favorable for planetesimal formation.
citing papers explorer
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DiskMINT-GARDEN: Self-consistent Models to Estimate Disk Masses
A new grid of disk models with grain-surface CO chemistry plus an ML inference tool produces gas mass estimates from ALMA observations that match independent dynamical and HD values without requiring extreme elemental depletion.
-
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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A Hybrid Origin for the Multiple Ring-Gap Structures in the Large Protoplanetary Disk V1094 Sco: A Low-Mass Planet and Secular Gravitational Instability
V1094 Sco's disk shows a planet-like double gap at ~100 au and outer rings matching secular gravitational instability, implying a hybrid origin for ring-gap pairs in one disk.
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Carbonaceous Chondrites provide evidence for late-stage planetesimal formation in a pressure bump
A 2D Monte Carlo dust evolution simulation shows that a planet-induced pressure bump reproduces the observed compositions and formation ages of carbonaceous chondrites, implying formation in a single long-lived dust trap outside Jupiter's orbit.
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Azimuthal Dust Polarization from Aerodynamically Aligned Grains as Evidence for the Streaming Instability in Protoplanetary Disks
In streaming-instability simulations, gas-dust relative flow becomes azimuthal wherever dust-to-gas ratio exceeds one, so birdie-aligned prolate grains naturally emit the azimuthal polarization seen in disks like HL Tau.
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Centrally concentrated star formation in young clusters II: Jet feedback
Jet feedback in centrally concentrated clouds reduces star formation efficiency to 12-16% and yields cluster structures more consistent with observations than models without jets.
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Active Galactic Nucleus Tori: Potential Birthplace to Millions of Planets
Streaming instability in magnetized AGN dust tori can yield tens of millions of planetary-mass objects per AGN, some formed directly above the hydrogen-burning limit.
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Diverse dust vertical height and settling strength conditions in protoplanetary discs
Modeling of ALMA observations reveals diverse vertical heights for millimeter dust in six protoplanetary disks, from very thin in T Cha and PDS 111 to extended in DoAr 25, with models failing to match small dust distributions.
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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.
-
Dust characterization of halos: The extended emission in protoplanetary disks
Halos in Elias 2-24, IM Lup, and DM Tau hold 20-30% of total dust mass with cm-sized grains, helping resolve the disk mass-budget problem even though drift and growth timescales are shorter than disk ages.
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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.