Initial misalignment between magnetic field and rotation axis in star-forming cores naturally produces twisted pseudodisks and asymmetric streamer-like accretion, as shown by a parameter survey of 3D MHD simulations.
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The Disk Substructures at High Angular Resolution Project (DSHARP) VI: Dust trapping in thin-ringed protoplanetary disks
11 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
A large fraction of the protoplanetary disks observed with ALMA display multiple well-defined and nearly perfectly circular rings in the continuum, in many cases with substantial peak-to-valley contrast. The DSHARP campaign shows that several of these rings are very narrow in radial extent. In this paper we test the hypothesis that these dust rings are caused by dust trapping in radial pressure bumps, and if confirmed, put constraints on the physics of the dust trapping mechanism. We model this process analytically in 1D, assuming axisymmetry. By comparing this model to the data, we find that all rings are consistent with dust trapping. Based on a plausible model of the dust temperature we find that several rings are narrower than the pressure scale height, providing strong evidence for dust trapping. The rings have peak absorption optical depth in the range between 0.2 and 0.5. The dust masses stored in each of these rings is of the order of tens of Earth masses, though much ambiguity remains due to the uncertainty of the dust opacities. The dust rings are dense enough to potentially trigger the streaming instability, but our analysis cannot give proof of this mechanism actually operating. Our results show, however, that the combination of very low alpha_turb << 5e-4 and very large grains a_grain >> 0.1 cm can be excluded by the data for all the rings studied in this paper.
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2026 11representative citing papers
The 69 au dust ring in LkCa 15 is broad and thick at 0.88 mm and progressively narrower and thinner at 1.34 and 3.08 mm, implying a massive population of small grains alongside a more concentrated large-grain population.
A new radiation-hydrodynamics scheme for the PLUTO code couples gas, radiation, and multiple independently moving dust species, validated on analytic test problems.
Serpens disk dust masses resemble Lupus and Taurus despite its high 2D stellar density, and the Ophiuchus and Corona Australis low-mass tension shifts to disks lacking Gaia identifications.
Faint Class II disks in Taurus show the same 198-358 GHz spectral index distribution as brighter disks, suggesting they too are optically thick at submillimeter wavelengths.
Cloud-fed ideal-MHD zoom-in simulations of nine young stars show discs are replenished on ~10,000-year timescales via surface-layer accretion and can be truncated by massive streamers.
An optically thick dust ring around PDS 70 c can explain the observed flat radio spectrum, whereas a smooth dust disk would require implausibly high dust inflow rates.
New ALMA data resolve a faint outer dust ring at about 45 au around Sz 76, shifting its dust radius from about 7 to 41 au and bringing its gas-to-dust size ratio into the typical range for Lupus disks.
Observations of 33 young solar-type stars show that inner-disk dust mass and accretion rate decline with age, and large centimetre-sized grains are depleted in discs older than 2 Myr, consistent with the formation of giant planet cores.
2D radiation-hydrodynamical simulations find accretion outbursts unstable to Rossby-wave instability, forming vortices that suppress planetesimal formation until post-burst quiescence.
A candidate 0.3-7.6 MJup companion is reported in the gap of the ~2.8 Myr pre-transitional disk around WRAY 15-1880, with an ALMA blob interpreted as a vortex at the m=1 Lindblad resonance.
citing papers explorer
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Twisted Pseudodisk and Asymmetric Mass Accretion on the Circumstellar Disk II: Parameter Survey
Initial misalignment between magnetic field and rotation axis in star-forming cores naturally produces twisted pseudodisks and asymmetric streamer-like accretion, as shown by a parameter survey of 3D MHD simulations.
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Geometry of dust rings in protoplanetary disks: the case of LkCa 15
The 69 au dust ring in LkCa 15 is broad and thick at 0.88 mm and progressively narrower and thinner at 1.34 and 3.08 mm, implying a massive population of small grains alongside a more concentrated large-grain population.
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Simulating the thermodynamics of gas, radiation, and multispecies dust: Method and applications to protoplanetary disks
A new radiation-hydrodynamics scheme for the PLUTO code couples gas, radiation, and multiple independently moving dust species, validated on analytic test problems.
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Disk survey in the Serpens star-forming region: Environmental effects in nearby star-forming regions
Serpens disk dust masses resemble Lupus and Taurus despite its high 2D stellar density, and the Ophiuchus and Corona Australis low-mass tension shifts to disks lacking Gaia identifications.
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SMA 200-400 GHz Survey for 10 faint Class II Disks in the Taurus Molecular Cloud
Faint Class II disks in Taurus show the same 198-358 GHz spectral index distribution as brighter disks, suggesting they too are optically thick at submillimeter wavelengths.
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Accretion across scales: streamers, surface-layer transport, and rapid replenishment in young protoplanetary discs
Cloud-fed ideal-MHD zoom-in simulations of nine young stars show discs are replenished on ~10,000-year timescales via surface-layer accretion and can be truncated by massive streamers.
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Interpreting ALMA Multiwavelength Continuum Observations of PDS 70 c: An Optically Thick Dust Ring in the Circumplanetary Disk
An optically thick dust ring around PDS 70 c can explain the observed flat radio spectrum, whereas a smooth dust disk would require implausibly high dust inflow rates.
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A faint dust ring beyond the compact disk of Sz 76
New ALMA data resolve a faint outer dust ring at about 45 au around Sz 76, shifting its dust radius from about 7 to 41 au and bringing its gas-to-dust size ratio into the typical range for Lupus disks.
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The evolution of discs and the epoch of formation of giant planets around solar type stars
Observations of 33 young solar-type stars show that inner-disk dust mass and accretion rate decline with age, and large centimetre-sized grains are depleted in discs older than 2 Myr, consistent with the formation of giant planet cores.
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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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Analysis of the young disk around WRAY 15-1880: does it contain a primitive planetary system?
A candidate 0.3-7.6 MJup companion is reported in the gap of the ~2.8 Myr pre-transitional disk around WRAY 15-1880, with an ALMA blob interpreted as a vortex at the m=1 Lindblad resonance.