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Hydro-, Magnetohydro-, and Dust-Gas Dynamics of Protoplanetary Disks
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The building of planetary systems is controlled by the gas and dust dynamics of protoplanetary disks. While the gas is simultaneously accreted onto the central star and dissipated away by winds, dust grains aggregate and collapse to form planetesimals and eventually planets. This dust and gas dynamics involves instabilities, turbulence and complex non-linear interactions which ultimately control the observational appearance and the secular evolution of these disks. This chapter is dedicated to the most recent developments in our understanding of the dynamics of gaseous and dusty disks, covering hydrodynamic and magnetohydrodynamic turbulence, gas-dust instabilities, dust clumping and disk winds. We show how these physical processes have been tested from observations and highlight standing questions that should be addressed in the future.
Forward citations
Cited by 21 Pith papers
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A Radially Resolved Magnetic Field Threading the Disk of TW Hya
A magnetic field of roughly 10 mG is detected between 60 and 120 au in the TW Hya disk via Zeeman-induced differential broadening of CN hyperfine lines.
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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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Developing a Non-Newtonian Fluid Model for Dust, for Application to Astrophysical Flows
Collisionless dust in turbulent gas is derived as a 6D anisotropic Maxwell fluid whose rheological stress tensor is dynamically important in accretion discs.
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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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JWST/MIRI Detection of Molecular H$_2$ Winds from an Edge-on Class II Source HV Tau C
The edge-on Class II disk HV Tau C hosts a spatially extended, wide-angled molecular hydrogen wind with warm (~600 K) and hot (~2000 K) components and a mass-loss rate near 1e-8 solar masses per year.
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Magnetohydrodynamical opening of dust traps in protoplanetary disks
Large-scale magnetic stresses can overwhelm the pressure-bump trap and force dust to drift inward, "opening" dust traps in wide, low-contrast rings.
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Dust and Gas Transport in Substructured Nonideal MHD Wind-Launching Disks with Embedded Planets
In magnetized wind-launching disks, planet-opened gaps remain partially permeable: small grains and gas leak through, while large grains are filtered, making substructures regulators rather than barriers.
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The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): VII. Testing accretion mechanisms from disk population synthesis
Population synthesis of ALMA disk masses and sizes favors MHD disk-wind-driven accretion over turbulence-driven accretion with photoevaporation.
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Capture and Escape of Planetary Mean-motion Resonances in Turbulent Discs
Active disc turbulence raises equilibrium eccentricities and overstability growth rates in mean-motion resonances, causing migrating planet pairs to escape toward tighter resonances.
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exoALMA IV: Substructures, Asymmetries, and the Faint Outer Disk in Continuum Emission
A homogeneous 15-disk ALMA continuum analysis quantifies disk asymmetries with a new index, links strong asymmetries to inner-disk accretion and NIR excess, and shows that larger disks taper more slowly at their outer edges.
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Compact protoplanetary discs can be produced by dead zones
Fragile dust destroyed beyond a dead zone limits mm-dust emission to the dead zone radius, naturally producing the compact discs seen around young stars.
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Investigating the Bouncing Barrier with Collision Simulations of Compressed Dust Aggregates
Collision simulations show that compressed dust aggregates bounce above a mass threshold that scales as impact velocity to the -4/3 power and drops sharply with packing fraction.
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Observational Signatures of Disk Winds in Protoplanetary Disks: Differentiating Magnetized and Photoevaporative Outflows With Fully Coupled Thermochemistry
Magnetized and photoevaporative protoplanetary disk winds produce distinguishable CO and [C I] emission signatures, with magnetized winds super-Keplerian and photoevaporative winds sub-Keplerian.
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Shedding light on the origin of the broken misaligned circumtriple disk around GW Ori
GW Ori's disk only breaks in simulations when it is unusually thin; at the estimated typical thickness, the stars alone cannot explain the observed gap, favoring circumtriple planets.
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Dust Growth in Binary Systems: Inhibition of dust settling and growth in circumbinary discs
Dust grains in circumbinary discs end up five times smaller than in single-star discs, and the conditions for streaming-instability clumping are not met, arguing against in-situ planet formation there.
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Local three-dimensional simulations of the convective overstability in protoplanetary discs
The manuscript's abstract describes a protoplanetary disc simulation study, but the body is a mathematics paper on Prandtl spirals, so the claimed results are unsupported.
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Ionized gas emission in protoplanetary disks with the SKAO
Synthetic SKA-Mid observations of simulated MHD and photoevaporative disk winds show that free-free emission is detectable in hours and stacked hydrogen recombination lines are spectrally resolvable in ~10 hours.
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Connecting Planetary Composition with Formation: a New Paradigm Emerges
A synthesis review argues that MHD disk winds, not turbulence, dominate disk evolution and planet formation, linking observed disk structures to exoplanet composition and orbits.
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An Introduction to Dust Evolution and Vertical Transport in Protoplanetary Disks
A tutorial that reviews the physics and observational methods for measuring dust sizes and vertical settling in protoplanetary disks.
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Circumstellar and circumbinary discs in multiple stellar systems
This review consolidates current knowledge on how stellar multiplicity shapes protoplanetary disc structure, dust evolution, and planet formation outcomes.
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Planet formation theory: an overview
A review of the current theoretical understanding of planet formation, covering disk evolution, dust growth, planetesimal formation, core accretion, and planetary system dynamics.
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