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Physical processes in protoplanetary disks
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This review introduces physical processes in protoplanetary disks relevant to accretion and the initial stages of planet formation. After a brief overview of the observational context, I introduce the elementary theory of disk structure and evolution, review the gas-phase physics of angular momentum transport through turbulence and disk winds, and discuss possible origins for the episodic accretion observed in Young Stellar Objects. Turning to solids, I review the evolution of single particles under aerodynamic forces, and describe the conditions necessary for the development of collective gas-particle instabilities. Observations show that disks can exhibit pronounced large-scale structure, and I discuss the types of structures that may form from gas and particle interactions at ice lines, vortices and zonal flows, prior to the formation of large planetary bodies. I conclude with disk dispersal.
Forward citations
Cited by 4 Pith papers
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Azimuthal molecular variations in the AB Aur planet-forming disk
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Episodic accretion in high-mass star formation: An analysis of thermal instability for axially symmetric disks
Two-dimensional simulations of thermal instability in high-mass protostar disks produce bursts with peak accretion rates of 2-3e-4 solar masses per year, weaker and longer than observed events.
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Extending dynamical mass measurements: probing GI as a possible origin of mm-dust spirals
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