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Evolution of a Viscous Protoplanetary Disk with Convectively Unstable Regions. II. Accretion Regimes and Long-Term Dynamics

Authors
  • Maksimova, L. A.1
  • Pavlyuchenkov, Ya. N.1
  • Tutukov, A. V.1
  • 1 Institute of Astronomy, Russian Academy of Sciences, Moscow, 119017, Russia , Moscow (Russia)
Type
Published Article
Journal
Astronomy Reports
Publisher
Pleiades Publishing
Publication Date
Oct 10, 2020
Volume
64
Issue
10
Pages
815–826
Identifiers
DOI: 10.1134/S1063772920110050
Source
Springer Nature
License
Yellow

Abstract

AbstractIn this article, we proceed to study convection as a possible factor of episodic accretion in protoplanetary disks. Within the model presented in Article I, the accretion history is analyzed at different rates and areas of matter inflow from the envelope onto the disk. It is shown that the burst-like regime occurs in a wide range of parameters. The long-term evolution of the disk is also modeled, including the decreasing-with-time matter inflow from the envelope. It is demonstrated that the disk becomes convectively unstable and maintains burst-like accretion onto the star for several million years. Meanwhile, the instability expands to an area of several tens of astronomical units and gradually decreases with time. It is also shown that at early stages in the disk evolution, conditions arise for gravitational instability in the outer parts of the disk and for dust evaporation in the convectively unstable inner regions. The general conclusion of the study is that convection can serve as one of the mechanisms of episodic accretion in protostellar disks, but this conclusion needs to be verified using more consistent hydrodynamic models.

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