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Accretion discs around young stellar objects and the proto-sunObserved IR and UV excesses have widely been interpreted as signatures for accretion disks around young stellar objects. Analyses of the observed properties of these disks are important for the investigation of star formation as well as the dynamics of the protoplanetary disk out of which the solar system was formed. Accretion-disk theories suggest that evolution of protoplanetary disks is determined by the efficiency of angular momentum transport. During the formation stages, the disk dynamics are regulated by mixing of infalling material and disk gas. In the outermost regions of the disk, self-gravity may promote the growth of nonaxisymmetric perturbations which can transfer angular momentum outwards. After infall has ceased, convectively driven turbulence can redistribute angular momentum with an evolutionary timescale of 0.1 - 1 Myr. Convection in protoplanetary disks may eventually be stabilized by surface heating as the disk material is depleted.
Document ID
19900064400
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Lin, D. N. C.
(Lick Observatory Santa Cruz, CA, United States)
Date Acquired
August 14, 2013
Publication Date
January 1, 1989
Subject Category
Astrophysics
Meeting Information
Meeting: Dynamics of Astrophysical Discs
Location: Manchester
Start Date: December 13, 1988
End Date: December 16, 1988
Accession Number
90A51455
Funding Number(s)
CONTRACT_GRANT: NSF AST-85-21636
CONTRACT_GRANT: NAGW-1211
Distribution Limits
Public
Copyright
Other

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