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Theory of protostellar accretion disksI will present an overview of the current paradigm for the theory of gaseous accretion disks around young stars. Protostellar disks form from the collapse of rotating molecular cloud cores. The disks evolve via outward angular momentum transport provided by several mechanisms: gravitational instabilities, thermal convective turbulence, and magnetic stresses. I will review the conditions under which these mechanisms are efficient and consistent with the observed disk evolutionary timescales of several million years. Time permitting, I will discuss outbursts in protostellar disks (FU Orionis variables), the effect of planet formation on disk structure, and the dispersal of remnant gas.
Document ID
19940026631
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Ruden, S.
(California Univ. Irvine, CA, United States)
Date Acquired
September 6, 2013
Publication Date
January 1, 1994
Publication Information
Publication: Lunar and Planetary Inst., Workshop on Physics of Accretion Disks Around Compact and Young Stars
Subject Category
Astrophysics
Accession Number
94N31136
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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