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Paper: Protostellar Disk Structure
Volume: 321, Extrasolar Planets: Today and Tomorrow
Page: 252
Authors: Balbus, S.A.
Abstract: Protostellar disk modeling is reviewed. The importance of retaining fluctuations explicitly in models is emphasized. The presence of shear turbulence in a disk seems also to require the presence of magnetic fields, which in the case of protostellar disks leads to as yet unresolved questions of ionization structure. Most calculations find a three-zone disk model involving a central decoupled region, but answers to several fundamental questions remain incomplete or unknown (e.g., the nature of energy dissipation, dust grain disposition, magnetic coupling criteria). Numerical simulations will play an essential role in the development of a deeper understanding of protostellar disk structure.
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