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Viscous Diffusion Stage of Evolution of Protoplanetary Disks

Author: TaoYanFen
Tutor: JinLiPing
School: Jilin University
Course: Theoretical Physics
Keywords: Uniform viscous Protoplanetary disk Accretion disk Solar nebula
CLC: P181
Type: Master's thesis
Year: 2010
Downloads: 23
Quote: 0
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Abstract


Evolution of the solar nebula can be divided into three stages: the whereabouts of viscous dissipation and cleanup phase . Each stage of the dish structure determined by the different physical processes . When merging from the molecular cloud collapse and fall onto the plate of the material surface, the surface of the plate material by thin accretion shock sub-sonic stabilized when the solar nebula is formed. This process of accretion shock nebula surface to provide a lot of heat. Convergence of the angular momentum of the gas in the accretion shock beneath a thin layer of turbulent shear layer will be adjusted to the Kepler disk angular momentum values ??and has the potential to provide local viscous . In this article we focus on the viscous dissipation phase. We consider the evolution dish dish mainly on the viscosity of the internal pressure generated . At this stage, the viscous mechanism will redistribute nebula mass and angular momentum . Plate material flows inwards angular momentum flow out nebula gradually outward expansion. With previous uniform viscous consider different , in which we join to study inhomogeneous viscous viscous dissipation primitive solar nebula stage . Calculation of non-uniform application of the latest sticky . In the viscous calculations, we joined the magnetic rotational instability effect . Nebula surface density radial distribution and other physical considerations conventional homogeneous viscous nebula significantly different models . We believe more in line with the results of non-uniform viscous nebula evolution of historical truth .

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CLC: > Astronomy,Earth Sciences > Astronomy > Solar system > The origin and evolution of the solar system
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