Physics
Scientific paper
Feb 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978m%26p....18....5c&link_type=abstract
Moon and the Planets, vol. 18, Feb. 1978, p. 5-40.
Physics
207
Solar Corona, Solar Physics, Stellar Evolution, Stellar Mass Accretion, Stellar Models, Angular Momentum, Comets, Dynamic Stability, Energy Dissipation, Gas Giant Planets, Momentum Transfer, Nebulae, Planetary Evolution, Rotating Disks, Steady Flow, Stellar Mass Ejection, Stellar Structure, Viscous Fluids
Scientific paper
The theory of viscous accretion disks developed by Lynden-Bell and Pringle (1974) has been applied to the evolution of the primitive solar nebula. The additional physical input needed to determine the structure of the disk is described. A series of calculations was carried out using a steady flow approximation to explore the effects on the disk properties of variations in such parameters as the angular momentum and accretion rate of the infalling material from a collapsing interstellar cloud fragment. The more detailed evolutionary calculations involved five cases with various combinations of parameters. It was concluded that the late stages of evolution of the disks would be dominated by the effects of mass loss from the expansion of a hot disk corona into space, and the effects of this were included in the evolutionary calculations. A new theory of comet formation is formulated upon these results. The most important result is the conclusion that the primitive solar accretion disk was repeatedly unstable against axisymmetric perturbations, in which rings would form and collapse upon themselves, with the subsequent formation of giant gaseous protoplanets.
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