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- W1992452382 abstract "We have studied the non-steady evolution of both gas and solid grains in the convective solar nebula by using accretion disk model. Time-dependent processes considered are the accretion from the outer boundary of the nebula, the collisional growth of grains, the sublimation/recondensation of solid ice. The calculations show that the grain growth weakens the convection, and therefore the laminar nebula is left. The remaining nebula has about 0.05 solar mass with the lifetime of about 107 years. This remnant mass shows weak dependences on the efficiency factor a in the turbulent viscosity and the accretion rate. The spatial distribution of the remnant gas is determined by the size of grains because they grow to the size of mm-cm. This remnant mass is smaller than that of Ruden and Pollack (1991) because of the heatings besides the dissipation which decreases at the final stage. Thus the grains and the heating sources are the keys to guess the remaining mass and its distribution, or in other words, the initial condition of planetary accumulation." @default.
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- W1992452382 date "1994-01-01" @default.
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- W1992452382 title "Non-Steady Evolution of the Accretion Disk Solar Nebula." @default.
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- W1992452382 doi "https://doi.org/10.5636/jgg.46.771" @default.
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