Structure of the satelitary accretion disk of Saturn

Details Structure of the satelitary accretion disk of Saturn Structure of the satelitary accretion disk of Saturn

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984icar...59..376c&link_type=abstract

Icarus (ISSN 0019-1035), vol. 59, Sept. 1984, p. 376-391.

Physics

9

Accretion Disks, Planetary Evolution, Planetary Structure, Saturn (Planet), Saturn Satellites, Density Distribution, Temperature Distribution, Turbulence, Turbulence Models, Saturn, Structure, Satellites, Accretion, Disk, Convection, Energy, Parameters, Dissipation, Flux, Dust, Abundance, Turbulence, Models, Evolution, Time Scale, Condensation, Mass, Thermal Effects, Silicate, Temperature, Iron, Ice, Grains, Formation, Data, Calculations

Scientific paper

A study of both the physical and the thermodynamical characteristics of a satellitary accretion disk around Saturn has been performed in order to investigate the primordial stages of the formation of the Saturn satellites. In particular, the evolution of a satellitary disk during the infall of material from the surrounding cloud is analyzed. The dependence of the disk structure on the intensity of the external radiation field, the accretion time, the abundance of solid material in the disk, and the degree of turbulence is verified. IT is shown that the external energy flux does not play an important role in the evolution of the disk structure. Models characterized by either longer times or a noticeable depletion of condensable elements have a total mass of the order of 0.34-0.1 times the mass of the regular satellites increased by the mass of the light elements. Low turbulence models have approximately a mass twice that of the regular satellites.

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