Physics
Scientific paper
Aug 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988icar...75..371m&link_type=abstract
Icarus (ISSN 0019-1035), vol. 75, Aug. 1988, p. 371-379.
Physics
37
Accretion Disks, Cosmochemistry, Interplanetary Dust, Protoplanets, Solar System, Star Formation, Coagulation, Cosmology, Evaporation, Grain Size, Optical Thickness, Particle Size Distribution, Turbulence Effects, Viscosity
Scientific paper
Steady axisymmetric turbulent-disk models of solar-system formation are developed analytically, with a focus on the effects of strong convectively driven turbulence, dust coagulation (leading to decreased disk opacity), and inner-disk grain evaporation. The treatment of coagulation, radial transport, and fragmentation is explained; the derivation of the opacity law and the governing equations for the viscous protoplanetary disk is outlined; and numerical results are presented in graphs. It is shown that the disk can remain optically thick (despite significantly lower opacity values) and develop broad transition regions, in which major chemical species are present at near-sublimation temperatures. One such region at about 1500 K (the Si-Fe transition zone), possibly extending to a radial distance greater than 1 AU, is considered in detail.
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