From Dust to Planetesimals: Global Evolution of Ice in the Solar Nebula

Details From Dust to Planetesimals: Global Evolution of Ice in the Solar Nebula From Dust to Planetesimals: Global Evolution of Ice in the Solar Nebula

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27.1269s&link_type=abstract

Lunar and Planetary Science, volume 27, page 1269

Physics

1

Dust: Coagulation Of, Giant Planets: Formation, Ice In The Solar System, Solar Nebula

Scientific paper

Planets form by the accumulation of solid matter entrained in a gaseous solar nebula that accretes on the proto-Sun. We model part of this process starting from dust particles suspended in a gaseous disk, and ending up with most of the solid material aggregated into 1-10-km-sized planetesimals. At present, only water-ice solids are considered in our model. The model simultaneously keeps track of the viscous evolution of the gas and the evolution of solid particles due to gas-solid coupling, coagulation, sedimentation, and evaporation/condensation. We have found that the final radial distribution of (icy) solids is very sensitive to initial conditions. Fiducial initial conditions lead to all (icy) solids being lost to the proto-Sun. However, it is possible to find reasonable initial conditions that lead to a radial distribution of (icy) solid material similar to that found in our solar system.

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