Other
Scientific paper
Nov 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993icar..106..102c&link_type=abstract
Icarus, vol. 106, p. 102
Other
230
Gas Dynamics, Protoplanets, Planetary Evolution, Particle Size Distribution, Turbulence Models, Nebulae, Navier-Stokes Equation, Parameterization, Viscous Flow, Turbulent Flow, Equations Of Motion
Scientific paper
In the planetary-formation stage during which particulate material is dispersed in cm-to-m primordial aggregates, particles can settle toward the midplane, forming a layer whose mass density is far greater than that of the gas; it is in this environment that the earliest planetesimals may form. The present numerical models for this planetary formation stage rely on the Reynolds-averaged Navier-Stokes equations for the gas and particles, and are viscous and turbulent. It is established that the rapid accretion of planetesimals by gravitationally unstable fragmentation on an orbital timescale will not occur until objects have already accreted to the mass of the largest extant meteorite samples, through some other process.
Champney Joelle M.
Cuzzi Jeffrey N.
Dobrovolskis Anthony R.
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