Evolution of grains in a turbulent solar nebula

Details Evolution of grains in a turbulent solar nebula Evolution of grains in a turbulent solar nebula

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985pggp.rept..140w&link_type=abstract

In NASA, Washington Repts. of Planetary Geol. and Geophys. Program, 1984 p 140-142 (SEE N85-23474 13-91)

Computer Science

Sound

Accretion Disks, Coagulation, Interplanetary Dust, Protoplanets, Solar Corona, Turbulence, Grain Boundaries, Opacity, Particle Size Distribution

Scientific paper

Planetesimal formation by gravitational instability of a dust layer requires a nonturbulent solar nebula. The assumption that the solar nebula is a turbulent, convective accretion disk is explored. Self consistent models of a convective disk depend on high opacity of the disk material, which must be provided by grains. Grain coagulation is implied by the requirement of forming planetesimals, as the turbulent velocities (approx. 1/3 sound speed) in the accretion disk would disrupt any dust layer. Collisional coagulation could form large planetesimals, simultaneously leaving a sufficient fraction of matter in small grains to maintain the nebula's opacity. Or, coagulation of grains into small (approx. cm) aggregates could lower the opacity enough for turbulence to decay. The evolution of a population of grains in a turbulent solar nebula is calculated numerically.

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