Radial drift of particles in the solar nebula: implications for planetesimal formation

Details Radial drift of particles in the solar nebula: implications for planetesimal formation Radial drift of particles in the solar nebula: implications for planetesimal formation

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icar..165..438w&link_type=abstract

Icarus, Volume 165, Issue 2, p. 438-442.

Astronomy and Astrophysics

Astrophysics

16

Scientific paper

For standard cosmic abundances of heavy elements, a layer of small particles in the central plane of the solar nebula cannot attain the critical density for gravitational instability. Youdin and Shu (2002, Astrophys. J. 580, 494-505) suggest that the local surface density of solids can be enhanced by radial migration of particles due to gas drag. However, they consider only motions of individual particles. Collective motion due to turbulent stress on the particle layer acts to inhibit such enhancement and may prevent gravitational instability.

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