Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.1109m&link_type=abstract
American Astronomical Society, DPS meeting #28, #11.09; Bulletin of the American Astronomical Society, Vol. 28, p.1108
Astronomy and Astrophysics
Astronomy
1
Scientific paper
To understand the role that vortices in the gaseous solar nebula disk played in the formation of grains from dust, three questions need to be answered: how would a large vortex form, what are the characteristics of a long-lived vortex, and how does such a vortex affect the flow of dust? The shear due to the disk's Keplerian velocity profile significantly influences a vortex. Since this shear varies radially, the vortex characteristics must be studied numerically. A pseudo-spectral model has been developed to track numerically the evolution of a vorticity field in a simple, two-dimensional system by using the conservation of vorticity equation. With initial conditions of random vorticity fields, which are representative of turbulence in the disk, fluid with negative vorticity (the same sign as the vorticity of the Keplerian shear) tend to merge to form a coherent vortex. The robust vortices have elliptical cross sections and can last without significant changes for 10(4) years. They are flattened radially, with their shape related to their size and their strength relative to the shear. These vortices influence the flow of the dust grains which are suspended in the gas disk, tending to bring material into the negative vortex. The relative velocity of the particles is also affected, which then affects the particle collisions.
Flierl Glenn R.
Mehta A. V.
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