Astronomy and Astrophysics – Astrophysics
Scientific paper
2007-11-28
Astronomy and Astrophysics
Astrophysics
ApJ, in press. Connections made to baroclinic instability. Movies available at http://astro.berkeley.edu/~echiang/im/im.html
Scientific paper
10.1086/527354
Gravitational instability of a vertically thin, dusty sheet near the midplane of a protoplanetary disk has long been proposed as a way of forming planetesimals. Before Roche densities can be achieved, however, the dust-rich layer, sandwiched from above and below by more slowly rotating dust-poor gas, threatens to overturn and mix by the Kelvin-Helmholtz instability (KHI). Whether such a threat is real has never been demonstrated: the Richardson criterion for the KHI is derived for 2-D Cartesian shear flow and does not account for rotational forces. Here we present 3-D numerical simulations of gas-dust mixtures in a shearing box, accounting for the full suite of disk-related forces: the Coriolis and centrifugal forces, and radial tidal gravity. Dust particles are assumed small enough to be perfectly entrained in gas; the two fluids share the same velocity field but obey separate continuity equations. We find that the Richardson number Ri does not alone determine stability. The critical value of Ri below which the dust layer overturns and mixes depends on the height-integrated metallicity Z (surface density ratio of dust to gas). Nevertheless, for Z between one and five times solar, the critical Ri is nearly constant at 0.1. Keplerian radial shear stabilizes those modes that would otherwise disrupt the layer at large Ri. If Z is at least 5 times greater than the solar value of 0.01, then midplane dust densities can approach Roche densities. Such an environment might be expected to produce gas giant planets having similarly super-solar metallicities.
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