A Two-Fluid Analysis of the Kelvin-Helmholtz Instability in the Dusty Layer of a Protoplanetary Disk: A Possible Path toward Planetesimal Formation through Gravitational Instability

Details A Two-Fluid Analysis of the Kelvin-Helmholtz Instability in the Dusty Layer of a Protoplanetary Disk: A Possible Path toward Planetesimal Formation through Gravitational Instability A Two-Fluid Analysis of the Kelvin-Helmholtz Instability in the Dusty Layer of a Protoplanetary Disk: A Possible Path toward Planetesimal Formation through Gravitational Instability

Apr 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apj...641.1131m&link_type=abstract

The Astrophysical Journal, Volume 641, Issue 2, pp. 1131-1147.

Astronomy and Astrophysics

Astronomy

10

Instabilities, Stars: Planetary Systems: Formation, Turbulence

Scientific paper

We analyze the stability of the dust layer in protoplanetary disks to understand the effect of relative motion between gas and dust. Previous analyses not including the effect of the relative motion between gas and dust show that shear-induced turbulence may prevent the dust grains from settling sufficiently to be gravitationally unstable. We determine the growth rate of the Kelvin-Helmholtz instability in a wide range of parameter space and propose a possible path toward planetesimal formation through gravitational instability. We expect the density of the dust layer to become ρd/ρg~100 if the dust grains can grow up to 10 m.

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