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Weanalyzethestabilityofthedustlayerinprotoplanetarydiskstounderstandtheeffectofrelativemotionbetween gas and dust. Previous analyses not including the effect of the relative motion between gas and dust show that shearinducedturbulencemaypreventthedustgrainsfromsettlingsufficientlytobegravitationallyunstable.Wedetermine 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  d/ g  100 if the dust grains can grow up to 10 m. Subject headingg instabilities — planetary systems: formation — turbulence

astrophysical journal/the astrophysical journal

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