Dust Settling in Stratified Protostellar Disks : Streaming Instability and a New Route to Planet Formation

Details Dust Settling in Stratified Protostellar Disks : Streaming Instability and a New Route to Planet Formation Dust Settling in Stratified Protostellar Disks : Streaming Instability and a New Route to Planet Formation

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.0328b&link_type=abstract

American Astronomical Society, AAS Meeting #212, #3.28; Bulletin of the American Astronomical Society, Vol. 40, p.189

Astronomy and Astrophysics

Astronomy

Scientific paper

It is generally thought that the early stages of planet formation require dust grains to agglomerate together to form pebble and boulder-sized objects. In the environment of a dusty protostellar disk, the interaction of dust grains of various sizes with the turbulent gas can determine the rate of grain growth, as turbulence can both keep the dust well-mixed with the gas (preventing the formation of a dense layer in which dust grains can grow quickly), and create concentrations of enhanced dust density (where grains can grow quickly). We perform a suite of 3D shearing box simulations that are representative of the conditions in a minimum-mass solar nebula at radii of 0.3-300 AU. We examine the structure of an initially well-mixed layer of dust as in interacts with the gaseous disk, which is turbulently driven via the magnetorotational instability (MRI). We find that large dust grains settle into a thin layer, while smaller dust grains can remain well-mixed with the gas. We characterize this relationship between grain size and scale height for each of our radial stations within the protostellar disk.

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