Dust Motion at the Midplane in a Viscously Expanding Disk

Details Dust Motion at the Midplane in a Viscously Expanding Disk Dust Motion at the Midplane in a Viscously Expanding Disk

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dda....39.1517h&link_type=abstract

American Astronomical Society, DDA meeting #39, #15.17

Astronomy and Astrophysics

Astronomy

Scientific paper

Observations of long period comet spectra have long indicated a crystalline silicate content to comet material. Also, sample return from comet Wild 2 has indicated that crystalline silicates were incorporated into this Jupiter family comet when it formed, most likely in the Kuiper belt. These results from the Stardust mission have prompted the need for a mechanism that can transport grains of at least 20 microns in size from interior to 3 AU to beyond the orbit of Neptune. Work on turbulent mixing of the solar nebula has already pointed to the viability of this mechanism for addressing the Stardust results. We explore the outward transport of dust grains of various sizes due to gas drag at the midplane in a viscously expanding protoplanetary disk. We solve for the azimuthal and radial velocities of the gas following the treatment of Takeuchi and Lin (2002, ApJ 581, 1344-1355) and examine particles in the Epstein drag regime. The disk evolves due to turbulent viscosity using the alpha-parameterization, and photoevaporation by the central star. During early disk evolution we find direct outward transport of dust grains to several tens of AU on timescales of about a million years. This research was supported by NASA under grant NNX07AH08G.

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