Tracking Dust in an Evolving Disk: Implications for Crystalline Silicates

Details Tracking Dust in an Evolving Disk: Implications for Crystalline Silicates Tracking Dust in an Evolving Disk: Implications for Crystalline Silicates

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.4002h&link_type=abstract

American Astronomical Society, DPS meeting #41, #40.02

Astronomy and Astrophysics

Astrophysics

Scientific paper

Samples returned from comet Wild 2 by the Stardust mission confirm that substantial quantities of crystalline silicates were incorporated into the comet at the time of its formation. We present numerical models of radial transport of grains combining advection and turbulent diffusion at the disk midplane. We employ one-dimensional disk models that evolve with time under the action of viscosity and photoevaporative mass loss, and track solid transport using an ensemble of individual particle trajectories. We find that models of grain transport within steady-state disks significantly underestimate the efficiency of outward grain transport. Initially compact disks with characteristic scales of 5-10 AU may transport (at a minimum) several percent of inner disk particles to the outer disk on timesscales of about 100,000 yr. Much higher efficiencies are possible if the particles are entrained within a mid-plane layer in which the mean radial flow is outward. In many of our models the transport efficiency falls off rapidly with time, and hence high temperature material must be rapidly incorporated into icy bodies to avoid fallback to small radii. We suggest that significant radial transport may only occur during the initial phase of rapid disk evolution, and may vary substantially between disks depending on their initial mass distribution. This work was supported by NASA's Origins of Solar Systems program (NNX09AB90G), by NASA's Astrophysics Theory and Fundamental Physics program (NNX07AH08G), and by the NSF's Division of Astronomical Sciences (0807471).

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