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

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21544811h&link_type=abstract

American Astronomical Society, AAS Meeting #215, #448.11; Bulletin of the American Astronomical Society, Vol. 42, p.456

Astronomy and Astrophysics

Astrophysics

Scientific paper

Samples returned from comet Wild 2 by the Stardust mission confirm that when the comet formed it incorporated substantial quantities of crystalline silicates. Crystalline silicates require high processing temperatures and therefore likely originated interior to the comet-forming region. 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 with inward flowing disk gas preferentially lose particles that begin at small AU, but that the particles up to 0.2 mm in size that remain in the disk become radially well-mixed out to the comet-forming regions. 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 intial mass distribution. This work was supported by NASA's Origins of the 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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