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A. Moro-Martin, R. Malhotra (Steward Observatory)
Main sequence stars are commonly surrounded by debris disks, formed by cold far-IR-emitting dust that is thought to be continuously replenished by a reservoir of undetected dust-producing planetesimals. We have investigated the orbital evolution of dust particles in debris disks harboring massive planets. Small dust grains are blown out by radiation pressure, but gravitational scattering by the giant planets also creates an outflow of large grains, mainly confined in angular extent to a disk. We describe the characteristics of this large-particle outflow in different planetary architectures, discuss its detectability, its implications for exo-planetary debris disks, its contribution to the clearing of circumstellar debris in planetary systems, its effect on the particle size distribution of the immediate vicinity of star-forming regions, and its implications for the interpretation of in-situ dust detection experiments in space probes traveling in the outer Solar System.
This work is part of the SIRTF FEPS Legacy project (http://feps.as.arizona.edu). We acknowledge NASA for research support (contract 1224768 administered by JPL and grants NAG5-10343 and NAG5-11661) and IPAC for providing access to their facilities.
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The author(s) of this abstract have provided an email address for comments about the abstract: amaya@as.arizona.edu
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.