Title: Dynamical simulations of the planetary system HD 69830
Abstract: The star HD 69830 exhibits radial velocity variations attributed to three planets as well as infrared emission at 8–35 μm attributed to a warm debris disc. Previous studies by Alibert et al. and Wyatt et al. have developed models for the planet migration and mass growth and the replenishment of warm grains. In this paper, we perform n-body integrations in order to explore the implications of these models for (1) the excitation of planetary eccentricity, (2) the accretion and clearing of a putative planetesimal disc, (3) the distribution of planetesimal orbits following migration and (4) the implications for the origin of the infrared emission from the HD 69830 system.