Dynamical Simulations of the Planetary System HD69830
Matthew J. Payne, Eric B. Ford, Mark C. Wyatt, Mark Booth

TL;DR
This study uses n-body simulations to explore planetary dynamics, disk evolution, and dust emission in the HD 69830 system, revealing complexities in eccentricity excitation, planetesimal accretion, and dust origin.
Contribution
It provides new insights into planetary eccentricity excitation, planetesimal disk evolution, and dust emission mechanisms through detailed dynamical simulations.
Findings
Planetary eccentricities cannot be explained solely by migration unless system is nearly face-on.
Planetesimal accretion rates differ from semi-analytic models, challenging simplified treatments.
A significant mass of planetesimals remains after planetary migration, supporting sustained dust emission.
Abstract
HD 69830 exhibits radial velocity variations attributed to three planets as well as infrared emission attributed to a warm debris disk. Previous studies have developed models for the planet migration and mass growth (Alibert et al. 2006) and the replenishment of warm grains (Wyatt et al. 2007). 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 disk, 3) the distribution of planetesimal orbits following migration, and 4) the implications for the origin of the IR emission. We find that: i) It is not possible to explain the observed planetary eccentricities (e~0.1) purely as the result of planetary perturbations during migration unless the planetary system is nearly face-on. ii) The rate of accretion of planetesimals onto planets in our n-body…
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