Debris disks are dusty circumstellar disks found around many main-sequence stars. Grain sizes in these disks range from micron (for the dust component) to meter (for planetesimals). Those disks are dynamical systems, where the dust evolves through collisions and fragmentation, thus continually replenishing the disk with new dust. Recent resolved debris disk images exhibit interesting radial and azimutal structures, such as gaps, rings and warps. Those configurations are likely to be the results of planetary companions shaping the disk by their gravitational influence. Using a N-body code, the main purpose of my PhD is to create numerical simulations of such systems and thus infer the presence of planetary systems to explain the current observations.
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