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A small number of young stellar objects show signs of a halo-like structureof optically thin dust. This halo or torus is located within a few AU of thestar, but its origin has not yet been understood. A dynamically excited cloudof planetesimals colliding to eventually form dust could produce such astructure. The cause of the dynamical excitation could be one or more planets.This work investigates an inwardly migrating planet that is dynamicallyscattering planetesimals as a possible cause for the observed structures. Ifthis mechanism is responsible, the observed halo-like structure could be usedto infer the existence of planets in these systems. We present analyticalestimates on the maximum inclination reached owing to dynamical interactionsbetween planetesimals and a migrating planet. A symplectic integrator is usedto simulate the effect of a migrating planet on a population of planetesimals.It is found that an inwardly migrating planet is only able to scatter thematerial it encounters to highly-inclined orbits if the material is on aneccentric orbit. Such eccentric orbits can be the result of resonance trappingand eccentricity pumping. Simulations show that for a certain range ofmigration rates and planet masses, resonance capture combined with planetarymigration indeed causes the planetesimals to reach eccentric orbits andsubsequently get scattered to highly-inclined orbits. The size distribution ofthe resulting dust is calculated determined to find the total mass and opticaldepth, which are found to compare reasonably well with the observed structures.Dynamical scattering of planetesimals caused by a planet migrating in, followedby the grinding down of these planetesimals to dust grains, appears to be apromising explanation for the inferred circumstellar dust clouds. Further studyis needed to see if the haloes can be used to infer the presence of planets.

Stirring up the dust: A dynamical model for halo-like dust clouds in transitional disks