Modeling the Planetesimal formation Process and Its Comparison to Observations of Vega-like stars

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We study planetesimal formation processes. The following effects are studied : turbulence induced by the dust layer formed at the midplane of the gas disks, self-gravity of the dust layer, grain charges, and collisional fragmentation. We derived properties of the gas disks required for planetesimal formation. In order to compare the planetesimal formation theory to the observations of Vega-like stars, we study dust disk structure affected by the stellar radiation and the disk gas. We have also performed experimental studies of high velocity collisions of dust particles and derived the size distribution of collisional fragments. Finally, we derived the gas disk properties from the observation of the transitional disk, which is considered to be a former stage of Vega-like disks.