| Abstract |
The Stardust mission reveals the existence of crystalline silicates at the outer part of protoplanetary disks. These grains were thought to be formed in inner hot region, however, the process how such igneous products were incorporated into the object in the colder outer region is completely unknown.△ I consider two types of porous aggregate models and investigate the constraints of the radial drift of dust grains induced by stellar radiation pressure using the numerical simulation. Based on the simulation result, I discuss whether such radial drift is possible in our early solar system. |
