Host: The Japanese Society for Planetary Sciences: Local Organizing Committee for 2006 Fall Meeting
We showed a process of dust circulation in protoplanetary disks using the disk model with the puffed-up inner rim, which has the shadowed region behind (Dullemond et al. 2001). Then, we found that the abundance of dust particles is enhanced in the inner shadowed region of the disk due to dust circulation. Recently, Krauss and Wurm (2005), Wurm and Krauss (2006) suggested that the dust can move outward in the radial direction due to photophoresis. The photophoresis is based on the interaction between the particle with a radiation-induced non-uniform temperature distribution over its surface and the surrounding gas.Depending on the gas pressure, photophoresis can be stronger than the radiation pressure and gas drag at the optically thin region of the disk. Therefore, photophoresis may be effectively influence the motion of dust particles at the inner rim of the disks, where the gas pressure is high and the disk is optically thin. In this presentation, we will show the results of numerical simulations of dust circulation, taking the effect of photophoresis into account.
