Abstract
The meter-sized particles rapidly fall into the central star due to the gas drag force, before planetesimal formation. Thus, some outflow mechanisms are required for planetesimal formation. We consider the stellar radiation pressure induced the dust outflow for a weak turbulent disk with the puffed-up inner rim, where the gas convection is induced because of a steep radial temperature gradient. Our main objective is to investigate a possibility for the realization of dust circulation in the protoplanetary disk. We find that dust circulation is realized in the shadowed region of the disk. The outflow mass flux at the surface layer becomes a quasi-steady state on a short timescale compared with the disk evolution time through the inflow. Further, the outflow mass flux at the surface layer is comparable to the inflow mass flux at the disk interior in the shadowed region. From our results, we show that the steady surface density distribution of dust is enhanced due to dust circulation in the inner shadowed region. Their enhanced abundance of dust may cause planetesimal formation.
