High-resolution simulations and visualization of protoplanetary disks: structure of the flow in the vicinity of a massive planet

A problem of mass flow in the immediate vicinity of a planet embedded in a protoplanetary disk is studied numerically in two dimensions. Large differe nces in temporal and spatial scales involved suggest that a specialized dis cretization method for solution of hydrodynamical equations may offer great savings in computational resources, and can make extensive parameter studi es feasible. Preliminary results obtained with help of Adaptive Mesh Refine ment technique and high order explicit Eulerian solver are presented. This combination of numerical techniques appears to be an excellent tool which a llows for direct; simulations of mass flow in vicinity of the accretor at m oderate computational cost. The present communication is focused on the str ucture of the outer part of the circumplanetary disk. We employ the multifl uid option to the hydrodynamical solver to prove that the circumplanetary d isk is composed of the gas transfered into it from the edges of the gap.