Comparison of Two Methods for Modeling the Dynamics of Gas Flows in a Protoplanetary Disk

During the birth of a planetary system from a protoplanetary disk surrounding a young star, events such as collisions of formed dense gas and dust clumps, or the fall of such clumps of matter onto the disk from outside can occur in the disk itself. As a result of such events, a local increase in the density of matter is formed in the disk, which has a different velocity relative to the star than the surrounding matter. In this paper, we describe the numeric simulation of the evolution of a protoplanetary disk with the described heterogeneity, using for this two different approaches: the finite-volume method (PLUTO package) and the SPH method (Gadget-2 package). The computations were carried out in parallel mode. Based on the results obtained, we estimate the efficiency of parallelization at different stages of clump decay.