Clumpy accretion in pre-main-sequence stars as a source of perturbations in circumstellar disks

Abstract

The development of perturbations in the circumstellar disks of pre-main-sequence stars caused by clumpy accretion was investigated. Here we perform 3D hydrodynamical SPH simulations of disks perturbed by a recent clump accretion event. These simulations are further explored by radiative transfer calculations to quantify observational appearance of such disks. It was shown that the density waves in the disks were formed at the fall of the clump. After several revolutions they can transform into spirals and ring structures. Their images in mm-wavelengths are very similar to those observed with ALMA in some protoplanetary disks. We assume that the clumpy accretion may be the source of such structures.