Analysis of convectively unstable regions arising in simulations of a protoplanetary disk evolution

The formation and evolution of protoplanetary disks are important stages of the formation of planetary systems. However, despite the impressive success in observing protoplanetary disks, the mechanism of mass and angular momentum transfer is still an unsolved question. The convection may be one of these mechanisms which leads to turbulization and to a growth of the disk viscosity. The convection in protoplanetary disks is a complex process, so realistic hydrodynamic and thermal models are required to study it. Given the lack of such a model, the role of convection in general disk evolution is still poorly understood. In this paper, we analyze the conditions for convective instability based on an evolutionary model of a gaseous disk FEOSAD, within which the detailed vertical structure is calculated. It is shown that inner areas of the model disk are convectively unstable, which makes it necessary to take them into account in future models.