On the Modeling of a Compressible MHD Turbulence of an Accretion Protoplanetary Disk

In the framework of the basic problem of cosmogony, which is associated with the reconstruction of the protoplanetary solar disk at the very early stages of its existence, a closed system of MHD equations on the mean flow scale is formulated. This system is intended for numerical solution of problems on interconsistent simulation of the structure and evolution of the accretion protoplanetary disk and its corona. The model of a thin (but optically thick) disk is considered, in which turbulence dissipation due to kinematic and magnetic viscosity, opaqueness of the medium, accretion from the surrounding space, and the action of turbulent alpha omega dynamo on the generation of magnetic field, as well as the magnetic force and energy interaction between the disk and its corona are taken into account.