The purpose of the work is to build a self-consistent gas-dynamic model of the accretion disk of a compact astrophysical object, taking into account viscosity. The matter falling on a compact object consists of proton gas, electrons, and radiation arising from the braking of a rotating gas at a speed comparable to light. Physical proton viscosity is not enough in the gas-dynamic accretion model with laminar flow. It is necessary to introduce the so-called turbulent viscosity, probably arising from the development of instabilities, to explain the loss of the disk angular momentum. With a quantitative mathematical model of gas dynamics, taking into account the generally accepted turbulent viscosity, we want to demonstrate a solution with such instability.
Aksenov et al. (Wed,) studied this question.