About the influence of accounting the energy equation on the formation model of a large-scale vortical flow in the accreting envelope of a protostar

This paper studies the development of magnetorotation instability (MRI) in the accreting envelope of a protostar in the non-isothermal case, i.e. taking into account the energy equation, by RKDG method with a second order of an approximation using the parallel algorithm with MPI technology. It is shown that taking into account the energy equation in the general system of MHD equations does not significantly affect the modelling of the formation and the evolution of a large-scale turbulence structure, which leads to the removal of angular momentum to the periphery of the envelope and, as a consequence, to an increase in the rate of accretion to the protostar. The simulation results are compared qualitatively with observations of the star formation region G31.41+0.31 and other observations.