About the Influence of Accounting for 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 magnetorotational instability (MRI) in the accreting envelope of a protostar in the nonisothermal case, i.e., taking into account the energy equation, by the second-order Runge–Kutta discontinuous Galerkin (RKDG) method using MPI parallelization technology. It is shown that taking into account the energy equation in the general system of magnetohydrodynamic (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 the angular momentum to the periphery of the envelope and, as a consequence, to an increase in the rate of accretion onto the protostar. The simulation results are compared qualitatively with observations of the star formation region G31.41+0.31 and other observations.