Abstract:
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.
Keywords:MRI, simulation of MHD-instability, angular momentum transfer, accretion.
Fulltext:
PDF file (631 kB)