Abstract
The magnetorotational mechanism for supernova type II explosions is investigated numerically in 2-D . For the simulations we use a specially developed, implicit Lagrangian method on a triangular grid with grid reconstruction. We show that the shape of the explosion qualitatively depends on the initial configuration of the poloidal magnetic field. We also have done simulations of the problem of collapse of the protoneutron star. It was shown that after the collapse the resulting configuration consists of a dense, almost rigid, rapidly rotating core and a prolate, slowly rotating envelope. The angular velocity changes very quickly in the transitional region between the core and the envelope. In such a situation we can expect rapid evolution of the toroidal component of the magnetic field due to differential rotation, which can lead to the explosion.
