Nonstationary magnetorotational processes in a rotating magnetized cloud

We perform 2D numerical simulations of a magnetorotational explosion of a r otating magnetized gas cloud. We found that amplification of a toroidal mag netic field due to the differential rotation leads to a transformation of t he part of the rotational energy of the cloud to the radial kinetic energy. Simulations have been made for 3 initial values of xi (the relation of mag netic energy to the gravitational energy of the cloud): xi = 10(-2), 10(-4) , 10(-6). Part of the matter - similar to 7% of the mass of the cloud (simi lar to 3.3% of the final gravitational energy of the cloud) - gets radial k inetic energy which is larger than its potential energy and can be thrown a way to the infinity. It carries about 30% of the initial angular momentum o f the cloud. This effect is important for angular momentum loss in the proc esses of stellar formation, and for the magnetorotational mechanism of expl osion suggested for supernovae. Simulations have been made on the basis of the Lagrangian 2D numerical implicit scheme on a triangular grid with grid reconstruction.