Magnetorotational supernova

We present the results of 2D simulations of the magnetorotational model of the supernova explosion. After the core collapse the core consists of rapidly rotating proto-neutron star and differentially rotating envelope. The generated by the differential rotation toroidal part of the magnetic energy growths linearly with time at the initial stage of the evolution of the magnetic field. The linear growth of the toroidal magnetic field is terminated by the development of magnetohydrodynamic instability, leading to the drastic acceleration of the growth of magnetic energy. At the moment when the the magnetic pressure becomes comparable with the gas pressure at the periphery of the proto-neutron star $\sim 10-15$km from the star center the MHD compression wave appears and goes through the envelope of the collapsed iron core. It transforms soon to the fast MHD shock and produces supernova explosion. Our simulations give the energy of the explosion $0.6\cdot 10^{51}$ ergs. The amount of the ejected by the explosion mass $\sim 0.14M_\odot$. The implicit numerical method, based on the Lagrangian triangular grid of variable structure was used for the simulations.