A magnetorotational core-collapse model with jets

We present the results of the 2D simulation of a magnetorotational (MR) core-collapse model accompanied by jet formation in the core-collapse model explosion. The initial magnetic field used in the simulations has a dipole-like symmetry. Contrary to the simulations of the MR core-collapse model with an initial quadrupole-like magnetic field, where the matter was ejected mainly near the equatorial plane, in the presence of the dipole-like initial magnetic field the core-collapse model explosion is developing preferably along a rotational axis and leads to the formation of a protojet. We expect that protojet propagation through the envelope of the star will be accompanied by its collimation. The magnetorotational instability (MRI) was found in the simulations, similar to the earlier considered case of the quadrupole-like initial magnetic field. Our estimations show that the characteristic time for the reconnection of the magnetic field is much larger than the MRI development time. The supernova explosion energy for the dipole-like field is about 0.61 x 10(51) erg, and about 0.13 M-circle dot of mass was ejected during the explosion.