  We present results of 2D simulation of magnetorotational (MR) supernova
accompanied by jet formation in the core collapse supernova explosion. Initial
magnetic field used in the simulations has dipole-like symmetry. Contrary to
the simulations of MR supernova with initial quadrupole-like magnetic field,
where the matter was ejected mainly near the equatorial plane, in presence of
the dipole-like initial magnetic field the supernova explosion is developing
preferably along a rotational axis, and leads to 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 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 $0.61\cdot 10^{51}$erg, and about $0.13M_\odot$ of
mass was ejected during the explosion.
