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"Collapse of rotating astrophysical objects and magnetorotaional processes
in protostellar clouds and core-collapse supernovae"
(based on doctor's thesis)

S.G. Moiseenko (IKI)


Gravitational collapse of rapidly rotating cold protostellar cloud was simulated numerically. It was shown that density distribution after the collapse is disk-like. An instability after the bounce shock in gravitational field was found. 

Magnetorotational processes in rotating magnetized protostellar cloud were investigated.It was shown, that differential rotation leads to the appearing and amplification of toroidal component of magnetic field. Magnetic pressure grows with time and leads to ejection of part of energy and mass of the cloud.

The problem of iron core collapse of massive star was investigated numerically. We show that gravitational collapse leads to the formation of proto neutron star, the bounce shock and neutrino radiation flash appears. While the energy ejected due to the bounce shock evolution is not enough for the explanation of core-collapse supernova event. 

For the first time the magnetorotational supernova explosion was simulated numerically in 2D approach. Explosion energy is  (0.5-0.6 10^{51}erg) what is enough for the explanation of the core-collapse supernova event. A magnetorotational instability during simulation of magnetorotational supernova explosion was found and investigated. We found that the shape of magnetorotational supernova qualitatively depends on the initial configuration of the magnetic field.

A mechanism of magnetic field mirror symmetry violation in rotating stars was suggested. We show that this mechanism allows to explain formation of one-sided ejections and formation of rapidly moving radiopulsars after supernovae explosions.