A magnetohydrodynamic supernova model

A quasi-spherical model is developed for the supernova explosion of a massive rotating magnetic star. The dynamic development that leads to the explosion is represented in three phases: the collapse phase, the field intensification phase, and the explosion phase. Numerical results show that the explosion leads to the ejection of masses with energies of 10 to the 50th erg, leaving behind a rotating magnetic neutron star with a mass of 0.8-1.5 solar masses. A physical description and mathematical formulation of the model are given and calculations are presented with and without consideration of the magnetic field.