The article describes the collapse and explosion of a rotating, magnetized, Fe-Ni stellar core as an essential process in the formation of supernovae and pulsars, and in nucleosynthesis. The sequence of events comprising the core collapse, MHD disruption of the core, and mass ejection is visualized. Conversion of gravitational energy to other forms (radial KE, rotational KE, magnetic energy) by the infall of the stellar core, poloidal circulation and differential rotation of the core material, amplification of the seed magnetic field, and violent expulsion of the ejecta when magnetic stresses become unmanageable are analyzed. MHD buoyancy instabilities and other MHD phenomena are related to data on the dynamics of supernovae, the chemical composition of the interstellar gas, and cosmic rays.
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Meier et al. (1976) studied this question.