On Rapidly Rotating Magnetic Core‐Collapse Supernovae

We have analyzed the magnetic effects that may occur in rapidly rotating corecollapse supernovae. We consider effects from both magnetic turbulence and theformation of magnetic bubbles. For magnetic turbulence we have made aperturbative analysis for our spherically symmetric core-collapse supernovamodel that incorporates the build up of magnetic field energy in the matteraccreting onto the proto-neutron star shortly after collapse and bounce. Thissignificantly modifies the pressure profile and increases the heating of thematerial above the proto-neutron star resulting in an explosion even inrotating stars that would not explode otherwise. Regarding magnetic bubbles weshow that a model with a modest initial uniform magnetic field and uniformangular velocity of ~0.1 rad/s can form magnetic bubbles due to the very nonhomologous nature of the collapse. It is estimated that the buoyancy of thebubbles causes matter in the proto-neutron star to rise, carrying neutrino-richmaterial to the neutron-star surface. This increases the neutrino luminositysufficiently at early times to achieve a successful neutrino-driven explosion.Both magnetic mechanisms thus provide new means for initiating a Type IIcore-collapse supernova.Comment: 12 pages, 9 figure