On Rapidly Rotating Magnetic Core-Collapse Supernovae

• Published in: The Astrophysical journal 2005-07, Vol.628 (1), p.335-342
• Main Authors: Wilson, J. R, Mathews, G. J, Dalhed, H. E
• Format: Article
• Language: English
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1086/430297

We have analyzed the magnetic effects that may occur in rapidly rotating core collapse supernovae. We consider effects from both magnetic turbulence and the formation of magnetic bubbles. For magnetic turbulence we have made a perturbative analysis for our spherically symmetric, core-collapse supernova model that incorporates the buildup of magnetic field energy in the matter accreting onto the proto-neutron star shortly after collapse and bounce. This significantly modifies the pressure profile and increases the heating of the material above the proto-neutron star resulting in an explosion even in rotating stars that would not explode otherwise. Regarding magnetic bubbles, we show that a model with an initial uniform magnetic field similar to 10 super(8) G and uniform angular velocity of similar to 0.1 rad s super(-1) can form magnetic bubbles due to the very nonhomologous nature of the collapse. It is estimated that the buoyancy of the bubbles causes matter in the proto-neutron star to rise, carrying neutrino-rich material to the neutron star surface. This increases the neutrino luminosity sufficiently at early times to achieve a successful neutrino-driven explosion. Both magnetic mechanisms thus provide new means for initiating a Type II core-collapse supernova.