Three-Dimensional Magnetic Fields in Realistic Simulations of Stellar Core Collapse and Bounce

Details Three-Dimensional Magnetic Fields in Realistic Simulations of Stellar Core Collapse and Bounce Three-Dimensional Magnetic Fields in Realistic Simulations of Stellar Core Collapse and Bounce

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jrasc..99q.140l&link_type=abstract

Journal of the Royal Astronomical Society of Canada, Vol. 99, No. 4, p.140

Physics

Scientific paper

The evolution of massive stars ends with an inner iron core that is unstable to gravitational collapse. Its dynamics is determined by electron capture on nuclei in the condensing matter. When the energydependent neutrino mean free path becomes short, emitted neutrinos escape in a competition between thermalization and diffusion. This process is accurately captured in spherically symmetric simulations with Boltzmann neutrino transport (e.g. Liebendoerfer et al. 2005, ApJ, 620, 840). Here, I present a simple parameterization of the comprehensive treatment of neutrino physics so that multi-dimensional simulations {of the collapse phase} can include the results of stateof- the-art neutrino transport in an efficient and accurate way (Liebendoerfer, astro-ph/0504072). With the application to the 3-D MHD simulations of Liebendoerfer, Pen, & Thompson (2005, to be published in Nucl. Phys. A), realistic three-dimensional simulations of slowly rotating collapse with magnetic fields become feasible to narrow the configuration space at bounce, i.e. at the onset of the not fully understood supernova explosion. The evolution of the magnetic field is followed for different choices of the uncertain initial values at the onset of collapse. Until a few milliseconds after bounce, a mainly compression-induced field amplification of about two orders of magnitude is found in the hot material layered around the protoneutron star. Larger magnetic fields are trapped within the protoneutron star. After bounce, the magnetic field lines entangle in the layers where convection is driven by entropy gradients. Cross-view stereograms are shown to visualize their evolution in 3-D.

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