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Turbulent magnetic field amplification from spiral SASI modes in core-collapse supernovae...

by Christian Y Cardall, R. D. Budiardja, Anthony Mezzacappa
Publication Type
Conference Paper
Journal Name
Journal of Physics: Conference Series
Publication Date
Page Number
Conference Name
Conference on Computational Physics 2011
Conference Location
Gatlinburg, Tennessee, United States of America
Conference Date

We describe the initial implementation of magnetohydrodynamics (MHD) in our astrophysical simulation code \genasis.
Then, we present MHD simulations exploring the capacity of the stationary accretion shock instability (SASI) to generate magnetic fields by adding a weak magnetic field to an initially spherically symmetric fluid configuration that models a stalled shock in the post-bounce supernova environment.
Upon perturbation and nonlinear SASI development, shear flows associated with the spiral SASI mode contributes to a widespread and turbulent field amplification mechanism.
While the SASI may contribute to neutron star magnetization, these simulations do not show qualitatively new features in the global evolution of the shock as a result of SASI-induced magnetic field amplification.