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

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

2012-03-15

arxiv.org/abs/1203.3385v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

15 pages, 7 figures, To appear in the Journal of Physics: Conference Series. Proceedings of the IUPAP Conference on Computatio

Scientific paper

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.

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